XVIII Serbian Српска астрономска Astronomical Conference ...Olga Atanackovi¶c...

Belgrade, 17 - 21 October 2017

BOOK OF ABSTRACTS

Eds. L. Č. Popović, D. Urošević and R. Pavlović

Belgrade 2017

Српска астрономска конференција Serbian Astronomical Conference XVIII

XVIII SERBIAN ASTRONOMICAL CONFERENCEBelgrade, 17-21 October 2017

Scientific Organizing Committee:

Luka C. Popovic (co-chair, Astronomical Observatory, Belgrade)Dejan Urosevic (co-chair, Faculty of Mathematics, Belgrade)Olga Atanackovic (Faculty of Mathematics, Belgrade)Zorica Cvetkovic (Astronomical Observatory, Belgrade)Gojko Djurasevic (Astronomical Observatory, Belgrade)Slobodan Jankov (Astronomical Observatory, Belgrade)Predrag Jovanovic (Astronomical Observatory, Belgrade)Andjelka Kovacevic (Faculty of Mathematics, Belgrade)Rade Pavlovic (Astronomical Observatory, Belgrade)Nadezda Pejovic (Faculty of Mathematics, Belgrade)Srdjan Samurovic (Astronomical Observatory, Belgrade)

Local Organizing Committee:

Rade Pavlovic (chair, Astronomical Observatory, Belgrade)Aleksandra Ciprijanovic (Faculty of Mathematics, Belgrade)Miljana D. Jovanovic (Astronomical Observatory, Belgrade)Monika Jurkovic (Astronomical Observatory, Belgrade)Nemanja Martinovic (Astronomical Observatory, Belgrade)Ivana Milic Zitnik (Astronomical Observatory, Belgrade)Stanislav Milosevic (Faculty of Mathematics, Belgrade)Marko Pavlovic (Faculty of Mathematics, Belgrade)Djordje Savic (Astronomical Observatory, Belgrade)Milan Stojanovic (Astronomical Observatory, Belgrade)Milica Vucetic (Faculty of Mathematics, Belgrade)Vladimir Zekovic (Faculty of Mathematics, Belgrade)

The 18SAC is being organized by the Astronomical Observatory of Belgrade togetherwith the Department of Astronomy, Faculty of Mathematics, Belgrade University.The Conference is supported by the Ministry of Education, Science and Technolog-ical Development of the Republic of Serbia, Serbian Academy of Sciences and Arts,Telekom Srbija a.d. Beograd and TRAYAL KORPORACIJA AD, Krusevac.

Published by: Astronomical Observatory, 11060 Belgrade 38, Serbia

Computer text design: Tatjana Milovanov

ISBN 978-86-80019-85-7

Printed by: COPY PLANET d.o.o., Carice Milice 7, 11000 BeogradNumber of copies: 120

Belgrade, 17 - 21 October 2017

BOOK OF ABSTRACTS

Eds. L. Č. Popović, D. Urošević and R. Pavlović

Belgrade 2017

Српска астрономска конференција Serbian Astronomical Conference XVIII

XVIII SERBIAN ASTRONOMICAL CONFERENCE17-21 October 2017, Belgrade, Serbia

Book of abstracts, eds. L. C. Popovic, D. Urosevic and R. PavlovicAstronomical Observatory and Faculty of Mathematics, Belgrade, 2017

CONTENTS

INVITED LECTURES

S. BianchiCHALLENGES TO THE AGN UNIFIED MODEL . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 13D. V. BisikaloGASEOUS ENVELOPES OF HOT JUPITER . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 14V. Borka Jovanovic, P. Jovanovic, D. Borka and S. CapozzielloTESTS OF GRAVITY AT GALACTIC AND EXTRAGALACTIC SCALES:THEORY VS OBSERVATIONS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 15

D. Ilic, L. C. Popovic, E. Bon, N. Bon, P. Jovanovic, A. Kovacevic,J. Kovacevic-Dojcinovic, M. Lakicevic, S. Marceta-Mandic, Dj. Savic,S. Simic and M. StalevskiSPECTROSCOPY AND SPECTROPOLARIMETRY OF AGNs:FROM OBSERVATIONS TO MODELLING. . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 16Z. Kanuchova, G. Strazzulla, M. E. Palumbo, R. Brunetto and M. MelitaLABORATORY SIMULATIONS OF SPACE WEATHERING EFFECTS.SOME APPLICATIONS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 17Z. Knezevic125 YEARS FROM THE BIRTH OF ACADEMICIANVOJISLAV V. MISKOVIC. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 19O. LatkovicOBSERVATIONAL STUDIES OF CLOSE BINARY STARS. . . . . . . . . . . . . .. . . . . . . 20D. Onic and D. UrosevicEMISSION NEBULAE: STRUCTURE AND EVOLUTION – A BRIEFREVIEW OF THE RESULTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 21R. Pavlovic and Z. CvetkovicDYNAMICS AND KINEMATICS OF CELESTIAL BODIES ANDSYSTEMS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 22V. Protic - BenisekAKADEMIK VOJISLAV V. MISKOVIC (1892 - 1976):ZIVOT I DELO ZNAMENITOG SRPSKOG ASTRONOMA. . . . . . . . . . . . . .. . . . . . . 23J. C. RaymondCOLLISIONLESS SHOCK WAVES IN THE SOLAR CORONA ANDSUPERNOVA REMNANTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 24S. SamurovicVISIBLE AND INVISIBLE MATTER IN NEARBY GALAXIES:THEORY AND OBSERVATIONS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 25D. SijackiCOSMOLOGICAL SIMULATIONS OF STRUCTURE FORMATION:A CRITICAL VIEW . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 26

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O. TibollaCOSMIC RAY ORIGIN: BEYOND THE STANDARD MODEL(S).THE CASE OF PULSAR WIND NEBULAE AND UNIDENTIFIEDVERY HIGH ENERGY GAMMA-RAY SOURCES . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 27

PROGRESS REPORTS

O. AtanackovicASTRONOMY EDUCATION IN SERBIA 2014-2017 . . . . . . . . . . . . . . . . . . . . .. . . . . . . 31M. Boskovic, A. Obuljen, D. Vukadinovic, S. Milosevic, I. Milic and N. BozicDEPARTMENT OF ASTRONOMY AT PETNICA SCIENCE CENTER:2013-2017. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 32

A. CiprijanovicCONTRIBUTION OF GALAXIES AND GALAXY CLUSTERS TO THEDIFFUSE GAMMA-RAY BACKGROUND . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 33A. D’Addio, S. Capozziello, P. Jovanovic and V. Borka JovanovicTESTING EXTENDED THEORY OF GRAVITY BY Sgr A* . . . . . . . . . . . .. . . . . . . 34

D. Delibasic, D. D. Dimitrijevic, G. S. Djordjevic, M. Milosevic andM. StojanovicBRANEWORLD COSMOLOGY AND TACHYON INFLATION - RSIINUMERICAL MODELS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 35I. Dimitrijevic, B. Dragovich, J. Stankovic and Z. RakicCOSMOLOGICAL PERTURBATIONS IN NONLOCAL GRAVITY . . . . . .. . . . . . . 36I. Dimitrijevic, B. Dragovich, Z. Rakic and J. StankovicNEW COSMOLOGICAL SOLUTIONS IN NONLOCAL MODIFIEDGRAVITY. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 37M. S. DimitrijevicASTRONOMICAL WORK OF ANATOLY ANATOLYEVICH MIHAJLOV(1941-2016) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 38

V. Djosovic, B. Vukotic and M. M. CirkovicPROBING THE GALACTIC HABITABILITY TIME SCALES. . . . . . . . . . .. . . . . . . 39S. Gravina, S. Capozziello, D. Borka and V. Borka JovanovicSTELLAR KINEMATICS AROUND GALACTIC CENTER. . . . . . . . . . . . . .. . . . . . . 40

N. Janc, V. Protic Benisek, V. Benisek, L. C. Popovic, M. B. Gavrilov andS. B. MarkovicCORRESPONDENCE OF VOJISLAV V. MISKOVIC ABOUT HISDOCTORATE WITH MILUTIN MILANKOVIC, MIODRAG IBROVACAND OTON KUCERA . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 41S. Jankov, M. Hadjara and R. G. PetrovREGULUS OBSERVED WITH VLTI/AMBER. . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 42

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S. Knezevic, R. Lasker, G. van de Ven, G. Morlino, J. C. Raymond,C. Bailer-Jones, J. Font and J. Mendez-AbreuREVEALING SHOCK AND COSMIC-RAY PROPERTIES FROMBALMER EMISSION IN SUPERNOVA REMNANTS: THE CASE OFTYCHO . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 43

D. MarcetaPOSSIBILITIES AND OPTIMIZATION OF LANDING ON THESOUTHERN HEMISPHERE OF MARS. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 44

M. M. Martinovic, A. Zaslavsky, M. Maksimovic and S. SeganA STUDY OF QUASI-THERMAL NOISE AND SHOT NOISE IN SPACEPLASMAS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 45

N. Martinovic and M. MicicRECONSTRUCTING FORMATION AND EVOLUTION OF COMPACTDWARF CANDIDATES IN CLUSTERS OF GALAXIES . . . . . . . . . . . . . . . . .. . . . . . . 46

Z. Mijajlovic and N. PejovicIS COSMOLOGICAL CONSTANT TRANSIENT PHENOMENA? . . . . . . .. . . . . . . 47

I. Milic ZitnikIMPACT OF YARKOVSKY EFFECT AND MEAN-MOTIONRESONANCES ON MAIN BELT ASTEROID’S TRANSPORT. . . . . . . . . . .. . . . . . . 48

S. Milosevic, M. Micic, N. Martinovic, M. Smole and A. MitrasinovicINFLUENCE OF THE SOFTENING LENGTH ON STABILITY OFSPIRAL GALAXIES IN N-BODY SIMULATIONS . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 49

A. Mitrasinovic, M. Micic, N. Martinovic, M. Smole and S. MilosevicBAR DETECTION IN N-BODY SIMULATIONS USING FOURIERANALYSIS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 50

J. Petrovic, T. Prodanovic and M. KovacevicDISSECTING THE GALACTIC TeV EXCESS . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 51

T. Prodanovic and D. DonevskiCOSMIC-RAY ACCELERATION IN GALACTIC INTERACTIONS ANDITS IMPLICATIONS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 52

V. Radovic and B. NovakovicEXCLUDING INTERLOPERS FROM ASTEROID FAMILIES . . . . . . . . . . .. . . . . . . 53

M. Smole, M. Micic, N. Martinovic, A. Mitrasinovic and S. MilosevicEARLY GROWTH OF SUPERMASSIVE BLACK HOLES ANDGRAVITATIONAL WAVE RECOIL . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 54

V. A. Sreckovic, Lj. M. Ignjatovic, D. Jevremovic, V. Vujcic andM. S. DimitrijevicRADIATIVE AND COLLISIONAL ATOMIC/MOLECULAR DATA FORASTROPHYSICS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 55

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M. StalevskiPECULIAR MID-INFRARED MORPHOLOGY OF ACTIVE GALACTICNUCLEUS IN CIRCINUS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 56N. StanicTHE NATURE OF EDUCATIONAL ACTIVITIES IN PLANETARIUMAND ITS CONTRIBUTION TO THE ADVANCEMENT OFASTRONOMICAL EDUCATION . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 57D. Stoiljkovich and R. J. AndertonBOSCOVICH’S COMPREHESION OF ABSOLUTE AND RELATIVEMOVEMENT . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 58Z. TomicPROJECT OF PROMOTION OF ASTRONOMY SKY IS THE LIMIT . .. . . . . . . 59V. Trajkovska and S. NinkovicMILAN G. NEDELJKOVIC - THE FOUNDER AND FIRST DIRECTOROF THE OBSERVATORY OF THE GRAND SCHOOL (ON THEOCCASION OF 160th - ANNIVERSARY OF THE BIRTH) . . . . . . . . . . . . . .. . . . . . . 60

S. Vidojevic, S. Ninkovic, B. Simonovic, I. Beslic, S. Andjelkovic, V. Sarkovic,P. Obradovic, M. Puric and A. MiladinovicASTRONOMY COMPETITIONS AND THEIR ROLE IN ASTRONOMYEDUCATION IN SERBIA. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 61I. VinceILLUMINANCE AND VISIBILITY AT TWILIGHTS . . . . . . . . . . . . . . . . . . . .. . . . . . . 62O. Vince, S. Samurovic, R. Pavlovic, Z. Cvetkovic and G. DjurasevicTHE FIRST YEAR OF THE MILANKOVIC TELESCOPE . . . . . . . . . . . . . .. . . . . . . 63M. VuceticOPTICAL SUPERNOVA REMNANTS AND THEIR INFLUENCE ONSTAR FORMATION RATES DERIVED FROM Hα EMISSION. . . . . . . . . .. . . . . . . 64A. VudragovicSPECTROSCOPICAL AND PHOTOMETRICAL ANALYSIS OFNEARBY GALAXIES OF DIFFERENT MORPHOLOGICAL TYPES . . .. . . . . . . 65D. Vujicic and R. PavlovicTHE APPLICATION OF NINE DEGREES OF FREEDOM SENSOR INDETERMINATION OF TELESCOPE POSITION . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 67

L. Zivadinovic, S. Milosevic and D. MilicDENSITY PROFILE OF THE MILKY WAY: COMPARISON OFDYNAMICAL MODEL AND MONTE CARLO METHOD FORDETERMINING STELLAR SPACE DENSITIES. . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 68

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POSTERS

A. Bajic and M. S. DimitrijevicOVID, FASTI, SUN AND STARS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 71

M. Bılek and S. SamurovicTWO TYPES OF DARK MATTER DISTRIBUTION IN EARLY-TYPEGALAXIES . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72S. Boeva, G. Latev, G. Nikolov, R. Zamanov, B. Spassov and M. BelchevaFAST VARIABILITY OF GK PERSEI . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 73

V. M. Cadez and A. NinaANALYSIS OF ELECTROMAGNETIC WAVES IN IONOSPHERICPLASMA MODELS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 74

A. Ciprijanovic, T. Prodanovic and M. Z. PavlovicCONSTRAINING THE COLLECTIVE RADIO EMISSION OF LARGESCALE ACCRETION SHOCKS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 75G. Damljanovic, S. Boeva, O. Vince, G. Latev, R. Bachev, M. D. Jovanovic,Z. Cvetkovic and R. PavlovicOBSERVATIONS OF GAIA-FUN-TO FROM 2014 USING SERBIAN ANDBULGARIAN TELESCOPES . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 76M. S. DimitrijevicON THE ASTRONOMICAL SYMBOLS ON ROMAN REPUBLICAN ANDIMPERIAL COINS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 77M. S. Dimitrijevic, S. Sahal-Brechot and N. MoreauTHE STARK-B DATABASE, A NODE OF VIRTUAL ATOMIC ANDMOLECULAR DATA CENTER (VAMDC). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 78

Z. DisterloRADIO ODJEK DELTA AURIGIDS U PERIODU 2006-2016 GODINE. . .. . . . . . . 79M. D. Jovanovic, G. Damljanovic and O. VinceR AND V BAND MONITORING OF QUASARS THAT ARE IMPORTANTFOR THE LINK BETWEEN ICRF AND THE FUTURE GAIACELESTIAL REFERENCE FRAME . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 80A. I. Klyuyeva, A. V. Belov and E. A. EroshenkoRIGIDITY SPECTRUM OF GALACTIC COSMIC RAYS VARIATIONSDURING THE FORBUSH EFFECTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 81B. KrstinKORELACIJA ASTRONOMIJE I GEOGRAFIJE . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 82D. V. LukicPROTOCOL FOR ACTIVE SETI IN SOL NEIGHBORHOOD . . . . . . . . . . .. . . . . . . 83D. V. LukicSEARCH FOR POSSIBLE EXOMOONS WITH FAST TELESCOPE . . . . . . . . . . . 84

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D. V. LukicCAN WE AFFORD AN INTERSTELLAR FLIGHT?. . . . . . . . . . . . . . . . . . . . .. . . . . . . 85N. Martinovic, M. Micic, A. Mitrasinovic, S. Milosevic and M. SmoleDWARF GALAXY DEMOGRAPHY IN CLUSTERS OF GALAXIESFROM COSMOLOGICAL SIMULATIONS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 86N. Martinovic, M. Micic, A. Mitrasinovic, M. Smole and S. MilosevicWHAT CAN ECCENTRICITIES OF MEMBERS OF CLUSTERS OFGALAXIES TELL US ABOUT CLUSTER EVOLUTION? . . . . . . . . . . . . . . .. . . . . . . 87A. B. NedeljkovicNECESSITY OF RE-DEFINITION OF PLANET, AS PROPOSED BYALAN STERN ET AL . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 88

A. Nina, V. M. Cadez, L. C. Popovic, V. A. Sreckovic, J. Bajcetic,S. T. Mitrovic, M. Radovanovic, M. Todorovic Drakul, A. Kolarski andS. SimicLOW IONOSPHERIC RESPONSE TO ASTRO-GEO-PHENOMENA- RECENT RESEARCH. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 89S. NinkovicON A NEW FORMULA FOR THE VELOCITY-DISPERSION RATIO . .. . . . . . . 90S. NinkovicON A SIMPLE FORMULA FOR CALENDARS . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 91B. Novakovic, V. Radovic and V. -DosovicASTEROID FAMILIES PORTAL: AN ONLINE PLATFORM TO STUDYASTEROID FAMILIES. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 92R. Pavlovic, Z. Cvetkovic, G. Damljanovic, O. Vince and M. D. JovanovicTHE FIRST TEST OF NEW ANDOR IXON 897 EMCCD CAMERA . . . .. . . . . . . 93Z. PrnjatMILUTIN’S SUNDIAL IN KRALJEVO . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 94N. M. Sakan, V. A. Sreckovic, Z. Simic and M. S. DimitrijevicTHE SPECTRAL COEFFICIENTS OF ABSORPTION PROCESSES INDENSE STRONGLY IONIZED ASTROPHYSICAL PLASMAS . . . . . . . . . .. . . . . . . 95N. M. Sakan, V. A. Sreckovic, Z. Simic and M. S. DimitrijevicTHE OPTICAL CHARACTERISTICS OF DENSE, STRONGLYIONIZED HYDROGENE PLASMA, APPLICABLE IN ASTROPHYSICALOBJECTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 96S. SamurovicDYNAMICAL MODELS OF THREE LENTICULAR GALAXIES:NGC 1023, NGC 3115 and NGC 4526. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 97

S. Samurovic, G. Djurasevic, Z. Cvetkovic, R. Pavlovic and O. VinceTELESCOPE “MILANKOVIC”: MOUNTING, PRESENT AND FUTUREWORK . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 98

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V. A. Sreckovic, Lj. M. Ignjatovic, A. Nina and M. S. DimitrijevicTHE NEW MODEL METHOD OF THE ELECTROSTATICSCREENING OF THE ASTROPHYSICAL PLASMAS:MULTI-COMPONENT SYSTEMS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. . . . . . . 99

V. A. Sreckovic and D. M. SulicSTRONG SOLAR X RAY FLARES: INFLUENCE ON THEIONOSPHERE . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 100M. StalevskiTHE DUST COVERING FACTOR IN ACTIVE GALACTIC NUCLEI . . . . . . . . 101N. TodorovicTHE FINE STRUCTURE OF CHAOS IN THE SOLAR SYSTEM . . . . . . . . . . . . 102O. Vince, M. D. Jovanovc and I. VinceFIRST SPECTRA FROM THE TELESCOPE MILANKOVIC . . . . . . . . . . . . . . . . . 103A. Vudragovic, O. Vince, S. Samurovic and M. JovanovicNEAR-INFRARED PHOTOMETRY OF THE NEARBY SPIRALGALAXY NGC 2841 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 104V. ZekovicRESONANT MICROINSTABILITY AS A TRIGGER OFCOLLISIONLESS SHOCK FORMATION . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 105

PROGRAMME OF XVIII SERBIAN ASTRONOMICAL CONFERENCE. . . . . 109LIST OF POSTERS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 115LIST OF PARTICIPANTS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 119AUTHORS’ INDEX . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 125

9

Invited Lectures



Invited Lecture

CHALLENGES TO THE AGN UNIFIED MODEL

S. Bianchi

A Dipartimento di Matematica e Fisica, Universita degli Studi Roma Tre,via della Vasca Navale 84, 00146 Roma, Italy

E-mail : [email protected]

Although the basic ingredient of the Unification Model of Active Galactic Nuclei,i.e. the presence of nonspherically symmetric absorbers at the origin of the type1/type 2 dichotomy, remains certainly valid, several new observations and models,mostly in the X-ray and infrared domain, suggest that multiple absorbers are presentaround the central source, on quite different physical scales. In this talk, we reviewthese pieces of evidence, in order to picture the structure of AGN obscuration ondifferent scales, from the vicinity of the Black Hole to the host galaxy. We then focuson some of the open issues, which still challenge any attempt to picture an updatedunification scenario explaining all the complex observed phenomenology.

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Invited Lecture

GASEOUS ENVELOPES OF HOT JUPITER

D. V. Bisikalo

Institute of astronomy of the Russian Academy of Sciences,48, Pyatnitskayastr., 119017, Moscow, Russia


Hot Jupiter exoplanets, have a number of outstanding features, caused mostly bytheir proximity to the host star, e.g.: gas outflowing from the planet’s atmosphere tothe star, as it happens in close binary stars. In addition, the short distance betweenthe planet and the star results in a large planet’s orbital velocity. If this velocityexceeds the local sound speed a bow-shock forms ahead of the planet. Gas-dynamicalmodeling shows that, if the dynamical pressure of the stellar-wind is high enoughto stop the outflow from the vicinity of the inner Lagrangian point, a quasi-closednon-spherical envelope, bounded by the bow-shock of a complex shape, forms inthe system. In this report we discuss possible types of gaseous envelopes of hotJupiters and compare their properties with available observations. We also considerthe variations of flow patterns in the gaseous envelopes, occurring under the actionof coronal mass ejections.

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Invited Lecture

TESTS OF GRAVITY AT GALACTIC AND EXTRAGALACTICSCALES: THEORY VS OBSERVATIONS

V. Borka Jovanovic1, P. Jovanovic2, D. Borka1 and S. Capozziello3,4,5

1Atomic Physics Laboratory (040), Vinca Institute of Nuclear Sciences,University of Belgrade, P.O. Box 522, 11001 Belgrade, Serbia

2Astronomical Observatory, Volgina 7, P.O. Box 74, 11060 Belgrade, Serbia3Dipartimento di Fisica ”E. Pancini”, Universita di Napoli ”Federico II”,

Compl. Univ. di Monte S. Angelo, Edificio G, Via Cinthia, I-80126, Napoli, Italy4Istituto Nazionale di Fisica Nucleare (INFN) Sez. di Napoli, Compl. Univ.

di Monte S. Angelo Edificio G, Via Cinthia, I-80126, Napoli, Italy5Gran Sasso Science Institute, Viale F. Crispi, 7, I-67100, L’Aquila, Italy.

E-mail : [email protected], [email protected], [email protected], [email protected]

We present a short overview of our results considering a possibility to explain theobserved galactic and extragalactic dynamics using gravitational potentials derivedfrom Extended Theories of Gravity (ETGs) without dark matter (DM) hypothesis.These theories can have observational signatures at astrophysical and cosmologicalscales, and thus we consider different ETG potentials within the Galactic CentralParsec, as well as on extragalactic scales. The simulated stellar orbits, obtained bymodified gravity potentials, are compared with astrometric observations of S2 starorbit around the central suppermassive black hole of the Milky Way. The obtainedresults give strong constraints on the gravity interaction parameters. We also usedETGs to investigate the baryonic Tully-Fisher relation of spiral galaxies and thefundamental plane of ellipticals, and found that these empirical relations could betheoretically explained by the existence of a further gravitational radius predicted byETGs and without the DM hypothesis. This gravitational radius plays analogue role,in the case of weak gravitational field, like the Schwarzschild radius in the case ofstrong gravitational field.

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Invited Lecture

SPECTROSCOPY AND SPECTROPOLARIMETRY OF AGNs:FROM OBSERVATIONS TO MODELLING

D. Ilic1, L. C. Popovic2, E. Bon2, N. Bon2, P. Jovanovic2, A. Kovacevic1,J. Kovacevic-Dojcinovic2, M. Lakicevic2, S. Marceta-Mandic1, Dj. Savic2,

S. Simic3 and M. Stalevski2

1Department of Astronomy, Faculty of Mathematics, University of Belgrade, Serbia2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia3Department of Physics, Faculty of Sciences, Kragujevac, Serbia


Active galactic nuclei (AGNs) are one of the most luminous objects in the Uni-verse, emitting powerful continuum and line emission across all wavelength bands.They represent an important link in the investigations of the galaxy evolution andcosmology. The resolving of the AGNs inner structure is still a difficult task withcurrent instruments, therefore the spectroscopy and spectropolarimetry are crucialtools to investigate these objects and their components, such as the properties ofthe supermassive black hole, the broad line region, and the dusty torus. In this re-view, we are going to present the results of the project ”Astrophysical spectroscopyof extragalactic objects”, from the observations, data processing and analysis, to themodelling of different regions in AGNs.

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Invited Lecture

LABORATORY SIMULATIONS OF SPACE WEATHERING EFFECTS.SOME APPLICATIONS

Z. Kanuchova1,2, G. Strazzulla2, M. E. Palumbo2, R. Brunetto3

and M. Melita4

1Astronomical Institute of Slovak Academy of Sciences,SK-059 60 T. Lomnica, Slovakia

2INAF-Osservatorio Astrofisico di Catania, Via S. Sofia 78, I-95123 Catania, Italy3Institut d’Astrophysique Spatiale, CNRS, UMR-8617, Universite Paris-Sud,

F-91405 Orsay Cedex, France4Instituto de Astronomıa y Fısica del Espacio (IAFE), Buenos Aires, Argentina


The surfaces of atmosphere-less bodies are irradiated by solar ion populations(solar wind, flares, and solar energetic particles events), galactic cosmic rays, electrons,UV and X-rays, and bombarded by interplanetary dust. The effects induced by theseprocesses are commonly known as space weathering (SW) and depend on severalparameters such as surface composition and location in the Solar System. As aconsequence of the chemical-physical alterations induced by SW, optical propertiesof asteroid surfaces may change, thus affecting the interpretation of their spectralproperties and the efforts to establish a solid meteorites-asteroids link (Hapke, 2001;Clark et al., 2002; Brunetto et al., 2015). Major effects of SW processes are darkening,and reddening (a larger lowering of reflectance at lower wavelength) of the visible-nearinfrared spectra (VNIR) of surface materials; as well as a ”degrading” of absorptionfeatures (Chapman 1996; Pieters et al. 1993). In contrast with the reddening in theVNIR (550 - 1640 nm), the opposite trend - bluing (relative increasing of reflectance atlower wavelength) of the spectrum at near-ultraviolet (NUV, 200-400 nm) wavelengthsseems to take place (Hendrix and Vilas, 2006; Vilas et al., 2015; Brunetto et al., 2015and references therein) in some rocky objects in the Solar System (such as S-typeasteroids).A number of experimental studies have focused on the spectral alterationinduced by irradiating various types of meteorites and terrestrial silicates using the twomain agents of SW of asteroids, namely energetic ions - to simulate the effects of solarwind and cosmic rays, and laser pulses (nano-pico seconds) to simulate micrometeoritebombardment.The aim of laboratory experiments is to mimic the energy transferdistribution of the solar wind ions. The study of space weathering is essential for thecorrect interpretation of the observed spectral characteristics of small bodies of theSolar System.

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References

Brunetto, R., Loeffler, M.J., Nesvorny, D., Sasaki, S., Strazzulla, G.: 2015, AsteroidSurface Alteration by SW Processes. Asteroids IV, in press.

Chapman, C. R.: 1996, S-Type Asteroids, Ordinary Chondrites, and SW: The Ev-idence from Galileo’s Fly-bys of Gaspra and Ida. Meteorit. Planet. Sci., 31,699.

Clark, B. E., Hapke, B., Pieters, C., Britt, D.: 2002, Asteroid SW and RegolithEvolution. Asteroids III 585-599.

Hapke, B.: 2001, SW from Mercury to the asteroid belt. J. Geophys. Res., 106, 10,039.

Hendrix, V., Vilas, F.: 2006, The effects of SW at UV wavelengths: S-class asteroids.Astrophys. J., 132, 1396.

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Invited Lecture

125 YEARS FROM THE BIRTH OFACADEMICIAN VOJISLAV V. MISKOVIC

Z. Knezevic

Serbian Academy of Sciences and Arts, Knez Mihailova 35, 11001 Belgrade, SerbiaE-mail : [email protected]

The life and work of academician Vojislav V. Miskovic (1892–1976) are presentedon the occasion of the 125th anniversary of his birth. His main scientific achieve-ments are briefly reviewed, his roles as one of the first professors of astronomy atthe University of Belgrade and the builder and director of the contemporary Astro-nomical Observatory of Belgrade described and acknowledged. Particular attention ispaid to numerous activities and important duties he carried out in the Serbian RoyalAcademy (Serbian Academy of Sciences and Arts), after being elected its correspond-ing member in 1929, and the full member in 1939.

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Invited Lecture

OBSERVATIONAL STUDIES OF CLOSE BINARY STARS

O. Latkovic

Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected]

The Stellar Physics group at Astronomical Observatory of Belgrade conducts ob-servational studies at the forefront of binary star research with the aim to improveunderstanding and modeling of complex physical processes within close, interacting bi-naries on both ends of the stellar mass scale. On the high mass end, we study Double-Periodic Variables massive close binaries featuring accretion disks, gas streams andvarious circumbinary structures; on the low mass end, we study W UMa contact bina-ries as well as semi-detached and detached binaries in pre- and post-common-envelopestages of evolution. In this talk, I will showcase some of our recent results and publi-cations, and present our plans to enter the scene of automated processing of massivedata sets using machine learning and heuristic optimization.

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Invited Lecture

EMISSION NEBULAE: STRUCTURE AND EVOLUTION– A BRIEF REVIEW OF THE RESULTS

D. Onic and D. Urosevic

Department of Astronomy, Faculty of Mathematics,University of Belgrade, Studentski trg 16, 1100 Belgrade, Serbia


Since its beginning, the project ”Emission nebulae: structure and evolution”, sup-ported by the Ministry of Education, Science, and Technological Development of theRepublic of Serbia, gathered researchers from several different institutions: the De-partment of Astronomy at the Faculty of Mathematics of Belgrade University, theAstronomical Observatory of Belgrade, as well as from the Physics Department atthe Faculty of Sciences of the University of Novi Sad. The theoretical research andthe results obtained by observations of the astronomers of this group and in coopera-tion with fellow colleagues from several different institutions from abroad are mainlyfocused on supernova remnants. Supernova remnants are the most powerful Galacticsources of electromagnetic radiation (prominent at low as well as at high frequencies).These spectacular objects are responsible for the creation of the so-called cosmicrays, so that they represent the most efficient particle accelerators in our galaxy, aswell as in other galaxies throughout the Space. Some of the most important resultsachieved by this group, which pertain to the evolution of the supernova remnants, tothe appearance of their radio-spectra in continuum, and to the computation of theequipartition of the energy density of the magnetic field and of the energy densityof the ultra-relativistic particles, will be described. The analysis of the shape of theradio-continuum spectrum and position of the remnant in the co-called Σ − D dia-gram, complemented with the calculation of the magnetic field strength, enable us todetermine the evolutionary status of a supernova remnant. These topics will be brieflyelaborated in the context of our detailed theoretical interpretation of the particularobservations of the supernova remnants from the Magellanic clouds and from our owngalaxy which are performed by the colleagues from Australia. Related to this collab-oration is an investigation of the radio-evolution of the observed planetary nebulae(e.g. for the sample of Magellanic clouds objects). In addition, a search for opticallydetected supernova remnants in nearby galaxies and an analysis of their influenceon star formation rates derived from Hα emission, as a part of the activities of thisresearch group, will also be presented. Finally, a possible existence of so-called tidalcosmic ray population, formed by the tidal shock waves that result from the galac-tic interactions, as well as the existence of hypothetical structure-formation cosmicrays, produced by the large-scale accretion shocks during the process of large-scalestructure formation, will be discussed too.

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Invited Lecture

DYNAMICS AND KINEMATICS OF CELESTIALBODIES AND SYSTEMS

R. Pavlovic and Z. Cvetkovic

Astronomical Observatory, Volgina 7, P.O. Box 74, 11060 Belgrade, SerbiaE-mail : [email protected]

Here the most important results achieved and published by the participants inthe project ”Dynamics and Kinematics of Celestial Bodies and Systems” within 2011-2016 are presented. The results are numerous and significant, they cover the followingfour fields: dynamics of Solar-System minor bodies, analysis of orbital motion andobservations of double and multiple stars, kinematical properties of stars from thesolar neighbourhood and photometric observations of WEBT objects and morphologyof quasars.

The work on asteroid classification into families by use of a new polyphase methodhas been finished. In the analysis of the obtained results one also uses the availabledata on albedo and color index of asteroids. On a sufficient number of examples ithas been demonstrated how the new classification contributes to a better and moreexact determination of family age, member distribution in size, and other importantphysical and dynamical family characteristics.

The existing orbital elements for double and multiple stars have been improved,the new ones and the linear solutions calculated, by applying methods and algorithmscreated by the authors themselves, including as well the astrophysical parameters(masses, distances and luminosities). The obtained results have been announcedin IAU Commission G1 Information Circular and they have become immediatelyaccessible in the proper international database.

The potential calculation for a typical spiral galaxy has been elaborated, the localMilky-Way kinematics with importance of segregating two disc components and discfrom the halo has been treated; the statistics of nearby double stars has been studiedand elaborated.

The study of random and systematic errors of astrometric data for the Hippar-cos stars has been continued by comparing the Hipparcos value to those from severalother catalogues: new Hipparcos, EOC-2, EOC-3, EOC-4,PZT, IL. CCD observationsof quasars have been performed at NAO Rozhen and Astronomical Station Vidoje-vica aimed at providing a link between the existing and future (GAIA) internationalcelestial coordinate systems.

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Invited Lecture

AKADEMIK VOJISLAV V. MISKOVIC (1892 - 1976):ZIVOT I DELO ZNAMENITOG SRPSKOG ASTRONOMA1

V. Protic - Benisek


Radeci vec vise od jedne decenije na sto svestranijem i objektivnom prikazu delaakademika Vojislava Miskovica, autor ovog puta cini pokusaj da istakne one znacajnemomente koji su obelezili ne samo njegov zivotni put, vec su bili i reperi razvojaastronomske nauke u presudnim trenutcima razvoja modernih istrazivanja u Srbijidvadesetog veka.

I mada se ime profesora Vojislava Miskovica vezuje neposredno za Astronomskuopservatoriju u Beogradu (ciji je bio i prvi upravnik), on je u sustini najveci deo svogradnog i zivotnog veka proveo realizujuci i mnoge druge naucne zadatke o kojima semalo, ili nedovoljno zna.

Vojislav V. Miskovic je bio, moze se to slobodno reci, vrli, dostojni nastavljac delaprofesora Velike skole i osnivaca Meteoroloske i astronomske opservatorije u Beogradu,Milana Nedeljkovica ( 1857 – 1950).

1Iz MONOGRAFIJE posvecene AKADEMIKU VOJISLAVU V. MISKOVICU autora VOJISLAVE PROTIC – BENISEK (u Stampi)

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Invited Lecture

COLLISIONLESS SHOCK WAVES IN THE SOLAR CORONAAND SUPERNOVA REMNANTS

J. C. Raymond

Center for Astrophysics, 60 Garden St., Cambridge, MA 02176, USAE-mail : [email protected]

A shock wave is a transition from supersonic to subsonic flow in a narrow interval.A shock in neutral gas is governed by collisions, and collisions quickly bring the gas to anew thermodynamic equilibrium. Shocks in plasmas are governed by electromagneticfields and plasma turbulence, and they do not generally lead to thermal equilibrium.Electron, proton and ion temperatures can be very different, and the shocks canproduce non-thermal velocity distributions including cosmic rays or solar energeticparticles. This talk will cover observations of shocks in supernova remnants and thesolar corona that indicated those non-equilibrium conditions.

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Invited Lecture

VISIBLE AND INVISIBLE MATTER IN NEARBY GALAXIES:THEORY AND OBSERVATIONS

S. Samurovic


We describe the main accomplishments of the project “Visible and Invisible Matterin Nearby Galaxies: Theory and Observations” (no. 176021) funded by the Ministryof Education, Science and Technological Development of the Republic of Serbia. Wehave studied both visible (stars, gas, dust) and invisible (dark) matter in nearbygalaxies of various morphological types. One of the main tasks of the project wasto define the sample which includes both early- (elliptical) and late- (spiral) typegalaxies and this was accomplished successfully. The galaxies from our sample werestudied using their photometric and spectroscopic (also radio) data that come fromavailable catalogs and databases. We studied in detail their kinematics and dynamicsand we analyzed the anisotropies in stellar motions. We decomposed photometricprofiles to discover various structures in those objects. Dark matter was especiallyanalyzed in the case of elliptical galaxies using various observational techniques andtheoretical approaches. This project also included several sub-projects, where themost important one was dedicated to the purchase and the construction of the 1.40m telescope “Milankovic” mounted at the Vidojevica Astronomical Station. Theremaining three sub-projects include the work on i) the Galactic habitable zone andits features connected with the kinematics and dynamics of the Milky Way and nearbyspiral galaxies, ii) blazars and iii) cosmological simulations related to supermassiveblack holes, massive and dwarf galaxies and semi-analytic analysis of cosmologicalsimulations.

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Invited Lecture

COSMOLOGICAL SIMULATIONS OF STRUCTURE FORMATION:A CRITICAL VIEW

D. Sijacki

Institute of Astronomy and Kavli Institute for Cosmology,University of Cambridge, Madingley Road, Cambridge CB3 0HA, United Kingdom


Cosmological simulations of structure formation have undergone rapid develop-ment over the last decade and evolved from purely gravitational computations oflarge scale structure to full hydrodynamical simulations which include a plethora ofcomplex baryonic physics. Recent successes of these simulations have been impressive,with several independent groups obtaining models of present day galaxies with a mor-phological mix in broad accord with observation, which has been a long standing goalfor more than 20 years. Yet, due to many unknowns and the prohibitively large massand spatial resolutions needed to solve the problem ab initio, cosmological simula-tions have adopted so-called ”sub-grid” physics models, which are employed on small,unresolved scales. These invariably contain a number of free or poorly constrainedparameters which can crucially affect the main simulation results. In this talk I willcritically review how much cosmological simulations are subject to fine tuning due tothese ”sub-grid” models, which consequences this has for our understanding of theunderlying physics and what are the future prospects of moving towards ab initiosimulations.

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Invited Lecture

COSMIC RAY ORIGIN: BEYOND THE STANDARD MODEL(S).THE CASE OF PULSAR WIND NEBULAE AND UNIDENTIFIED

VERY HIGH ENERGY GAMMA-RAY SOURCES

O. Tibolla

Mesoamerican Centre for Theoretical Physics (MCTP),Universidad Autonoma de Chiapas (UNACH),

Carretera Emiliano Zapata Km. 4, Real del Bosque (Teran).29050 Tuxtla Gutierrez, Chiapas, Mexico


The riddle of the origin of Cosmic Rays is open since one century. Recentlywe got the experimental proof of hadronic acceleration in Supernovae Remnants,however new questions rised and no final answer has been provided so far. Gammaray observations above 100 MeV reveal the sites of cosmic ray acceleration to energieswhere they are unaffected by solar modulation. In the last years the knowledge inthis field of research widely increased, however almost 50% of the TeV (> 1012 eV)Galactic sources are still unidentified; at GeV (> 109 eV) energies, 67% of EGRETsources were unidentified and also with the newer generation of gamma-ray satelliteswe have the same result: in fact, at low Galactic latitudes (b < 10 deg), 62% of theFermi LAT detected sources have no formal counterpart. Hence understanding thehigh energy unidentified sources will be a crucial brick in solving the whole riddle ofCosmic Rays origin. Several examples will be shown, underlining the importance ofthe so-called ”dark sources“. Both theoretical aspects (with particular emphasis tothe so-called Ancient Pulsar Wind Nebulae scenario) and their observational proofswill be discussed.

27

Progress Reports



Progress Report

ASTRONOMY EDUCATION IN SERBIA 2014-2017

O. Atanackovic

Department of Astronomy, Faculty of Mathematics, University of Belgrade,Studentski Trg 16, 11000 Belgrade, P.O.Box 550, Serbia


A review of triennial activities in astronomy education in Serbia at all levels isgiven. An emphasis is put on various activities organized by the Department ofAstronomy, on the students’ practices held at the Astronomical Station on the moun-tain Vidojevica, newly published books, Petnica Science Center’s activities relatedto astronomy education, the participation of the Serbian team in the InternationalAstronomy Olympiads and activities of amateur astronomical societies.

31



Progress Report

DEPARTMENT OF ASTRONOMY AT PETNICA SCIENCE CENTER:2013-2017.

M. Boskovic1, A. Obuljen2, D. Vukadinovic1, S. Milosevic3, I. Milic4

and N. Bozic1

1Petnica Science Center, Potanski Fah 14, 14000 Valjevo, Serbia2SISSA - International School for Advanced Studies,

Via Bonomea 265, 34136 Trieste, Italy3Faculty of Mathematics, University of Belgrade,

Studentski Trg 14-16, 11000 Belgrade, Serbia4Max-Planck-Institut fur Sonnersystemforschung,

Justus-von-Liebig-Weg 3, 37075 Gottingen, GermanyE-mail : [email protected], [email protected],

[email protected], [email protected], [email protected], [email protected]

Activities of the Department of Astronomy at Petnica Science Center (PSC) withinthe period 2013-2017. will be given. The main activities of the Department of As-tronomy are aimed at high school students. The main educational principle of PSCis “education of students by other students” as high school students are taught andmentored mostly by undergraduate students. The full educational cycle at the De-partment of Astronomy presumes two years during which participants are introducedto the basics of astronomy and research methodology and, as a result of that, finish aresearch project. We will outline the present structure of the astronomical educationalactivities at PSC, topics of the participants’ research projects and other activities inthe mentioned period and future plans.

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Progress Report

CONTRIBUTION OF GALAXIES AND GALAXY CLUSTERSTO THE DIFFUSE GAMMA-RAY BACKGROUND

A. Ciprijanovic

Department of Astronomy, Faculty of Mathematics, University of Belgrade,Studentski trg 16, 1100 Belgrade, Serbia


Interactions of cosmic rays with the interstellar medium pro duce gamma rays,neutrinos, and lithium. Measurements of different pro ducts of cosmic-ray interac-tions can tell us more about the cosmic-ray population that produced them. In thethesis links between these different pro ducts were applied to accretion shocks assources of cosmic rays in clusters of galaxies and cosmic rays accelerated in supernovaremnants inside small galaxies. When considering galaxy clusters we include evolutionof accretion shocks that form during large-scale structure formation. This will resultin the evolution of gamma-ray production, which we include in our models, for thefirst time. The developed models are then compared to the observed isotropic diffusegamma-ray background observed by telescope Fermi-LAT and also to the high-energyneutrinos detected by the Ice Cube detector. We find that if the accretion shocks arepredominantly strong, neutrino background is more limiting to the possible gamma-ray emissivity of these objects. In case of weaker shock these cosmic rays can havenon-negligible contribution to the isotropic diffuse gamma-ray background.

One part of the thesis also deals with small galaxies, in particular the Small Mag-ellanic Cloud, and the production of cosmic rays in supernova remnants. This galaxywas detected in gamma-rays, but also has measurements of the lithium abundancesavailable. Galactic cosmic rays, produced in supernova remnants, should be the dom-inant cosmic-ray population in this galaxy. We show that even if we assume that theentire observed gamma-ray emissivity of this galaxy originates from galactic cosmicrays, we can still explain only a small fraction of the observed lithium. This leavesroom for the possible existence of other sources of lithium in the Small MagellanicCloud.

The thesis studies and links different products of cosmic-ray interactions withingalaxies and galaxy clusters. It is shown that in addition to the galactic cosmic raysaccelerated in supernova remnants, other still hypothetical cosmic rays, producedfor example in accretion or tidal shocks, can have a non-negligible contribution todifferent measurements.

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Progress Report

TESTING EXTENDED THEORY OF GRAVITY BY Sgr A*

A. D’Addio1, S. Capozziello1,2,3, P. Jovanovic4 and V. Borka Jovanovic5

1Dipartimento di Fisica ”E. Pancini”, Universita di Napoli ”Federico II”,Compl. Univ. di Monte S. Angelo, Edificio G, Via Cinthia, I-80126, Napoli, Italy

2Istituto Nazionale di Fisica Nucleare (INFN) Sez. di Napoli,Compl. Univ. di Monte S. Angelo Edificio G, Via Cinthia, I-80126, Napoli, Italy

3Gran Sasso Science Institute, Viale F. Crispi, 7, I-67100, L’Aquila, Italy4Astronomical Observatory, Volgina 7, P.O. Box 74, 11060 Belgrade, Serbia

5Atomic Physics Laboratory (040), Vinca Institute of Nuclear Sciences,University of Belgrade, P.O. Box 522, 11001 Belgrade, Serbia

E-mail : [email protected], [email protected], [email protected],[email protected]

Here we analyze an Extended Gravity Theory model, in which there is non-minimalcoupling between the geometry and a scalar field. We derived a particular theoryamong the class of scalar-tensor theories of gravity, and then tested it by studyingdynamics of S2 star around supermassive black hole at Galactic Center. We alsodiscuss the Newtonian limit of this class of scalar-tensor theories of gravity, as wellas its parameters. To constrain these parameters, we compare the observed orbit ofS2 star with our simulated orbit which we obtained theoretically with the derivedpotential.

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Progress Report

BRANEWORLD COSMOLOGY AND TACHYON INFLATION - RSIINUMERICAL MODELS

D. Delibasic, D. D. Dimitrijevic, G. S. Djordjevic, M. Milosevicand M. Stojanovic

Faculty of Sciences and Mathematics, University of Nis,Visegradska 33, 18000 Nis, Serbia

E-mail : [email protected], [email protected], [email protected]

A popular class of the inflationary cosmological models introduce a scalar field withnonstandard tachyonic Lagrangian of the Dirac-Born-Infeld (DBI) type. A potentiallyfundamental role of the tachyon fields in the braneworld cosmology was proposed by A.Sen. Our research is motivated by the second Randall-Sundrum (RSII) cosmologicalmodel. The main objective of the research is to formulate differential equations forinflationary model with DBI-tachyon field and RSII model with an additional radionfield. These systems of equations are not analytically solvable in general.

In this work, we used an approach based on different numerical methods to solvethe systems of differential equations for different inflationary scenarios, as well as tocompute the slow-roll and observational parameters. The slow-roll approximation isused only to estimate the initial conditions. The solutions for the dynamics of inflationis calculated numerically. The results are used to calculate the Hubble parameter, aswell as the observational parameters for random values of the free parameters in agiven range and the corresponding initial conditions.

The calculated numerical values of observational parameters are compared withthe results of observations obtained by the Planck Collaboration. Obtained results arein a good agreement with the astrophysical data and provide a better understandingof the role of strings and branes in modern cosmology.

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Progress Report

COSMOLOGICAL PERTURBATIONS IN NONLOCAL GRAVITY

I. Dimitrijevic1, B. Dragovich2, J. Stankovic3 and Z. Rakic1

1University of Belgrade, Faculty of Mathematics,Studentski trg 16, 11000 Belgrade, Serbia

2Mathematical Institute of the Serbian Academy of Sciences and Arts,Belgrade,Serbia

3Teacher Education Faculty, University of Belgrade, SerbiaE-mail : [email protected]

After discovery of accelerating expansion of the Universe, there has been a renewedinterest in gravity modification. One of promising approaches is nonlocal modificationwith the scalar curvature R in the action replaced by a suitable function F (R, ¤),where ¤ = 1√−g

∂µ√−ggµν∂ν is the Laplace-Beltrami operator. In particular we

analyze the modification in the form

S =∫ √−g

( R

16πG+H(R)F(¤)G(R)

)d4x, (1)

where F(¤) is an analytic function. Also we will discuss perturbations of this modelwith several backgrounds.

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Progress Report

NEW COSMOLOGICAL SOLUTIONS IN NONLOCALMODIFIED GRAVITY

I. Dimitrijevic1, B. Dragovich2, Z. Rakic1 and J. Stankovic3


2Mathematical Institute of the Serbian Academy of Sciences and Arts,Belgrade,Serbia

3Teacher Education Faculty, University of Belgrade, SerbiaE-mail : [email protected]

In this contribution we consider model of nonlocal gravity without matter, givenby the following action

S =1

16πG

∫ √R− 2Λ F (¤)

√R− 2Λ

√−g d4x, (2)

where R is Ricci scalar curvature, Λ cosmological constant and F (¤) = 1+F(¤) = 1+∞∑

n=1

fn¤n. The corresponding Einstein equations of motion are derived and presented.

Using ansatze we can solve equations of motion and get some cosmological solutions.

37



Progress Report

ASTRONOMICAL WORK OFANATOLY ANATOLYEVICH MIHAJLOV (1941-2016)

M. S. Dimitrijevic


Anatoly Anatolyevich Mihajlov (20 October 1941, Krasnoyarsk - 27 September2016, Belgrade) was educated in Leningrad. After graduating from the Faculty ofPhysics 1967, he worked in the State Optical Institute. In 1975 he married JelicaJokanovic Mihajlov, and in 1976 the family settled in Belgrade. He worked at theInstitute of Physics, where he created the new laboratories for Physics of nonidealplasma, and the first in the region Laboratory of Physics of the ionosphere and itsinteraction with the solar emission.

He cooperated with the Astronomical Observatory and among the large numberof his scientific papers, cited many hundreds of times, 36 are in the internationalastronomical journals of the highest rank. In these works he analyzed the effectsof various atomic collisional processes on the radiation of the Sun, stars, and whitedwarfs.

Mihajlov was awarded for scientific work by the Institute of Physics in 1994 and bythe Astronomical Observatory in 1999. He was a member of the Management Boardof the Eurasian Astronomical Society, based in Moscow, and founded its Serbianbranch and a representative office in Belgrade 2008. He was also a member of theInternational Astronomical Union.

In this contribution his work and life will be presented with the emphasis on hiswork in astronomy and his connections with the Belgrade Astronomical observatory.

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Progress Report

PROBING THE GALACTIC HABITABILITY TIME SCALES

V. Djosovic1, B. Vukotic2 and M. M. Cirkovic2

1Department of Astronomy Faculty of Mathematics University of Belgrade,Studentski Trg 16, 11000 Belgrade 38, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected], [email protected]

There has been a surge of interest in numerical modeling of habitability in the lastcouple of years. Here we implement a simple probabilistic toy model of the Galacticdisk astrobiological history. Characteristic times for the emergence of catastrophicand colonization events are varied in the relevant range. The results averaged overmultiple runs show an emerging pattern of astrobiological landscape which can be usedto quantify the probability of various models for evolution and expansion of Galacticcivilizations. Various approaches to building numerical models of Galactic habitabilityare briefly compared, and some potentially fruitful direction for the further workoutlined.

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Progress Report

STELLAR KINEMATICS AROUND GALACTIC CENTER

S. Gravina1, S. Capozziello1,2,3, D. Borka4 and V. Borka Jovanovic4

1Dipartimento di Fisica ”E. Pancini”, Universita di Napoli ”Federico II”,Compl. Univ. di Monte S. Angelo, Edificio G, Via Cinthia, I-80126, Napoli, Italy

2Istituto Nazionale di Fisica Nucleare (INFN) Sez. di Napoli,Compl. Univ. di Monte S. Angelo Edificio G, Via Cinthia, I-80126, Napoli, Italy

3Gran Sasso Science Institute, Viale F. Crispi, 7, I-67100, L’Aquila, Italy4Atomic Physics Laboratory (040), Vinca Institute of Nuclear Sciences,

University of Belgrade, P.O. Box 522, 11001 Belgrade, SerbiaE-mail : [email protected], [email protected], [email protected],

[email protected]

In this paper we discuss the deviations between the observed and Keplerian orbitof S2 star around the Galactic Center (GC), using the gravitational potential thatwe derived from the modified theories of gravity. S2 star is one the brightest amongS-stars, with the short orbital period, and also with the smallest uncertainties indetermining the orbital parameters. So we use it as a good candidate for investigatingthe precession of the orbit, deviations from the Keplerian orbits, as well as stellarkinematics around supermassive black hole at GC.

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Progress Report

CORRESPONDENCE OF VOJISLAV V. MISKOVIC ABOUT HISDOCTORATE WITH MILUTIN MILANKOVIC, MIODRAG IBROVAC

AND OTON KUCERA

N. Janc1, V. Protic Benisek2, V. Benisek2, L. C. Popovic2,M. B. Gavrilov3 and S. B. Markovic3

1415 Old Trail Road, Baltimore, MD 21212, USA2Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia

3University of Novi Sad, Faculty of Sciences,Laboratory for Paleoenvironmental Reconstruction,Trg Dositeja Obradovica 3, 21000 Novi Sad, Serbia


Many letters documenting the correspondence between Vojislav V. Miskovic andleading scientists such as Milutin Milankovic, Miodrag Ibrovac and Oton Kucerafrom 1916 to 1952 have been preserved. Most often Miskovic corresponded withMilutin Milankovic, who was informed about all phases of his Ph.D, from its writing,to its defense, promotion and publication. The title of Miskovic’s doctoral thesisin the mathematical sciences was “Statistical Methods in the Study of the Stars”(“Etudes de statistique stellaire”) and was defended on July 12, 1924 at the Universityof Montpelier in front of a panel chaired by Professor P. Humbert. Miskovic alsoinformed Miodrag Ibrovac about the dissertation and asked him to see the Secretaryof Education about the funding he needed to print the thesis. Miskovic then sentthis printed thesis to Milankovic, Ibrovac and Kucera. They congratulated him andpraised his work. Milankovic read it and passed it to Professor Anton Bilimovic,who was one of Miskovic’s committee members at the University of Belgrade. Kuceraintended to write a review of Miskovic’s dissertation in “Nastavni Vjesnik” (“Teacher’sNewsletter”), but the printing of the magazine was postponed and it was not sentalong with the letter, as Kucera had intended for.

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Progress Report

REGULUS OBSERVED WITH VLTI/AMBER

S. Jankov1, M. Hadjara2,3 and R. G. Petrov3

1Astronomical Observatory, Volgina 7, 11060 Belgrade, SerbiaE-mail : [email protected]

2Universidad Catolica del Norte, Av. Angamos 0610 Antofagasta, ChileE-mail : [email protected]

3Universite de Nice-Sophia Antipolis, Campus Valrose, 06108 Nice cedex 2, FranceE-mail : [email protected]

The rapidly rotating primary component of Regulus A system has been observed,for the first time, using the technique of differential interferometry at high spectralresolution. The observations have been performed across the Brγ spectral line withthe VLTI/AMBER focal instrument in high spectral resolution mode (R ≈ 12 000) at≈ 80m (projected on the sky) Auxiliary Telescopes triplet baseline configurations. Weconfirm, within the uncertainties, the results previously obtained using the techniquesof classical long-baseline interferometry, although the question of anomalous gravitydarkening remains open for future study.

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Progress Report

REVEALING SHOCK AND COSMIC-RAY PROPERTIES FROMBALMER EMISSION IN SUPERNOVA REMNANTS:

THE CASE OF TYCHO

S. Knezevic, R. Lasker, G. van de Ven, G. Morlino, J. C. Raymond,C. Bailer-Jones, J. Font and J. Mendez-Abreu

Weizmann Institute of Science, P.O. Box 26, Rehovot 76100, IsraelE-mail : [email protected]

We present Hα spectroscopic observations and detailed modelling of the Balmerfilaments (Hα-line profiles) in Tycho’s supernova remnant. For this purpose, weused GHαFaS on the William Herschel Telescope with a 3.4′× 3.4′ field-of-view, 0.2′′

pixel scale, spectral coverage of 392 kms−1 and instrumental dispersion of 8.1 kms−1.We find that the narrow Hα-line width is (54.8±1.8) kms−1 at the 95% confidencelevel, much broader than the intrinsic (thermal) ≈ 20 kms−1 and we explain it withCR proton acceleration. We also find wide-spread Bayesian evidence for an ad-ditional intermediate-line emission of a neutral-induced precursor, with a width of(180±14) kms−1. Therefore, our results reveal the existence of and interplay betweenshock precursors in Tycho’s remnant. Furthermore, we intend to present observationsof the broad-Hα component (∼ 1000 kms−1) in Tycho’s shock filaments for whichwe used OSIRIS narrow-band tunable filter imaging at Grand Telescope Canaria.Observing exactly the same parts of the remnant with both GHαFaS and OSIRIS,resolving narrow and broad Hα components, and using the state-of-the-art collision-less shock models, we place tight constrains on CR properties (acceleration efficiencyand particles’ maximum momentum) in Tycho’s remnant.

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Progress Report

POSSIBILITIES AND OPTIMIZATION OF LANDING ON THESOUTHERN HEMISPHERE OF MARS

D. Marceta

University of Belgrade, Faculty of Mathematics,Studentski trg 16, 11000 Belgrade, Serbia


Almost 40 years after the first successful landing on Mars, exploration of its surfacestill presents enormous scientific and technological challenge. This particularly holdsfor the Mars southern highlands where no successful landings have been achieved upto date. On the other hand, in the northern lowlands there have been 7 successfullandings. This difference is the consequence of the so-called global or hemisphericdichotomy of Martian topography, which is a unique characteristic in the Solar system.Due to the difference in the surface elevations, the vehicle that might try to land onthe southern highlands would have a thinner layer of the atmosphere that can usefor the dissipation of its kinetic energy. The main objective of this dissertation is todetermine whether it is possible to land on the southern highlands, without advancingthe technology which was used for the previous landings on Mars and to identify theoptimal conditions for such landing.

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Progress Report

A STUDY OF QUASI-THERMAL NOISE ANDSHOT NOISE IN SPACE PLASMAS

M. M. Martinovic1, A. Zaslavsky2, M. Maksimovic2 and S. Segan1


2LESIA, Observatoire de Paris, UPMC, Universite Paris Diderot, CNRS,92190 Meudon, France

E-mail : mihailo [email protected]

The quasi-thermal noise spectroscopy is an accurate method of determination ofdensity and temperature in space plasmas. Quasi-therma electrostatic fluctuations areobserved close to electron plasma frequency for both electrons and protons. Besideinducing the fluctuating electric field, some of the electrons are impacting the antennasurface. The signal caused by this population is directly proportional to the flux ofplasma electrons impacting the antenna and is dominant if the antenna has a largesurface area. In this work, we use the orbit limited theory to calculate the incomingparticle flux for a non-thermal plasma described by κ velocity distribution function,commonly measured in the solar wind. The increase in the particle collection bycylindrical and spherical objects is quantified and presented as a function of the surfaceelectrostatic potential and the fraction of supra-thermal particles. The comprehensivestudy of data on STEREO mission is also performed, as it is motivated by the factthat the electron analyzers are malfunctioning since launch and no information onthermal electrons is available. Results obtained are verified by comparing with theresults from Wind, showing a good match between the values measured by the twospacecraft.

45



Progress Report

RECONSTRUCTING FORMATION AND EVOLUTION OFCOMPACT DWARF CANDIDATES IN CLUSTERS OF GALAXIES

N. Martinovic and M. Micic

Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected]

We present results from recently published paper in which we have identifieda possible solution for the question of formation and evolution of compact dwarfgalaxies in clusters of galaxies. We will present a process, involving halo catalogueand particle data, used to reconstruct formation and evolution histories from Illustris-1 cosmological simulation for objects which were not found in merger tree data. Thishas lead to the discovery of two channels for formation of compact objects in vicinityof the simulation’s most massive cluster galaxies.

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Progress Report

IS COSMOLOGICAL CONSTANT TRANSIENT PHENOMENA?

Z. Mijajlovic and N. Pejovic

Faculty of Mathematics, Studentski trg 16, 11000 Belgrade, SerbiaE-mail : [email protected], [email protected]

We applied in Mijajlovi’c et al. (2012) the theory of regularly varying functionsin asymptotic analysis of solutions of Friedmann equations:

(a

a

)2

=8πG

3ρ− kc2

a2, Friedmann equation,

a

a= −4πG

3

(ρ +

3p

c2

), Acceleration equation,

ρ + 3a

a

(ρ +

p

c2

)= 0, Fluid equation.

Functions appearing in these equations represent basic cosmological parameters: thescale factor a = a(t), the energy density ρ = ρ(t) and the pressure p = p(t). In thispaper we discuss a pressureless flat universe with nonzero cosmological constant Λ.For this type of universe Carroll, Press and Turner introduced in Carroll et al. (1992)a function F (Ω), Ω = Ω(t) is the density parameter, by which other cosmologicalparameters can be expressed. For the convergent Ω(t) at infinity we proved that thecosmological constant Λ is a transient phenomena, i.e. Λ → 0 as t → ∞. We alsoproved that in both cases, with the cosmological constant or without it, the asymp-totics of the cosmological parameters a(t), p(t), ρ(t) and the deceleration parameterq(t) are same.

References

Carroll, S. M., Press, W. H., Turner, E. L.: 1992, Ann. Rev. Astron. Astrophis. J.,30, 499.

Mijajlovic, Z., Pejovic, N., Segan, S., Damljanovic, G.: 2012, Appl. Math. andComput., 219, 1273–1286.

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Progress Report

IMPACT OF YARKOVSKY EFFECT AND MEAN-MOTIONRESONANCES ON MAIN BELT ASTEROID’S TRANSPORT

I. Milic Zitnik


The long-term dynamics of main belt asteroids is governed by complex interactionamong the gravitational and non-gravitational phenomena. A detailed study aboutthis interaction has not been performed yet. The most important gravitational mech-anisms are orbital resonances and the most important non-gravitational effects are theYarkovsky and the Yarkovsky-O’Keefe-Radzievskii-Paddack forces. This motivatedus to study the effect of different mean-motion resonances (MMRs) on the mobility ofan asteroid’s semimajor axis due to the Yarkovsky effect. We established our findingsabout the effect of 11 two-body MMRs with Jupiter, on the mobility of an asteroid’ssemimajor axis caused by the Yarkovsky effect. This study was accomplished usingnumerical integrations of test particles. The obtained results revealed that MMRscould either speed up or slow down the drift in the semimajor axis. Moreover, thisallowed us to determine the distribution that represents the best data obtained fortime delays, dtr, caused by the resonances on the mobility of an asteroid. We found acertain functional relationship that describes dependence of the average time lead/lag< dtr > on the strength of the resonance, SR, and the semimajor axis drift speed,da/dt. As the Yarkovsky effect scales as 1/D, an important consequence of thisrelationship was that average time lead/lag < dtr > is directly proportional to thediameter D of an asteroid. Also, we analyzed how the time spent inside the resonancedepends on orbital eccentricity, and proposed the relation that taking this parameterinto account as well.

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Progress Report

INFLUENCE OF THE SOFTENING LENGTH ON STABILITYOF SPIRAL GALAXIES IN N-BODY SIMULATIONS

S. Milosevic1, M. Micic2, N. Martinovic2, M. Smole2 and A. Mitrasinovic2

1Department of Astronomy, Faculty of Mathematics, Studentski trg 16,11000 Belgrade, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected], [email protected],

[email protected], [email protected]

Softening length is a numerical parameter which is included in calculation of gravi-tational force between two bodies, in N-body simulations, in order to avoid divergenceon small distances and ensure smooth function for gravitational potential. It dependson number of particles in simulations, mass of the particles, dimension of the systemand timestep. In this paper we presented how specific choice of values for the soft-ening length affects stability of spiral galaxies like Milky Way and M31. Galaxies inour simulations are consisted of three components: bulge, disk and dark matter halo.Components have different number of particles, dimension and particle mass. Differ-ences between rotatiton curves, density profiles and energy conservation for differentvalues of softening length were investigated.

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Progress Report

BAR DETECTION IN N-BODY SIMULATIONSUSING FOURIER ANALYSIS

A. Mitrasinovic1, M. Micic1, N. Martinovic1, M. Smole1 and S. Milosevic2

1Astronomical Observatory, Volgina 7, 11160 Belgrade, Serbia2Department of Astronomy, Faculty of Mathematics, Studentski trg 16,

11000 Belgrade, SerbiaE-mail : [email protected], [email protected], [email protected],


Bars are considered to be a common feature in disk galaxies. Since their formationand evolution can be fully studied only using N-body simulations, it is important torefine and improve methods for bar detection and determination of its propeties. Themost practical and frequently used method is based on fourier analysis of the face-ondensity distribution of disk particles. However, criteria for positive bar detection anddetermination of its parameters are usually biased toward long and strong bars orcases where no other feature is present in the disk (e.g. spiral structure, tidal tails).

We propose a new criterion which enables positive bar detection for both weak andshort bars, and also successfully distinguishes bar region from other possibly presentfeatures.

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Progress Report

DISSECTING THE GALACTIC TeV EXCESS

J. Petrovic1, T. Prodanovic1 and M. Kovacevic2

1Department of Physics, Faculty of Science, Trg Dositeja Obradovica 4,Novi Sad, Serbia

2Department of Physics and ICRA, Sapienza University of Rome,Piazzale Aldo Moro 5, 00185 Rome, Italy

E-mail : [email protected], [email protected],[email protected]

Diffuse gamma-ray emission has been studied in detail by the Fermi LAT tele-scope. Most of the emission comes from the interactions of galactic cosmic rays withthe interstellar gas, as well as leptonic cosmic rays. However, at least a portionof the emission belongs to unresolved point sources. Another eye-on-the-sky in thepast years, focused on the high energy range (TeV), was the Milagro Cherenkov tele-scope and its last report of the diffuse galactic disk emission for the region 30 ≤l ≤ 65, −2 ≤ b ≤ 2 states a gamma-ray differential flux differential flux ofFγ,diff,MGO = 4.1 ± 1.0 × 10−12 photons TeV−1 cm−2 s−1 sr−1 on 12 TeV, adoptinga spectral index of 2.62. We compare this value to the Fermi LAT diffuse modeland find an excess in gamma-rays dubbed the TeV excess. After inserting all knownpoint sources found in catalogues, such as the Fermi LAT and TeVCat catalogues,the TeV excess remains. Our goal was to give possible explanations for this excess bymodeling point source candidates - pulsars and supernova remnants, that could stillbe unresolved.

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Progress Report

COSMIC-RAY ACCELERATION IN GALACTIC INTERACTIONSAND ITS IMPLICATIONS

T. Prodanovic1 and D. Donevski2

1Department of Physics, Faculty of Sciences, University of Novi Sad,Trg Dositeja Obradovica 4, 21000 Novi Sad, Serbia

2Laboratoire d’Astrophysique de Marseille, Aix-Marseille University,38 Rue Frederic Joliot Curie, 13013 Marseille, France


It has been shown that galactic interaction and mergers can result in large-scaletidal shocks that propagate through interstellar gas. As a result, this can give rise to anew population of cosmic rays, additional to standard galactic cosmic rays present instar-forming galaxies. We investigate the impact of this tidal cosmic-ray populationon the nucleosynthesis of lithium in interacting systems (such is the Small Magellanicclod for example) in the context of the cosmological lithium problem. Moreover wealso demonstrate that the presence of these tidal shock-waves and may also havefar reaching consequences on our understanding of galactic evolution by affectingthe far-infrared radio correlation observed in star-forming galaxies and impactingstar formation rates estimates. We discuss how these effects can be further probedthrough numerical simulations and used to on high-redshift observations of interactingsystems.

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Progress Report

EXCLUDING INTERLOPERS FROM ASTEROID FAMILIES

V. Radovic and B. Novakovic

Faculty of Mathematics, University of Belgrade,Studentski trg 16, 11000 Belgrade, Serbia


Asteroid families are valuable source of information to many asteroid-related re-searches, assuming a reliable list of their members could be obtained. However, asthe number of known asteroids increases fast it becomes more and more difficult toobtain robust list of members of an asteroid family. Here we are proposing a newapproach to deal with the problem, based on the well known Hierarchical ClusteringMethod (HCM). An additional step in the whole procedure is introduced in orderto reduce a so-called chaining effect. The main idea is to prevent chaining throughan already identified interloper. We show that in this way a number of potentialinterlopers among family members is significantly reduced. Moreover, we developedan automatic on-line based portal to apply this procedure, i.e to generate a list offamily members as well as a list of potential interlopers. The Asteroid Families Portal(AFP) is freely available to all interested researchers.

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Progress Report

EARLY GROWTH OF SUPERMASSIVE BLACK HOLESAND GRAVITATIONAL WAVE RECOIL

M. Smole1, M. Micic1, N. Martinovic1, A. Mitrasinovic1 and S. Milosevic2

1Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia2Department of Astronomy, Faculty of Mathematics, Studentski trg 16,



Formation mechanism of supermassive black holes (SMBH) observed in the earlyUniverse is still not fully understood. At hight redshifts black holes (BHs) primarilygrow through mergers with other BHs and through episodes of gas accretion triggeredby major mergers of dark matter haloes. Combining Millennium-II and MillenniumN-body cosmological simulations we find that BH remnants of Population III starscould explain BH mass function observed at redshift z = 6 if effective Eddington ratiois fixed at fEdd = 3.7.

During BH mergers asymmetric emission of gravitational radiation can lead to BHkicks. Gravitational wave recoil can completely eject BH from it’s host if the kickvelocity is larger than the escape velocity from the galaxy. This process could affectformation of SMBHs if BH mergers are dominant growth mode. Recoiling BHs areinvestigated in analytical and numerical models of various host galaxies.

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Progress Report

RADIATIVE AND COLLISIONAL ATOMIC/MOLECULARDATA FOR ASTROPHYSICS

V. A. Sreckovic1, Lj. M. Ignjatovic1, D. Jevremovic2,V. Vujcic2,3 and M. S. Dimitrijevic2,4

1Institute of Physics, Belgrade University, Pregrevica 118,Zemun, 11080 Belgrade, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia3Faculty of Organizational Sciences, University of Belgrade

4LERMA, Observatoire de Paris, UMR CNRS 8112, UPMC,92195 Meudon Cedex, France

E-mail : [email protected], [email protected], [email protected],[email protected], [email protected]

Accurate spectroscopic diagnostics and modelling require different kinds of atomic/molecular input data. The access to such data via online databases is essential. Thiscontribution describes how such data are collected, stored and which limitations ex-ist. Also, here we summarize challenges of atomic/molecular databases and point outour experiences, in a/m databases development. Also, we present overview of futuredevelopments and needs in the areas of collisional processes, radiative transfer anddata storing.

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Progress Report

PECULIAR MID-INFRARED MORPHOLOGY OFACTIVE GALACTIC NUCLEUS IN CIRCINUS

M. Stalevski


Recent high angular resolutions finally resolved the mid-infrared (MIR) structureof nearby active galactic nuclei (AGN). Surprisingly, they revealed that a major frac-tion of the MIR emission comes from the polar regions, at odds with the expectationbased on the AGN unification which postulates a dusty torus in the equatorial re-gion. New highest quality MIR images of archetypal AGN in Circinus galaxy wereobtained as part of the science verification program of the upgraded VISIR instru-ment mounted on the Very Large Telescope. A striking feature of these images isa prominent bar extending 40 pc from both sides of the nucleus in the polar direc-tion. Motivated by the observation across a wide wavelength range and on differentspatial scales, we propose a dust emission model for AGN in Circinus consisting of acompact dusty disk and a large-scale dusty cone shell, illuminated by a tilted accre-tion disk with anisotropic emission pattern. Undertaking detailed radiative transfersimulations, we demonstrate that such a model is able to explain the peculiar MIRmorphology and account for the entire spectral energy distribution. Our results callfor caution when attributing dust emission of unresolved sources entirely to the torusand warrant further investigation of the MIR emission in the polar regions of AGN.

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Progress Report

THE NATURE OF EDUCATIONAL ACTIVITIES IN PLANETARIUMAND ITS CONTRIBUTION TO THE ADVANCEMENT OF

ASTRONOMICAL EDUCATION

N. Stanic

Astronomical Society Rudjer Boskovic, Kalemegnan,Gornji grad 16, 11000 Belgrade, Serbia


The outdoor educational activities in planetarium, in the frame of the educationalprogram in Planetarium are common part of a teaching practice in our country andthey have been an important educational resource for schools and preschools since the1970’s. Based on studies of planetarium learning process (PLP), planetarium educa-tional activities research (PEAR) and its implications enabled deeper connection ofastronomy and pedagogy as well as astronomy and psychology. Theoretical-empiricalPEAR research was simultaneously conducted in 60 places and 33 primary schoolsin Serbia, with 152 geography and physics teachers, as well as 811 sixth grade stu-dents as participants. Practical contribution of PEAR refers to: defining of PLPsocio-cultural potentials and weaknesses; identification and mapping of planetariumresources (on global, local and virtual level); suggestion for three indicators for qual-ity of PLP number of schools per planetarium (for particular region, country orcity), number of school’s annual planetarium visits (for particular planetarium) andnumber of planetarium visits per student during the primary school (total numberof different planetarium visits); PLP scenario with scientific terms index; knowledgetest in astronomy with answers (with sub test in declarative, conditional, proceduraland conceptual knowledge) which could be used in teaching practice in geography andphysics. Conducted PEAR showed that several critical variables could be extractedand observed in order to describe and measure planetarium’s influence on the learningprocess in terms of quality advancement of geography and physics teaching: frequencyof planetarium visits and student’s achievement in the astronomy knowledge test.

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Progress Report

BOSCOVICH’S COMPREHESION OF ABSOLUTEAND RELATIVE MOVEMENT

D. Stoiljkovich1 and R. J. Anderton2

1University of Novi Sad, Faculty of Technology, Serbia2United Kingdom

E-mail : [email protected], [email protected]

Boscovich (1711-1787) differentiates between absolute and relative movements.”We do not observe absolute motions, but merely relative motions with respect tothe Earth, or at most those with respect to the planetary system or the system ofall the fixed stars”. He described the relative movements of two bodies by parallel,crosswise and passing over (evading) paths. In this work, we present the mathematicalexpressions for the relative rates of two bodies moving at constant rate in paralleland crosswise trajectories. It follows, however, that relative rates are not constantbut increase on recession of two bodies and decrease as two bodies approach, evenwhen there is no force acting between them. Based on these comprehensions sometheoretical aspects and practical applications for rate measurements are considered.

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Progress Report

PROJECT OF PROMOTION OF ASTRONOMY SKY IS THE LIMIT

Z. Tomic

Astronomical Society Eureka, Kralja Petra Prvog 3, 37000 Krusevac, SerbiaE-mail : [email protected]

Project sky is the limit is realized within the SUPERSTE program as one of theten winners of the program for 2016. The project itself is realized in rural areas ofKrusevac municipality, where public observation and lectures are organized. In thisway, in addition to promoting of astronomy as science, astronomy is promoted also asa potential offer for rural tourism in Krusevac area. Also first astronomical camp aswell as the training of 25 young people to become young ”ambassadors” of astronomywill be done, so they can work on promotion of astronomy in Krusevac in future. Theproject will be completed by the end of 2017. This paper presents the results achievedin the project so far.

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Progress Report

MILAN G. NEDELJKOVIC - THE FOUNDER AND FIRST DIRECTOROF THE OBSERVATORY OF THE GRAND SCHOOL

(ON THE OCCASION OF 160th - ANNIVERSARY OF THE BIRTH)

V. Trajkovska and S. Ninkovic

Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected]

In this very year, 2017, the Astronomical Observatory in Belgrade has a few ju-bilees, among them 130 years from the foundation and 160 years from the birth ofMilan G. Nedeljkovic, the founder and first director of the Observatory of GrandSchool. These events appear as a special opportunity to emphasize the most impor-tant, and also those less known, facts from life and activity of Milan G. Nedeljkovic(1857-1950), professor of astronomy at the Grand School, as well as to offer a reviewconcerning the activity of one of the oldest scientific institutions in Serbia, whichstarted its activity as a ”Provisorial Observatory” and in which several institutionsengaged in the field of astro - and geosciences have their roots, through an analysisof his Observatory reports.

Milan G. Nedeljkovic obtained a scholarship and studied physics and astronomywith meteorology at Sorbonne in Paris and as a great enthoussiast he wanted to applythe acquired knowledge in his own country. He founded the Observatory in 1887 andin this way contributed to professional activities in astronomy in Serbia. It is hismerit that high-quality astronomical instruments were obtained from Germany aswar reparations after the First World War which was the main observational base ofthe new Astronomical Observatory. For almost 37 years he led the Observatory.

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Progress Report

ASTRONOMY COMPETITIONS AND THEIR ROLE INASTRONOMY EDUCATION IN SERBIA

S. Vidojevic1, S. Ninkovic2, B. Simonovic3, I. Beslic4, S. Andjelkovic5,V. Sarkovic4, P. Obradovic6, M. Puric5 and A. Miladinovic4

1State University of Novi Pazar, Department of Mathematical Sciences,Vuka Karadzica bb, 36300 Novi Pazar, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia3Astronomical Society “Rudjer Boskovic“, Kalemegdan,

Gornji grad 16, 11000 Belgrade4Faculty of Mathematics, Department of Astronomy,

Studentski trg 16, 11000 Belgrade, Serbia5Faculty of Phisics, Studentski trg 12, 11000 Belgrade, Serbia

6School of Electrical Engineering, University of Belgrade,Bulevar kralja Aleksandra 73, 11120 Belgrade, Serbia

E-mail : [email protected], [email protected], [email protected],[email protected], [email protected], [email protected],[email protected], [email protected], [email protected]

For many years astronomy was taught as a separate subject (one hour per week)in the final form of the secondary school education. However, since about quartera century ago it has been taught as part of physics, only in special schools (likeMathematical High School in Belgrade) it still exists as a separate subject in the finalform (also one hour per week). In order to fill the gap NAOC (National AstronomicalOlympic Committee) organises extra teaching of astronomy. In this way it becomespossible to prepare the interested pupils for astronomical contests both within Serbiaand international ones. During the period between the two last National Conferences,from 2014 to 2017, contestants from Serbia participated in the following internationalcontests: 8th IOAA (International Olympiad in Astronomy and Astrophysics) inRomania 2014, 9th IOAA in Indonesia 2015, 10th IOAA in India 2016 and the Saint-Petersburg Olympiad 2014− 2016.

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Progress Report

ILLUMINANCE AND VISIBILITY AT TWILIGHTS

I. Vince


There is an increasing require of community for information about some astronom-ical events, since they have an important influence on human everyday activities. Themost frequently needed information are the rise and set times of the Sun and Moon,the beginning and ending times of twilights, duration of daylight, azimuth and heightabove the horizon of the Sun or Moon, the amount of natural light at a designatedtime of day, at twilight or night etc. The determination of these quantities is the dutyof astronomers. In this lecture I would like to concentrate on the determination ofillumination of outdoor objects by natural light sources: the Sun, the Moon and therest of celestial objects. It is very important information since it determines, alongartificial light sources, the visibility of outdoor objects.

In every-day situations the visibility can be very important to detect, recognize oridentify a given object. One of such every-day situation is the roadway traffic, were thegood visibility is very important for safe driving conditions. Unfortunately, duringthe twilights and night this conditions decline very rapidly. Degradation of visualperformance during these periods of the day is a leading contributor to increasingnumber of roadway accidents.

Determination of the visibility under which the accident occurred is interesting forjudicial system, insurance companies, low firms etc. Therefore it is often necessary toreconstruct the visibility at given date, time and geographical position. The visibilityis a very complex phenomenon, which depends on many factors, first of all fromilluminance, luminance and vision. One possibility to reconstruct the visibility is itsmodeling. However, it is a very difficult problem due to highly complex physics oflight propagation from the source trough the Earth (inhomogeneous) atmosphere toan observed object and from the object to an observer trough air and other opticallayers (like fog, windscreen, spectacles etc.). Moreover, for a given observer (a driver,for instance), with a given acuity and a given contrast sensitivity, the ability todetect a given object (a car or a pedestrian, for instance) illuminated by natural lightdepends on adaptation luminance. In other words, the luminance difference requiredthe observer to detect an object on its background depends on the overall light levelto which the observer is adapted.

Due to time limitation of the lecture and to physical and mathematical complexityof visibility modeling, I intend to present only qualitatively the problem of visibilitydetermination during the twilights, utilizing some block diagrams and photographicillustration.

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Progress Report

THE FIRST YEAR OF THE MILANKOVIC TELESCOPE

O. Vince, S. Samurovic, R. Pavlovic, Z. Cvetkovic and G. Djurasevic


Astronomical station Vidojevica is our observational site since 2003. It accom-modates two telescopes - 60cm telescope, which is in function since 2011, and 1.4mtelescope, which is operational since last year. In this talk, we present the currentstatus of Vidojevica station with the special emphasis on the new 1.4m telescope. Weintroduce the Rulebook for time allocation for both telescopes.

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Progress Report

OPTICAL SUPERNOVA REMNANTS AND THEIR INFLUENCE ONSTAR FORMATION RATES DERIVED FROM Hα EMISSION

M. Vucetic

Faculty of Mathematics, University of BelgradeE-mail : [email protected]

In this dissertation we discuss influence of Hα emission from supernova remnants(SNRs) on Hα derived star formation rates (SFRs). We present the detection of 16optical SNR candidates in a part of nearby spiral galaxy IC342, and two more poten-tial SNRs in NGC 185 galaxy. The candidates were detected by applying [S ii]/Hαratio criterion on observations made with the 2 m telescope at Rozhen National As-tronomical Observatory in Bulgaria. Also, in this dissertation we present the mostup-to-date list of nearby galaxies with optically detected SNRs. When deriving Hαstar formation rates, assumption is that the radiation is coming from the ionized gassurrounding hot and young stars – H ii regions. In this case, emission from SNRscontaminates Hα flux used to derive SFR. We found that the contribution of SNRs’flux to the total Hα flux, for 18 galaxies in our sample of galaxies with optical SNRs,is 5± 5%. Due to the observational selection effects, the SNR contamination of SFRsderived herein represents only a lower limit. M83 is the galaxy with the most detectedoptical SNRs and in this galaxy SNRs account for 9 per cent of the total Hα emission.We expect that fraction similar to this would be close to the real contribution of SNRemission to the total Hα emission in spiral galaxies.

Using two dwarf galaxies as an example, Holmberg IX and NGC 185, we showthat the contamination of Hα flux by SNRs, or other sources, can be much larger,up to ten times higher than total Hα flux coming from H ii regions of the observedgalaxy.

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Progress Report

SPECTROSCOPICAL AND PHOTOMETRICAL ANALYSIS OFNEARBY GALAXIES OF DIFFERENT MORPHOLOGICAL TYPES

A. Vudragovic


Galaxies show high degree of organisation, proven by numerous scaling relations.However, most of these relations hold either for early- or late- type galaxies. Thereis a need for a study of galactic properties regardless of their morphological type, butdriven from the sample representative of the galactic morphology in the local Universe.HI blind surveys sample galaxies based solely on their gas content, regardless oftheir luminosity in the optical. This is why we have extracted our sample fromthe latest HI blind survey, the Arecibo Legacy Fast ALFA Survey (ALFALFA). Thefirst data release referring to the 40% of the planned survey was the alfa.40 catalog(Haynes et al. 2011), counting about 10 000 extragalactic sources. We have cross-matched this catalog with the sixth data release of the Galex Evolutionary Explorer(GALEX) and Two Micron All-Sky Survey (2MASS) catalogs to add ultraviolet andnear-infrared photometry. Our final sample counts 2180 galaxies with radio andoptical spectroscopy and ultraviolet through optical to near-infrared photometry.

Numerous empirical relations between galactic properties imply that there is afinal number of parameters whose continuous change is responsible and may describediversity of galactic types in the local Universe. The question that naturally arisesis how many independent parameters are sufficient to describe galaxies we see today,i.e. the dimensionality of the problem and whether there is a single driving forceresponsible for their present distribution. To this end, we have applied the principalcomponent analysis in order to reveal the true dimensionality of the problem. Thismethod was applied earlier by Disney et al. 2008 on the sample of 200 galaxieschosen from the earlier HI blind survey, the HI Parkes All-Sky Survey (HIPASS).The authors analyse six galactic properties: dynamical mass, HI mass, luminosity,Petrosian radii R50 and R90 and the colour and find that there is a single dimensionthat is statistically significant. We have explored larger parametric space, including inaddition: stellar mass, age, metallicity, colours with both ultraviolet and near infraredcomponents, velocity dispersion, maximal rotational velocity and the mass of the darkhalo. The parameters measured in the thesis are: dynamical mass, velocity dispersion,age and metallicity. Other parameters are taken from the existing catalogs. We havesuccessfully reduced our parametric space to ten parameters: dynamical mass, stellarmass, HI mass, age, luminosity, colour with ultraviolet component, velocity dispersion,maximal rotational velocity and two Petrosian radii enclosing 50% and 90% of theflux, respectively. As the result of the principal component analysis, we have found

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three statistically significant components (dimensions), the first being the ”size” of thegalaxy, the second being the galaxy colour and the third being the galaxy age. Thefourth component, although not statistically significant is dominated by the maximalrotational velocity. To conclude, there are at least three and possibly four ”drivingforces” that could explain the diversity of galaxies we see today.

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Progress Report

THE APPLICATION OF NINE DEGREES OF FREEDOM SENSORIN DETERMINATION OF TELESCOPE POSITION

D. Vujicic1 and R. Pavlovic2

1Faculty of Technical Sciences in Cacak, University of Kragujevac, Serbia2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia


This paper shows the application of nine degrees of freedom sensor to determine theposition of the telescope. Nine degrees of freedom sensor is consisted of three sensors:gyroscope, accelerometer, and magnetometer. By using DCM algorithm for sensordata fusion, Euler angles are calculated, upon which the coordinates of horizontalcoordinate system are calculated as well. The coordinates of equatorial coordinatesystem are retrieved by using these coordinates together with time data and sensorlocation, which can be gotten either via GPS or by manually entering them. The PCapplication is written in C# programming language for retrieval of data from sensorand calculation of horizontal and equatorial coordinates. Furthermore, the errors andimprecisions that have emerged are explained, together with some of the ways of theirelimination.

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Progress Report

DENSITY PROFILE OF THE MILKY WAY: COMPARISON OFDYNAMICAL MODEL AND MONTE CARLO METHOD FOR

DETERMINING STELLAR SPACE DENSITIES

L. Zivadinovic, S. Milosevic and D. Milic

Department of Astronomy, Faculty of Mathematics,Studentski trg 16, 11000 Belgrade, Serbia

E-mail : lazar [email protected], [email protected],[email protected]

We derived stellar space density of K giants in Milky Way in direction of galacticcenter and south galactic pole using Monte Carlo approach for solving equations ofstellar statistics. For luminosity function of K giants we assumed gaussian distribu-tion of with mean magnitude of = 1 and standard deviation σ = 0.7. Monte Carlomethod for solving equation of stellar statistics is based on randomly assigning ab-solute magnitudes from assumed luminosity function corrected for Malmquist bias tostar with measured apparent magnitude, which leads to randomly assigned distancemodules. The mean value of this quantity is used to calculate distance. This waywe estimated mean stellar space density in given direction. We compared deriveddensities in direction of galactic pole, where influence of extinction is negligible todensities derived in direction of galactic center, where influence of extinction can notbe neglected. Also we compared our results with density profiles derived from n-bodysimulation of Milky Way like galaxy in isolation.

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Posters



Poster

OVID, FASTI, SUN AND STARS

A. Bajic1 and M. S. Dimitrijevic1,2

1Society for Archaeoastronomical and Ethnoastronomical Research “Vlasici”,Belgrade, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected]

At the beginning of January 2017, the translation on Serbian, by the authorsof this contribution, of Ovid’s book “Fasti”, has been published by the Society forArchaeoastronomical and Ethnoastronomical Research ”Vlasici”. Fasti of PubliusOvid Naso has not been translated into Serbian so far, but the english translationwas widely available on the Internet. However, one fact has to be taken into account:reading in a foreign language, which the reader knows well, will be understandable.However, the flow of free associations will not be as fast as if it was read in its mothertongue and it will not have a full emotional response to the information it receives.This is well known to psychologists and psychiatrists, neurologists and lawyers: thepolygraphic examination can not be performed in a foreign language, the apparatuswill not be able to record those fine variations of the emotional response. If it is readin mother tongue, it is easier to understand the different layers of the message in thetext.

On the other hand, each translation necessarily contains a personal note, since thetranslator gives his personal view of the text. Therefore, translations and translatorsshould be more.

This translation was made primarily for personal curiosity of translators. Membersof the Society for Archaeoastronomical and Ethnoastronomical Research ”Vlaii” werenaturally interested in the matter, given in this Ovid’s work: this is the religiouscalendar of ancient Rome, based on the astronomically significant risings and settingsof the Sun and stars, during the morning or evening dusk, just before the sunrise orimmediately after the sunset. Ovid gives over forty holiday dates, firmly connectedto certain astronomical events. In such a way, he offered significant material forexploring the astronomical knowledge available to the Romans in the time betweenold and new era. At the same time, he made that the task of future translatorsin all possible languages is more difficult, since one, who has to translate this text,must understand the astronomical data in it and must be able to explain them to thereader.

The translation on the Serbian language, of the Ovid’s “Fasti”, which will be pre-sented in this contribution, has provided a new insights into astronomical knowledgeand ways of acquiring and preserving these knowledge in ancient Rome.

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Poster

TWO TYPES OF DARK MATTER DISTRIBUTIONIN EARLY-TYPE GALAXIES

M. Bılek1 and S. Samurovic2

1Astronomical Institute, Czech Academy of Sciences,Bocnı II 1401/1a, CZ-14100 Prague, Czech Republic

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected]

If one wants to explain the observed dynamics of galaxies, one is faced with thefact that gravitational force needed is greater than that which is produced by thevisible matter. This leads to the introduction of dark matter (DM) hypothesis. Inthis contribution we describe our sample of 15 early-type galaxies (ETGs) whichincludes both ellipticals and lenticulars. For all the galaxies in our sample we extractfull kinematic profiles out to several effective radii: we rely on globular clusters (GCs)and we calculate the mass-to-light ratios of all the galaxies using the Jeans equation.We parametrize the gravitational field by that produced by the stars and a Navarro-Frenk-White DM halo. We focus on the relation between the dynamically inferredgravitational acceleration and the acceleration expected from the distribution of thevisible matter (the acceleration relation, AR). The AR is nearly universal for thespiral galaxies, in agreement with the MOND modified dynamics theory. Up to now,observational difficulties precluded investigating the AR in the ETGs. Here we showthat a few of our ETGs also follow very tightly the AR for the spiral galaxies, while themajority shows substantial deviations. That the first group might be spiral galaxiesthat lost their gas support the facts that they rotate, have disky isophotes, appearmostly very elongated and have blue colors. The galaxies deviating from the AR forthe spirals either disprove MOND or contain unobserved matter.

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Poster

FAST VARIABILITY OF GK PERSEI

S. Boeva, G. Latev, G. Nikolov, R. Zamanov, B. Spassov and M. Belcheva

Institute of Astronomy and National Astronomical Observatory Rozhen,Bulgarian Academy of Sciences, 72 Tsarighradsko Shousse Blvd., 1784 Sofia, Bulgaria


We present observations of dwarf nova GK Per in normal state as well in outbursts.We discuss color changes, flickering amplitude and some other properties of the fastvariations in the light curves in different states.

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Poster

ANALYSIS OF ELECTROMAGNETIC WAVESIN IONOSPHERIC PLASMA MODELS

V. M. Cadez1 and A. Nina2

1Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia2Institute of Physics, University of Belgrade,

Pregrevica 118, 11080 Belgrade, SerbiaE-mail : [email protected], [email protected]

Specially emitted radio waves of given fixed frequency are commonly used as an ef-fective tool to study physical properties and structure of the ionospheric plasma. Thisis done by using the data of a recorded radio-wave in order to perform a procedureequivalent to solving an inverse problem of recovering plasma conditions at the loca-tion where the considered dispersive radio wave is being scattered and reflected fromthe ionosphere. In this mostly theoretical work we compute the corresponding localindex of refraction and study its sensitivity to variations of relevant physical quanti-ties about their standard, typical, values at selected altitudes within the ionosphere.In particular, we are focused on identification of electron concentration variations,geomagnetic field fluctuations, and contribution of collisional processes in observedsignatures of the recorded radio signal.

74



Poster

CONSTRAINING THE COLLECTIVE RADIO EMISSION OFLARGE SCALE ACCRETION SHOCKS

A. Ciprijanovic1, T. Prodanovic2 and M. Z. Pavlovic1

1Department of Astronomy, Faculty of Mathematics, University of Belgrade,Studentski trg 16, 1100 Belgrade, Serbia

2Department of Physics, University of Novi Sad,Trg Dositeja Obradovica 4, 21000 Novi Sad, Serbia

E-mail : [email protected], [email protected], [email protected]

Formation of large-scale structures is thought to give rise to accretion shocks,which could accelerate cosmic rays. These structure-formation cosmic rays are stillhypothetical, and their existence and flux could be constrained by observations invarious wavelengths, since cosmic rays interact with interstellar medium and magneticfields producing particles and radiation that can be detected. Typical objects whereaccretion shocks should be present are galaxy clusters. Here we use radio observationsof Coma cluster and its radio spectrum and assume that Coma is a typical galaxycluster. This is used to constrain the possible contribution of all unresolved galaxyclusters to the di?use radio background. This analysis can also give us the upperlimit of the part of the Coma radio spectrum that could potentially be produced bystructure-formation cosmic rays.

75



Poster

OBSERVATIONS OF GAIA-FUN-TO FROM 2014 USINGSERBIAN AND BULGARIAN TELESCOPES

G. Damljanovic1, S. Boeva2, O. Vince1, G. Latev2, R. Bachev2,M. D. Jovanovic1, Z. Cvetkovic1 and R. Pavlovic1

1Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia2Institute of Astronomy with NAO, BAS, Tsarigradsko Shosse 72, 1784 Sofia, Bulgaria


The Gaia mission is the cornerstone of the European Space Agency – ESA; thesatellite was launched at the end of 2013. In August 2014 the Gaia started with theastronomical observations. Some time after that, since October 2014, the Gaia Pho-tometric Science Alerts started to publish alerts. In September 2016, the first releaseof the Gaia catalogue (Gaia DR1) was appeared. The next one (DR2) would be inApril 2018. The Gaia is mapping the entire Galaxy (near one billion stars), and about600 000 extragalactic objects (mostly quasars – QSOs). Nearly 1000 alerts have beenissued by the Gaia Science Alerts group until the end of 2016. They are: cataclysmicvariables, supernovae, candidate microlensing events, etc. Gaia is now the secondlargest provider of transients in the world. During the test phase (in 2013 and 2014),we observed few objects using just Serbian D = 60 cm telescope at Astronomical Sta-tion Vidojevica – ASV (of Astronomical Observatory in Belgrade – AOB). At thattime Dr. G. Damljanovic established the cooperation so-called the Serbian–Bulgarianmini–network telescopes. Because of it, at the end of 2014 we continued the obser-vations of Gaia Alerts objects (Gaia–Follow–Up Network for Transients Objects orGaia–FUN–TO) using 5 instruments. Four telescopes are at two sites in Bulgaria:the 60 cm at Belogradchik AO, and three ones (2 m, 60 cm and 50/70cm Schmidt–camera) at Rozhen Observatory. As result, we observed about 30 objects until theend of 2016 (14 objects during 2016); there are about 1150 CCD images in JohnsonBV and Cousins RI filters. Also, since mid-2016 we used new 1.4 m ASV telescope(within the frame of the BELISSIMA project, see http://belissima.aob.rs). And fromtime to time (from the end of 2016), the 1.31 m ARIES telescope (Aryabhatta Re-search Institute of observational sciencES, Manora Peak, Nainital, India). We tookpart into observations of rare objects as the eclipsing AM CVn Gaia14aae one; we didit in October 2014 with two telescopes (the 60 cm at ASV and 60 cm at Belograd-chik), and the paper about that object was published (H.C. Campbell et al. 2015,MNRAS 452, 1960). Also, the Gaia16aye (or Ayers Rock, binary microlensing event,the first discovered towards the Galactic Plane); we observed that object 18 timesduring 2016, and at 25th October 2016 with three instruments: 2m Rozhen, 50/70 cmSchmidt–camera (Rozhen) and 1.4 m ASV. Here, we present some our observationsand results of Gaia-FUN-TO.

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Poster

ON THE ASTRONOMICAL SYMBOLS ON ROMAN REPUBLICANAND IMPERIAL COINS

M. S. Dimitrijevic


Various astronomical symbols like stars, crescent Moon, comets, personifications ofconstellations, meteorites... may be found on ancient roman coins and its appearancehas been considered and described many times. Here we present, describe and discusseight examples with astronomical symbols, like stars, the Sun, the crescent Moon andcomets, on coins of Roman republic and Empire. We will consider a silver denarius ofJulis Caesar with two stars, two denarii struck by Octavian Augustus, dedicated toJulius Caesar with the representation of a comet, two silver denarii of Hadrian, onewith crescent and one star and other with crescent and seven stars, an antoninianusof Caracalla with radiated crown, a symbol of Sun, an antoninianus of Julia Domnawith crescent Moon, and a double majorina of Julian Apostate with a bull and twostars.

Fig. 1: Silver denarius struck late 125 - early 128 in Rome by Hadrian. Obverse:Laureate head of Hadrian right, drapery on left shoulder. Inscription: HADRIANVSAVGVSTVS. Reverse: Seven stars within and above crescent Moon. Inscription:COS III (Consul the thitd time).

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Poster

THE STARK-B DATABASE, A NODE OFVIRTUAL ATOMIC AND MOLECULAR DATA CENTER (VAMDC)

M. S. Dimitrijevic1,2, S. Sahal-Brechot2 and N. Moreau2

1Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia2LERMA, Observatoire de Paris, 5 Place Jules Janssen, 92190 Meudon, France

E-mail : [email protected], [email protected],[email protected]

Accurate modelling of stellar atmospheres, opacity calculations and astrophysicalspectra analysis and synthesis require the knowledge of numerous collisional line pro-files, so that it is very important to provide the access to such data via an on linedatabase. The aim of STARK-B database is to contribute to these needs providingwidths and shifts of isolated lines of neutral and ionized atoms due to electron andion impacts. Besides the modelling and spectroscopic diagnostics of stellar atmo-spheres and envelopes, such data are also needed for laboratory plasmas diagnostics,fusion and laser produced plasmas as well as for design of lasers and technologicalplasmas. The precursor of STARK-B was BELDATA - database developed on Bel-grade Astronomical observatory. Now, STARK-B is a collaborative project betweenthe Astronomical Observatory of Belgrade (AOB) and the laboratory LERMA atObservatory of Paris, which started at the end of 2008 (http://stark-b.obspm.fr/).STARK-B is also a node of VAMDC (Virtual Atomic and Molecular Data Centre)and is organised with the standards of the Virtual Observatories. This database con-tains our calculated data published in more than 150 papers in international refereedjournals. In this contribution we will present the STARK-B database and discuss ourongoing work and our plans for the future.

78



Poster

RADIO ODJEK DELTA AURIGIDS U PERIODU 2006-2016 GODINE

Z. Disterlo

Radio-astronomski klub- DMI -Bor, SrbijaE-mail : [email protected]

Delta Aurigids su prvi put otkriveni 50-tih godina XIX veka, da bi prva ozbiljnijaposmatranja i zapaanja krenula 1979. godine. Vec 1981. godine grupa ruskih iamerickih istrazivaca zakljucuju da je srednja orbita meteorskog potoka retrogradnasa periodom od 115 godina. Radijant roja prikazan je na slici 1. (95.7, dec. + 52.5).

Radio posmatranje Delta Aurigids na ARAO ”Tesla” prati se od 2004.godine,maticna kometa je C/1911 N1 ciji period nije tacno utvrdjen (1800–2000.)U perioduod 2006. g. – 2016. g. ukazuje na asimetricnost, tj. broj refleksija posle maksimumaopada znatno brze, nego sto se povecava prema maksimumu. Sam maksimum jeveoma brz, i kratkotrajan prema broju i duzini odjeka. Pretpostavljam da je toposledica krupnijih meteora, koji duze gore na vecim visinama. Takodje je znatnoveca i elevacija antene radioteleskopske – sonde (> 30). Posmatranje je vrsenona frekvenciji (148MHz), sto nam ukazuje, da Delta Aurigidi pripadaju grupi brzihmeteora, kao i velikog elevacionog ugla, i duzine radio–odjeka. U 2006. ZHR = 133meteora.

79



Poster

R AND V BAND MONITORING OF QUASARS THATARE IMPORTANT FOR THE LINK BETWEEN ICRF ANDTHE FUTURE GAIA CELESTIAL REFERENCE FRAME

M. D. Jovanovic, G. Damljanovic and O. Vince

Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected],[email protected], [email protected]

The Gaia astrometric mission of the European Space Agency was launched at theend of 2013. It will provide a catalog of about 600 000 quasars and billion stars.Some of these quasars could be the basis of a new optical reference frame. Thecurrent International Celestial Reference Frame (ICRF) is based on the observationsof quasars at radio wavelengths. It is necessary to observe a set of common quasarsat both optical and radio wavelengths to link the ICRF with the future Gaia CelestialReference Frame - Gaia CRF. Only 10% of the ICRF sources (near 70 sources) aresuitable to establish this link, and because of it this number has increased by 47 sources(out of the ICRF list) with high astrometric quality, as required for the alingment. Ourobservations of 47 candidate sources have been carried out since July 2016 using threetelescopes: two of them with D=0.6m and D=1.4m are located at the AstronomicalStation Vidojevica (of the Astronomical Observatory of Belgrade) and the third onewith D=2m is located at the Rozhen Observatory of NAO BAS (Bulgaria). In thispaper we present main steps of our reduction and some results (as light curves in Rand V bands) of a few objects.

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Poster

RIGIDITY SPECTRUM OF GALACTIC COSMIC RAYS VARIATIONSDURING THE FORBUSH EFFECTS

A. I. Klyuyeva1, A. V. Belov2 and E. A. Eroshenko2

1The Main Astronomical Observatory of NAS of Ukraine,27 Akademika Zabolotnoho St. 03143, Kyiv, Ukraine

2Pushkov Institute of Terrestrial Magnetism, Ionosphere, and Radio wave Propagation,Russian Academy of Sciences, Troitsk, Moscow, 142190 Russia


In this research we have studied variations in the rigidity spectrum of primarycosmic rays during Forbush effects (FE) recorded in cycles 20–24 of solar activity onthe basis of data from the global network of neutron monitor stations processed byglobal survey method.

We investigated variations in the rigidity spectrum index of Forbush effects as afunction of the solar activity level, geomagnetic activity level, phases of the effect,polarity the total magnetic field of the Sun, type and parameters of the source ofcosmic ray modulation, etc..

We considered the magnetospheric effects problem of galactic cosmic rays (GSR)variations and estimated their influence on the accuracy of the rigidity spectrumdetermination of GCR variations. Comprehensive analysis of our results revealed newregularities in the dynamics of the energy spectrum of galactic cosmic rays variationsduring the FE that reflect the dynamic processes occurring in the interplanetaryspace.

81



Poster

KORELACIJA ASTRONOMIJE I GEOGRAFIJE

B. Krstin

OS ”Vasa Zivkovic”, Pancevo, SerbiaE-mail : [email protected]

Osnovna skola ”Vasa Zivkovic” u Pancevu, nije samo najstarija skola u graduvec je i jedina koja desetu godinu okuplja ljubitelje astronomije u okviru sekcije”Astronomska druzina”. Geografija kao multidisciplinarna nauka u petom razredu,uglavnom proucava astronomske sadrzaje. Jedan cas nedeljno nije dovoljan da seucenicima priblizi ovako apstraktna tema. Zbog toga sam se odlucila da uvedemodvocas astronomske sekcije, jednom nedeljno. Kako bih unapredila nastavu zatrazilasam pomoc eminentnih ljudi, astronoma i zaljubljenika u nebo AD ”Rudjer Boskovic”iz Beograda. I tako vec deceniju traje nasa zvezdana korelacija. Dr Natasa Stanic,nasa dugogodisnja zvezdana prijateljica svake godine nasim petacima odrzava inter-aktivni cas – naucnu igraonicu i radionicu ”Baloni, casa vode i mobilni telefon”. Svakegodine, takodje, posecujemo planetarijum na Kalemegdanu i Astronomsku opserva-toriju na Zvezdari gde nam dr Ninkovic pokazuje najveci teleskop i prica o razvojuastronomije kod nas. Sva ova dragocena znanja iz astronomije, koristimo u nastavigeografije za unapredjivanje kvaliteta nastave, i ugradjujemo ih u geografske zakoni-tosti koje vaze na Zemlji. Geografija astronomima pruza informacije o prirodnimi drustvenim procesima i zakonima kojima je izlozena planeta, ukazuje na uzrocnoposlednicne veze prirode i coveka a sve u cilju ocuvanja zivota na Zemlji i odrzivograzvoja.

Zbog izuzetno pozitivnog stava ucenika prema astronomskim sadrzajima i ak-tivnostima astronomske sekcije, velike motivisanosti za ucenje i boljih postignuca,svim kolegama - nastavnicima i profesorima u osnovnim i srednjim skolama, pre-porucujem uvodjenje astronomske sekcije i istrazivanje beskrajno zanimljive vasione.

82



Poster

PROTOCOL FOR ACTIVE SETI IN SOL NEIGHBORHOOD

D. V. Lukic

Institute of Physics, University of Belgrade, P.O. Box 57 11001 Belgrade, SerbiaE-mail : [email protected]

In the search for habitable planets, the ultimate aspiration is finding an extrater-restrial technical civilization. We already lost a half of century for an active searchfor extraterrestrial civilizations. If all civilizations in the Universe are only recipientsand not message-sending civilizations, then no Search for Extraterrestrial Intelligencemake any sense. Detecting only leaked radio signals is a hard job with present re-sources. We will propose scientifically based Messaging to Extraterrestrial Intelligenceprogram.

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Poster

SEARCH FOR POSSIBLE EXOMOONS WITH FAST TELESCOPE

D. V. Lukic

Institute of Physics, University of Belgrade, P.O. Box 57, 11001 Belgrade, SerbiaE-mail : [email protected]

Our knowledge of the Solar System, encourage us to beleive that we might expectexomoons to be present around some of the known exoplanets. With present hardwarewe shall not be able to find exomoons with existing optical astronomy methods atleast 10 years from now and even then, it will be hard task to detect them. Wesuggest radio astronomy based methods to search for possible exomoons around theseexoplanets. Using data from the Exoplanet Orbit Database (EOD) we find 2 starswith Jovian exoplanets within 50 light years fully accessible by the new radio telescope,The Five-hundred-meter Aperture Spherical radio Telescope (FAST).

84



Poster

CAN WE AFFORD AN INTERSTELLAR FLIGHT?

D. V. Lukic

Institute of Physics, University of Belgrade, P.O. Box 57, 11001 Belgrade, SerbiaE-mail : [email protected]

What is a price of interstellar flight? How are we prepared for such grandiose task?Let me sum up main costs for the projects from three papers [1,2,3]. We calculatedonly the most basic things, a price of building the sail and energy to power the system.

We can see that only adjusted system proposed in [4] has a chance to be financed.This is not a too big amount of money to be spent by the government with a senseof economic responsibility.

References

[1]Robert, L., Forward, J.: 1984, Spacecraft, 21, 187.[2]Philip, L.: 2016, JBIS, 69, 40.[3]Rene, H., Michael, H.: 2017, ApJL, 835, L32 and Rene, H., Michael, H., Pierre,

K.: 2017, arXiv:1704.03871.[4]David, K.: 2017, arXiv: 1704.04310. pdf.

85



Poster

DWARF GALAXY DEMOGRAPHY IN CLUSTERS OF GALAXIESFROM COSMOLOGICAL SIMULATIONS

N. Martinovic1, M. Micic1, A. Mitrasinovic1, S. Milosevic2 and M. Smole1

1Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia2Department of Astronomy, Faculty of Mathematics, Studentski trg 16,



We have defined clusters of galaxies and their member population from halo cat-alogues of Illustris-1 cosmological simulation, and we have determined which partof that member object population are dwarf galaxies. By analyzing dwarf galaxydemographics from retrieved clusters of galaxies we inspect what is the influence ofenvironment on census of different morphological types of dwarf galaxies. We alsomake an insight into influence of inter-cluster dynamics for dwarf galaxy evolution.

86



Poster

WHAT CAN ECCENTRICITIES OF MEMBERS OF CLUSTERSOF GALAXIES TELL US ABOUT CLUSTER EVOLUTION?

N. Martinovic1, M. Micic1, A. Mitrasinovic1, M. Smole1 and S. Milosevic2

1Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia2Department of Astronomy, Faculty of Mathematics, Studentski trg 16,



We have identified clusters of galaxies from Illustris-1 simulation and have ex-tracted objects that are designated as their members. Using parameters given in halocatalogues we have calculated orbital parameters for each member of selected clusters.Closer analysis of ellipticity of the member objects confirms that clusters of galaxiesare dynamically young structures which are only at beginning of the virialization pro-cess. We present what an ellipticity of cluster members can tell us about its recentglobal evolution.

87



Poster

NECESSITY OF RE-DEFINITION OF PLANET,AS PROPOSED BY ALAN STERN ET AL

A. B. Nedeljkovic

Filolosko-umetnicki fakultet - FILUM, Univerzitet Kragujevac, SerbiaE-mail : srpsko [email protected]

Recently, Alan Stern (of Pluto, New Horizons work) and other very competentpeople sent a letter to the International Astronomical Union - IAU, proposing a newdefinition of planet, <http://www.hou.usra.edu/meetings/lpsc2017/pdf/1448.pdf>,and there have been other calls for Prague 2006 definition of planet to be re-examinedand altered. Obviously a good definition should not mention Sun by name, becausethat excludes trillions of other planets from the definition; probably should not de-mand that a body must clear its orbital path of other bodies, because it excludes verydistant planets, such as those in the Kuiper belt; and, should not forget the rogueplanets, those without a star; but the proposal by Stern et al. is too liberal, it includesmoons also, which is wrong. This whole issue is obviously not just for experts, it isalso a matter of broad cultural and civilizational perceptions and traditions, involv-ing the traditional status of Pluto, too. (We could introduce a category ”traditionalnine planets”.) Public debates ought to be organized about this question. This canstrongly contribute to the popularization and perhaps also financing of astronomy asa science, in Serbia, because this topic generates a lot of interest in the public, andin the media.

88



Poster

LOW IONOSPHERIC RESPONSE TO ASTRO-GEO-PHENOMENA- RECENT RESEARCH

A. Nina1, V. M. Cadez2, L. C. Popovic2, V. A. Sreckovic1, J. Bajcetic3,S. T. Mitrovic3, M. Radovanovic4, M. Todorovic Drakul5,

A. Kolarski6 and S. Simic7

1Institute of Physics, University of Belgrade, Belgrade, Serbia2Astronomical Observatory, Belgrade, Serbia

3University of Defence, Military Academy, Belgrade, Serbia4Geographical Institute ”Jovan Cvijic” Serbian Academy of Sciences and Art,

Belgrade, Serbia5Department of Geodesy and Geoinformatics, Faculty of Civil Engineering,

University of Belgrade, Belgrade, Serbia6NTC NIS Naftagas DOO, Novi Sad, Serbia

7Faculty of Science, University of Kragujevac, Kragujevac, SerbiaE-mail : [email protected], [email protected], [email protected], [email protected],[email protected], [email protected], [email protected],


This paper overviews our recent studies of low ionospheric perturbations causedby numerous astrophysical and geophysical phenomena. We present theoretical andnumerical procedures developed for modeling THE spatial and time distributions ofplasma parameters and for detecting the ionospheric disturbances. Here, we examinethe effects of solar X-ray flares, gamma ray bursts, tropical depressions preceding ahurricane and earthquakes. The analyses are based on data collected by the radiosignal receiver located at the Institute of Physics in Belgrade.

89



Poster

ON A NEW FORMULA FOR THE VELOCITY-DISPERSION RATIO

S. Ninkovic


The ratio of two velocity dispersions - transversal-to-radial (random velocity) - isrevisited. A new formula is obtained. It contains the classical one (known as epicyclic)as a special case. Like the classical formula the new one is also applicable for the thindisc (low orbital eccentricities). However, in the new formula the influence of theratio of the Oort constants moduli and that of the distribution of orbital phases areclearly separated.

90



Poster

ON A SIMPLE FORMULA FOR CALENDARS

S. Ninkovic


A simple formula comprising and unifying the three calendars orginating from theRoman calendar is proposed. The significance of the formula is rather pedagogicalthan scientific because the objective is to explain in a way as simple as possible thecontributions of the Gregorian and Neojulian reforms.

91



Poster

ASTEROID FAMILIES PORTAL:AN ONLINE PLATFORM TO STUDY ASTEROID FAMILIES

B. Novakovic, V. Radovic and V. -Dosovic



One of the ways scientists are using to cope with the large size and complexityof data acquired in the recent years is development of web-portals. Such portals aretypically devoted to specific purposes, and allow scientists to easily review and analyzelarge amount of available data.

In this work we present an open access web portal devoted to asteroid families,namely the Asteroid Families Portal (AFP). The aim of the AFP is to collect differentdata about asteroid families. It can be used to quickly assess and visualized data.Still, this should not be the only purpose of this portal, but it should also allow toapply different tools and methods to the provided data. For instance, the well-knownHierarchical Clustering Method (HCM) could be employed on-line to obtained themost recent list of a family members.

The AFP is foreseen to be continuously updated and upgraded. The currentdatasets will be updated frequently by adding newly available data. Among the nexttools, we foresee for instance to offer a fully automatic estimation of family age,based on the so-called V-shape method. We also aim to develop an algorithm thatwill provide different basic information about an asteroid family, such is the size ofthe parent body and its corresponding escape velocity, the slope of the magnitude-frequency distribution, etc.

92



Poster

THE FIRST TEST OF NEW ANDOR IXON 897 EMCCD CAMERA

R. Pavlovic, Z. Cvetkovic, G. Damljanovic, O. Vince and M. D. Jovanovic

Astronomical Observatory, Volgina 7, P.O. Box 74, 11060 Belgrade, SerbiaE-mail : [email protected]

Here the results of the testing of a new, very quick, EMCCD Andor iXon 897,camera are reported. The camera was examined in early June and September 2017.The CCD frames of low-separation visual double stars were obtained with short ex-posures of a few milliseconds, the camera was mounted on the 60 cm telescope atASV. This quick camera will be part of the equipment for the speckle-interferometrictechnique of observing double stars and in the beginning it will be utilised for frameobtaining by applying lucky imaging.

93



Poster

MILUTIN’S SUNDIAL IN KRALJEVO

Z. Prnjat

Faculty of Geography University of Belgrade, SerbiaE-mail : [email protected]

A horizontal sundial at the Serbian Warriors’ Square in Kraljevo (4343′25′′ N,2041′14′′ E), with a diameter D = 58 m, is one of the largest in Europe. The tiledsquare has a half-degree inclination so that the base of the sundial presents a truncatedcone (D = 58 m, D1 = 17.5 m, α = 179). A monument to the Serbian Warrior (h= 14.43 m), popularly called by a traditional Serbian name ”Milutin”, has the roleof the gnomon. The author of the monument that is the symbol of Kraljevo was aRussian architect and sculptor Roman Nikolayevich Verhovskoy (Roman NikolaeviqVerhovskoi, 1881-1968).

The monument was erected in 1932, whereas the sundial’s network was carved inthe stone surface in 2001 (sundial calculation by M. Tadic, geodetic processing by S.Blagojevic, architectural design by M. Petrovic). The hour network consists of hourand date lines.

The hour lines have been cut for every hour in the range from 7 a.m. to 4 p.m.Central European Summer Time (UT + 2 h). Daytime hours are read according tothe position of the shadow’s end within the hour squares rather than the shadow’sdirection, which is confusing for many observers. The end of the spear’s shadow ofthe Serbian Warrior disperses, which complicates the reading of the daytime hoursadditionally, especially when the reading is done from the vicinity.

There are four date lines: the summer solstice hyperbola, the equinox line, andthe hyperbolas for October 7 and 14. The passage of the shadow’s end along thefirst hyperbola marks the first day of summer, along the equinox line - the first dayof spring and autumn, along the hyperbola for October 7 - the day of the city ofKraljevo, and along the hyperbola for October 14 - the day when 1,736 civilians ofKraljevo were shot in retaliation in 1941 by the German occupying forces.

Today, the hour network and the dial of the ”Milutin’s” sundial are considerablydamaged, and it is necessary to replace the inserted stone elements in its construction.

94



Poster

THE SPECTRAL COEFFICIENTS OF ABSORPTION PROCESSESIN DENSE STRONGLY IONIZED ASTROPHYSICAL PLASMAS

N. M. Sakan1, V. A. Sreckovic1, Z. Simic2 and M. S. Dimitrijevic2,3

1Institute of Physics, Pregrevica 118, 11080 Zemun, Belgrade, Serbia2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia


E-mail : [email protected], [email protected], [email protected],[email protected]

In this contribution we present a new model method of describing atomic photo-absorption processes in dense strongly ionized astrophysical plasmas, which is basedon the approximation of cut-off Coulomb potential. By now this approximation hasbeen used in order to describe transport properties of dense plasmas (see e.g. Mihajlovet al. 2011, 2015), but it was clear that it could be applied to the some absorptionprocesses in non-ideal plasmas too. This topic itself, and search of more consistentmodels of screening and more realistic potentials in plasmas is still continuing andis very actual. The presented results cover a wide region of the plasma electrondensities and temperatures. Such plasmas are of interest from both the laboratoryand the astrophysical aspect. Here, we keep in mind the plasma of the inner layers ofthe solar atmosphere, as well as of partially ionized layers of other stellar atmospheres,for example the atmospheres of DA and DB white dwarfs with effective temperaturesbetween 10 000 K and 25 000 K (Sreckovic et al. 2014).

References

Mihajlov, A. A., Sakan, N. M., Sreckovic, V. A., Vitel, Y.: 2011, J.Phys. A, 9,095502.

Mihajlov, A. A., Sreckovic, V. A., Sakan, N. M.: 2015, J. Astrophys. Astr., 36,635-642.

Sreckovic, V. A., Mihajlov, A. A., Ignjatovic, L. M. and Dimitrijevic, M. S.: 2014,JPCS, 565, 012022.

95



Poster

THE OPTICAL CHARACTERISTICS OF DENSE, STRONGLYIONIZED HYDROGENE PLASMA, APPLICABLE

IN ASTROPHYSICAL OBJECTS

N. M. Sakan1, V. A. Sreckovic1, Z. Simic2 and M. S. Dimitrijevic2,3

1Institute of Physics, Pregrevica 118, 11080 Zemun, Belgrade, Serbia2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia


E-mail : [email protected], [email protected], [email protected], [email protected]

The dense plasma absorption is a common measured characteristics of a experi-mental plasma measurement as well as basic quantity to describe a opacity of astro-physical objects. Here we keep in mind the plasma of the inner layers of the solaratmosphere, as well as of partially ionized layers of other stellar atmospheres, forexample the atmospheres of DA and DB white dwarfs with effective temperaturesbetween 10 000 K and 25 000 K (Sreckovic et al. 2014). In order to describe a denseplasma optical characteristics a model cut-off Coulomb potential is used. Up untillnow this approximation has been used in order to describe transport properties ofdense plasmas (see e.g. Mihajlov et al. 2011, 2015), but it was clear that it could beapplied to the same absorption processes in non-ideal plasmas too. This topic itself,and search of more consistent models of screening and more realistic potentials inplasmas is still continuing and is very actual.

References

Mihajlov, A. A., Sakan, N. M., Sreckovic, V. A., Vitel, Y.: 2011, J. Phys. A, 9,095502.

Mihajlov, A. A., Sreckovic, V. A., Sakan, N. M.: 2015, J. Astrophys. Astr., 36,635-642.

Sreckovic, V. A., Mihajlov, A. A., Ignjatovic, L. M. and Dimitrijevic, M. S.: 2014,JPCS, 565, 012022.

96



Poster

DYNAMICAL MODELS OF THREE LENTICULAR GALAXIES:NGC 1023, NGC 3115 and NGC 4526

S. Samurovic


Lenticular galaxies (S0s) together with elliptical galaxies belong to the class ofearly-type galaxies (ETGs). The main features of S0s are a visible disk componentand a prominent bulge component. In this contribution we study the kinematics anddynamics of three S0 galaxies which possess globular clusters (GCs) which extendbeyond approximately five effective radii. We analyze NGC 1023, NGC 3115 andNGC 4526 based on their GCs. We use the kinematics of these galaxies which weextracted in order to construct the dynamical models of these objects. We use theJeans equation based on both Newtonian and MOND methodologies. In the Newto-nian case we use mass-follows-light assumption and we also test the models with darkmatter (DM) in the Navarro-Frenk-White form. We find that while NGC 1023 doesnot need a significant amount of DM, for the remaining two galaxies, NGC 3115 andNGC 4526 the dark component fully dominates stellar matter. Three MOND modelsthat we tested show that while NGC 1023 can be modeled without DM in MOND,for NGC 4526 there is hint of an additional dark component and NGC 3115 needs asignificant amount of DM in its outer parts. Finally, we compare our findings withthe predictions of the Λ cold dark matter cosmology.

97



Poster

TELESCOPE “MILANKOVIC”: MOUNTING, PRESENTAND FUTURE WORK

S. Samurovic, G. Djurasevic, Z. Cvetkovic, R. Pavlovic and O. Vince

Astronomical Observatory, Volgina 7, 11060 Belgrade 38, SerbiaE-mail : [email protected], [email protected], [email protected],


In this contribution we present the final stages of the procurement of the telescope“Milankovic” purchased by the Astronomical Observatory of Belgrade (AOB) usingthe funds of the FP7 REGPOT project BELISSIMA with the support of the Ministryof Education, Science and Technological Development of the Republic of Serbia. Thefinal activities of the BELISSIMA project and the successful mounting of the 1.40m telescope “Milankovic” at the Vidojevica Astronomical Station (VAS) in 2016 arepresented. We outline the present activities related to the VAS and we also describeobservational projects currently active. Finally, we present the plans for the futurerelated to the purchase of new instruments, continuation of present and initiation ofnew observational projects and future collaborations.

98



Poster

THE NEW MODEL METHOD OF THE ELECTROSTATICSCREENING OF THE ASTROPHYSICAL PLASMAS:

MULTI-COMPONENT SYSTEMS

V. A. Sreckovic1, Lj. M. Ignjatovic1, A. Nina1 and M. S. Dimitrijevic2,3

1Institute of Physics, Belgrade University,Pregrevica 118, Zemun, 11080 Belgrade, Serbia

2Astronomical Observatory, Volgina 7, 11060 Belgrade 38, Serbia3LERMA, Observatoire de Paris, UMR CNRS 8112, UPMC,

92195 Meudon Cedex, FranceE-mail : [email protected], [email protected], [email protected]

This work is the natural extension of the research of plasmas inner electrostaticscreening whose results are presented in the papers Mihajlov et al. (2008, 2009).As the object of investigation, astrophysical fully ionized electron-ion plasma is cho-sen with positively charged ions of two different kinds (three-component systems),including the plasmas of higher non-ideality. The aim is to develop, a new modelself-consistent method of the electrostatic screening in a wide region of the electrondensities and temperatures. Within this method the electron-ion and ion-ion cor-relations are included in the used model, and all types of the necessary conditionsare defined. We wish to draw attention that developed method is suitable for astro-physical applications. Here we keep in mind that in outer shells of stars the physicalconditions change from those which correspond to the rare, practically ideal plasma,to those which correspond to extremely dense non-ideal one. However, the methodpresented gives a possibility to describe the electrostatic screening of all such outershells in the same way, by means of the obtained screening characteristics.

References

Mihajlov, A. A., Vitel, Y. and Ignjatovic, Lj. M.: 2009, High Temperature, 47, 147-157.

Mihajlov, A. A., Vitel, Y., and Ignjatovic, Lj. M.: 2008, High Temperature, 46, 737-745.

99



Poster

STRONG SOLAR X RAY FLARES:INFLUENCE ON THE IONOSPHERE

V. A. Sreckovic1 and D. M. Sulic2

1Institute of Physics, Belgrade University,Pregrevica 118, Zemun, 11080 Belgrade, Serbia

2University Union - Nikola Tesla, 11000 Belgrade, SerbiaE-mail : [email protected], [email protected]

The sensitivity of Very Low Frequency (VLF, 3-30 kHz) and Low Frequency (LF,30-300 kHz) radio signals in the lower ionosphere makes it an ideal probe for re-motely sensing the ambient state and localized perturbations of the lower ionosphere.During eruptive Solar activity, released X-ray flares, penetrate deeply into the lowerionosphere leaving their signatures in notable disturbances of monitored phase andamplitude of VLF/LF-signal. These ground-based observations of sudden phase andamplitude increase/decrease, as monitored by the Belgrade AWESOME and AbsPALfacility, for signals from worldwide transmitters, have been related to the space-basedGOES satellite measurements of the X-ray irradiance in the 0.1-0.8 nm band (Nina etal. 2011). Simultaneous measurement of amplitude and phase of the VLF/LF signalsduring a solar flare occurrence was applied to evaluate the electron density profileversus altitude, to carry out the function of time over the middle Europe (Sulic et al.2014, 2016).

References

Nina, A., Cadez, V. M., Sreckovic, V. A., Sulic, D.: 2011, Baltic Astronomy, 20, 609.Sulic, D., Sreckovic, V. A.: 2014, Serb. Astron. J., 188, 45-54.Sulic, D., Sreckovic, V. A. and Mihajlov, A. A.: 2016, Adv. Space. Res., 57, 1029-

1043.

100



Poster

THE DUST COVERING FACTOR IN ACTIVE GALACTIC NUCLEI

M. Stalevski


The primary source of emission of active galactic nuclei (AGN), the accretion disk,is surrounded by an optically and geometrically thick dusty structure (“the so-calleddusty torus”). The infrared radiation emitted by the dust is nothing but a reprocessedfraction of the accretion disk emission, so the ratio of the torus to the AGN luminosity(Ltorus/LAGN) should correspond to the fraction of the sky obscured by dust, i.e. thecovering factor. We undertook a critical investigation of the Ltorus/LAGN as the dustcovering factor proxy. Using state-of-the-art 3D Monte Carlo radiative transfer code,we calculated a grid of spectral energy distributions (SEDs) emitted by the clumpytwo-phase dusty structure. With this grid of SEDs, we studied the relation betweenLtorus/LAGN and the dust covering factor for different parameters of the torus. Wefound that in the case of type 1 AGNs the torus anisotropy makes Ltorus/LAGN

underestimate low covering factors and overestimate high covering factors. In type2 AGNs Ltorus/LAGN always underestimates covering factors. Our results providea novel easy-to-use method to account for anisotropy and obtain correct coveringfactors. Using two samples from the literature, we demonstrated the importance ofour result for inferring the obscured AGN fraction. We found that after the anisotropyis properly accounted for, the dust covering factors show very weak dependence onLAGN, with values in the range of ≈ 0.6−0.7. Our results also suggest a higher fractionof obscured AGNs at high luminosities than those found by X-ray surveys, in partowing to the presence of a Compton-thick AGN population predicted by populationsynthesis models.

101



Poster

THE FINE STRUCTURE OF CHAOS IN THE SOLAR SYSTEM

N. Todorovic


The behaviour of small bodies in our Solar System is determined by different dy-namical regimes, weak and strong chaos, long-term and short term stabilities. Usingdelicate numerical methods, we study chaotic regions in some of the most importantmain belt resonances. We were able to localize specific chaotic structures whose exis-tence is predicted by theoretical studies. Our results suggest that those structures area fertile source of fast diffusion and that the Solar System is much more dynamicallyactive than hitherto observed.

102



Poster

FIRST SPECTRA FROM THE TELESCOPE MILANKOVIC

O. Vince, M. D. Jovanovic and I. Vince


Telescope Milankovic is a 1.4m reflective telescope installed at Astronomical Sta-tion Vidojevica in 2016. It has an AltAz mount, RC optical system and 4 Nasmythports out of which 2 are provided with field derotators. While one port is regularlyused for photometrical and astrometrical measurements since installation, the otherwas used to setup and calibrate a portable spectrograph SpectraPro 2750. In thistalk, we present first spectra obtained by this instrument.

103



Poster

NEAR-INFRARED PHOTOMETRY OF THE NEARBYSPIRAL GALAXY NGC 2841

A. Vudragovic, O. Vince, S. Samurovic and M. Jovanovic


We present near-infrared photometry (Johnson-Cousins I passband) of the nearbyspiral galaxy NGC 2841 obtained with the Apogee U42 CCD camera mounted on the1.4m Milankovic telescope.

The methodology of observation given the sensitivity of the near-infrared I bandto the sky background variations and fringing is presented in more details. Thebackground model is created from a set of dithered exposures of a non-crowded field,avoiding the galaxy itself as an extended object by pointing the telescope 1 degreeaway from the galaxy to create the correct fringing pattern. The galaxy frames arecorrected for this effect by subtracting the fringing pattern from each of them. Thegalaxy images are also taken with dithering to enable the creation of large mosaic,thus enlarging the field of view. This may be particularly useful in searching for dwarfcandidates around nearby galaxies.

The astrometric calibration was done using publicly available Astrometry code.Also, the photometric calibration was done using The Whole-Sky USNO-B1.0 catalogof stars. Finally, the surface brightness of NGC 2841 galaxy was decomposed into thebulge and the disk. The results are compared to the previous work in the infrared3.6µm band.

104



Poster

RESONANT MICROINSTABILITY AS A TRIGGEROF COLLISIONLESS SHOCK FORMATION

V. Zekovic



We use electromagnetic N-body and Particle-In-Cell codes to simulate formationand propagation of quasi-parallel collisionless shocks. We capture the microphysics ofa shock at early phases of its formation. Different type instabilities develop in frontand behind of a shock. In an upstream region, streaming instabilities are initiatedby the return current of ions. In the downstream, the Weibel instability may developdepending on the magnetization strength. We also observe the growth of a circularlypolarized, resonant with the gyroradius of the flow, instability that appears at theshock transition and is then advected further downstream by the flow. It correspondsto electromagnetic mode induced by two interpenetrating plasmas. When the flow issuperalfvenic, this mode becomes unstable and then stays imprinted in the backgroundmagnetic field. Because of its resonance, such instability strongly scatters particles,thus forming the density jump. In our previous work we show that if such mode isto be the resonant one, equations then indicate that density jump in the downstreamshould be ∼ 4. We assimilate those theoretical results to preliminary simulationresults presented here and we investigate importance of such a resonant instability intriggering of shock formation or even in mediating the shock itself.

105

Programme of the Conference



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116

List of ParticipantsAuthors’ Index



LIST OF PARTICIPANTS

Ahad, Syeda LammimAstromundus student, [email protected]

Aleksic, JovanFaculty of Mathematics, University ofBelgrade, [email protected]

Anderton, Roger J.United [email protected]

Atanackovic, OlgaFaculty of Mathematics, University ofBelgrade, [email protected]

Bachev, RumenInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Belcheva, MayaInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Beslic, IvanaFaculty of Mathematics, University ofBelgrade, [email protected]

Bianchi, StefanoUniversita degli Studi Roma Tre, [email protected]

Bisikalo, Dmitry V.Institute of Astronomy RussianAcademy of Sciences, Moscow, [email protected]

Boeva, SvetlanaInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Bon, EdiAstronomical Observatory, Belgrade,[email protected]

Bon, NatasaAstronomical Observatory, Belgrade,[email protected]

Borka, DuskoAtomic Physics Laboratory (040),Vinca Institute of Nuclear Sciences,Belgrade, [email protected]

Borka Jovanovic, VesnaAtomic Physics Laboratory (040),Vinca Institute of Nuclear Sciences,Belgrade, [email protected]

Boskovic, MatejaPetnica Science Center, [email protected]

Cadez, VladimirAstronomical Observatory, Belgrade,[email protected]

Castanon, AdrianAstromundus student, [email protected]

Chougule, AbhishekAstromundus student, [email protected]

119



Ciprijanovic, AleksandraFaculty of Mathematics, University ofBelgrade, [email protected], ZoricaAstronomical Observatory, Belgrade,[email protected]’Addio, AnnaUniversity of Naples ”Federico II”, [email protected], GoranAstronomical Observatory, Belgrade,[email protected], MomchilInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected], IvanFaculty of Mathematics, University ofBelgrade, [email protected], Milan S.Astronomical Observatory, Belgrade,[email protected], JeanRadio-astronomski klub DMI, Bor, [email protected], VladimirFaculty of Mathematics, University [email protected], GojkoAstronomical Observatory, Belgrade,[email protected], StefaniaUniversity of Naples ”Federico II”, [email protected]

Ilic, DraganaFaculty of Mathematics, University ofBelgrade, [email protected]

Janc, Natalija415 Old Trail Rd Baltimore, MD 21212,[email protected]

Jankov, SlobodanAstronomical Observatory, Belgrade,[email protected]

Jovanovic, BoraAstronomical Observatory, Belgrade,[email protected]

Jovanovic, Miljana D.Astronomical Observatory, Belgrade,[email protected]

Jovanovic, PredragAstronomical Observatory, Belgrade,[email protected]

Jurkovic, MonikaAstronomical Observatory, Belgrade,[email protected]

Kanuchova, ZuzanaAstronomical Institute of SlovakAcademy of [email protected]

Klyuyeva, AntoninaThe Main Astronomical Observatory(MAO) of the National Academy of Sci-ences of [email protected]

Knezevic, SladjanaWeizmann Institute of Science, [email protected]

120



Knezevic, ZoranSerbian Academy of Sciences and [email protected]

Koleva, KostadinkaInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Kovacevic, AndjelkaFaculty of Mathematics, University ofBelgrade, [email protected]

Krstin, BiljanaOS ”Vasa Zivkovic”, Pancevo, [email protected]

Lakicevic, MasaAstronomical Observatory, Belgrade,[email protected]

Latev, GeorgiInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Latkovic, OliveraAstronomical Observatory, Belgrade,[email protected]

Lazarevic, SanjaFaculty of Mathematics, University ofBelgrade, [email protected]

Li, YushanAstromundus student, [email protected]

Lukic, DraganInstitute of Physics, University of Bel-grade, [email protected]

Marceta, DusanFaculty of Mathematics, University ofBelgrade, [email protected]

Marceta-Mandic, SladjanaFaculty of Mathematics, University ofBelgrade, [email protected]

Martinovic, MihailoFaculty of Mathematics, University ofBelgrade, Serbiamihailo [email protected]

Martinovic, NemanjaAstronomical Observatory, Belgrade,[email protected]

Mijajlovic, ZarkoFaculty of Mathematics, University ofBelgrade, [email protected]

Milic, DamnjanFaculty of Mathematics, University ofBelgrade, [email protected]

Milic Zitnik, IvanaAstronomical Observatory, Belgrade,[email protected]

Milosevic, MilanFaculty of Science and Mathematics,University of Nis, [email protected]

Milosevic, StanislavFaculty of Mathematics, University ofBelgrade, [email protected]

Mitrasinovic, AnaAstronomical Observatory, Belgrade,[email protected]

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Nedeljkovic, Aleksandar B.Filolosko-umetnicki fakultet, Univerzi-tet Kragujevac, [email protected]

Nikolov, YankoInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected]

Nina, AleksandraInstitute of Physics, University of Bel-grade, [email protected]

Ninkovic, SlobodanAstronomical Observatory, Belgrade,[email protected]

Novakovic, BojanFaculty of Mathematics, University ofBelgrade, [email protected]

Onic, DusanFaculty of Mathematics, University ofBelgrade, [email protected]

Pakvor, IvanAstronomical Observatory, Belgrade,[email protected]

Pavlovic, MarkoFaculty of Mathematics, University ofBelgrade, [email protected]

Pavlovic, RadeAstronomical Observatory, Belgrade,[email protected]

Pejovic, NadezdaFaculty of Mathematics, University ofBelgrade, [email protected], VanjaFaculty of Mathematics, University ofBelgrade, [email protected], BlagovestInstitute of Astronomy and NationalAstronomical Observatory, Sofia, [email protected], JovanaFaculty of Sciences, University of NoviSad; Faculty of Mathematics, Univer-sity of Belgrade, [email protected], Luka C.Astronomical Observatory, Belgrade,[email protected], ZoricaFaculty of Geography, University of Bel-grade, [email protected], TijanaFaculty of Sciences, University of NoviSad, [email protected] - Benisek, VojislavaAstronomical Observatory, Belgrade,[email protected], ViktorFaculty of Mathematics, University ofBelgrade, [email protected], JohnCenter for Astrophysics, Cambridge,[email protected]

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Sakan, NenadInstitute of Physics, University of Bel-grade, [email protected]

Samurovic, SrdjanAstronomical Observatory, Belgrade,[email protected]

Savic, DjordjeAstronomical Observatory, Belgrade,[email protected]

Sijacki, DeboraInstitute of Astronomy and Kavli Insti-tute for Cosmology, United [email protected]

Smole, MajdaAstronomical Observatory, Belgrade,[email protected]

Sreckovic, VladimirInstitute of Physics, Belgrade, [email protected]

Stalevski, MarkoAstronomical Observatory, Belgrade,[email protected]

Stanic, NatasaAstronomical Society ”RudjerBoskovic”, Belgrade, [email protected]

Stankovic, JelenaTeacher Education Faculty, Universityof Belgrade, [email protected]

Stoiljkovic, DragoslavFaculty of Technology, University ofNovi Sad, [email protected]

Stojanovic, MilanAstronomical Observatory, Belgrade,[email protected]

Tibolla, OmarMesoamerican Centre for Theoret-ical Physics (MCTP), UniversidadAutonoma de Chiapas (UNACH)[email protected]

Todorovic, NatasaAstronomical Observatory, Belgrade,[email protected]

Tomasevic, MarijaFaculty of Physics, University of Bel-grade, [email protected]

Tomic, ZoranAstronomical Society ”Eureka”, [email protected]

Topic, SasaMathematical faculty, University of Bel-grade, Serbiasasa topic [email protected]

Trajkovska, VeselkaAstronomical Observatory, Belgrade,[email protected]

Urosevic, DejanFaculty of Mathematics, University ofBelgrade, [email protected]

Velovic, VeliborFaculty of Mathematics, University ofBelgrade, [email protected]

Vidojevic, SonjaDepartment of Mathematical Sciences,State University of Novi Pazar, [email protected]

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Vince, IstvanAstronomical Observatory, Belgrade,[email protected]

Vince, OliverAstronomical Observatory, Belgrade,[email protected]

Vucetic, MilicaFaculty of Mathematics, University ofBelgrade, [email protected]

Vudragovic, AnaAstronomical Observatory, Belgrade,[email protected]

Vujcic, VeljkoAstronomical Observatory, Belgrade,[email protected]

Vujicic, DejanFaculty of Technical Sciences in Cacak,[email protected]

Vukadinovic, DusanFaculty of Mathematics, University ofBelgrade, [email protected]

Vukotic, BranislavAstronomical Observatory, Belgrade,[email protected]

Wislocka, Agata MariaAstromundus student, [email protected]

Zekovic, VladimirFaculty of Mathematics, University ofBelgrade, [email protected]

Zivadinovic, LazarFaculty of Mathematics, University ofBelgrade, Serbialazar [email protected]

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AUTHORS’ INDEX

Anderton, R. J. 58Andjelkovic, S. 61Atanackovic, O. 31Bachev, R. 76Bailer-Jones, C. 43Bajcetic, J. 89Bajic, A. 71Belcheva, M. 73Belov, A. V. 81Benisek, V. 41Beslic, I. 61Bianchi, S. 13Bılek, M. 72Bisikalo, D. V. 14Boeva, S. 73, 76Bon, E. 16Bon, N. 16Borka D. 15, 40Borka Jovanovic, V. 15, 34, 40Boskovic, M. 32Bozic, N. 32Brunetto, R. 17Cadez, V. M. 74, 89Capozziello, S. 15, 34, 40Ciprijanovic, A. 33, 75Cirkovic, M. M. 39Cvetkovic, Z. 22, 63, 76, 93, 98D’Addio, A. 34Damljanovic, G. 76, 80, 93Delibasic, D. 35Dimitrijevic, D. D. 35Dimitrijevic, I. 36, 37Dimitrijevic, M. S. 38, 55, 71, 77, 78,

95, 96, 99Disterlo, Z. 79Djordjevic, G. S. 35Djosovic, V. 39, 92Djurasevic, G. 63, 98Donevski D. 52Dragovich, B. 36, 37Eroshenko, E. A. 81

Font, J. 43Gavrilov, M. B. 41Gravina, S. 40Hadjara, M. 42Ignjatovic, Lj. M. 55, 99Ilic D. 16Janc, N. 41Jankov, S. 42Jevremovic, D. 55Jovanovic, M. 104Jovanovic, M. D. 76, 80, 93, 103Jovanovic, P. 15, 16, 34Kanuchova, Z. 17Klyuyeva, A. I. 81Knezevic, S. 43Knezevic, Z. 19Kolarski, A. 89Kovacevic, A. 16Kovacevic, M. 51Kovacevic-Dojcinovic, J. 16Krstin, B. 82Lakicevic, M. 16Lasker, R. 43Latev, G. 73, 76Latkovic, O. 20Lukic, D. V. 83, 84, 85Mendez-Abreu, J. 43Maksimovic, M. 45Marceta, D. 44Marceta-Mandic, S. 16Markovic, S. B. 41Martinovic, M. M. 45Martinovic, N. 46, 49, 50, 54, 86, 87Melita, M. 17Micic, M. 46, 49, 50, 54, 86, 87Mijajlovic, Z. 47Miladinovic, A. 61Milic, D. 68Milic, I. 32Milic Zitnik, I. 48Milosevic, M. 35

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Milosevic, S. 32, 49, 50, 54, 68, 86, 87Mitrasinovic, A. 49, 50, 54, 86, 87Mitrovic, S. T. 89Moreau, N. 78Morlino, G. 43Nedeljkovic, A. B. 88Nikolov, G. 73Nina, A. 74, 89, 99Ninkovic, S. 60, 61, 90, 91Novakovic, B. 53, 92Obradovic, P. 61Obuljen, A. 32Onic, D. 21Palumbo, M. E. 17Pavlovic, M. Z. 75Pavlovic, R. 22, 63, 67, 76, 93, 98Pejovic, N. 47Petrov, R. G. 42Petrovic, J. 51Popovic, L. C. 16, 41, 89Prnjat, Z. 94Prodanovic, T. 51, 52, 75Protic - Benisek, V. 23, 41Puric, M. 61Radovanovic, M. 89Radovic, V. 53, 92Rakic, Z. 36, 37Raymond, J. C. 24, 43Sahal-Brechot, S. 78Sakan, N. M. 95, 96Samurovic, S. 25, 63, 72, 97, 98, 104Sarkovic, V. 61Savic, Dj. 16Segan, S. 45

Sijacki, D. 26Simic, S. 16, 89Simic, Z. 95, 96Simonovic, B. 61Smole, M. 49, 50, 54, 86, 87Spassov, B. 73Sreckovic, V. A. 55, 89, 95, 96, 99, 100Stalevski, M. 16, 56, 101Stanic, N. 57Stankovic, J. 36, 37Stoiljkovich, D. 58Stojanovic, M. 35Strazzulla, G. 17Sulic, D. M. 100Tibolla, O. 27Todorovic, N. 102Todorovic Drakul, M. 89Tomic, Z. 59Trajkovska, V. 60Urosevic, D. 21van de Ven, G. 43Vidojevic, S. 61Vince, I. 62, 103Vince, O. 63, 76, 80, 93, 98, 103, 104Vucetic, M. 64Vudragovic, A. 65, 104Vujcic, V. 55Vujicic, D. 67Vukadinovic, D. 32Vukotic, B. 39Zamanov, R. 73Zaslavsky, A. 45Zekovic, V. 105Zivadinovic, L. 68

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Organizers

The conference is being organized by: Astronomical Observatory of Belgrade together with Department of

Astronomy, Faculty of Mathematics, Belgrade University.

The conference is also supported by: Ministry of Education, Science and Technological Development

of the Republic of Serbia, Serbian Academy of Sciences and Arts, Telekom Srbija a.d. Beograd and

TRAYAL KORPORACIJA AD, Kruševac.

CIP-

52-355.3(048) 533.92:537.228.5(048) 520/524:376(048) SERBIAN Astronomical Conference (18 ; 2017 ; Beograd) Book of Abstracts / XVIII Serbian Astronomical Conference Belgrade, 17-21 October 2017 ; eds. L. . Popovi , D. Uroševi and R. Pavlovi . - Belgrade : Astronomical Observatory, 2017 (Beograd : Copy Planet). - 126 str. : ilustr. ; 24 cm Tiraž 120. - Bibliografija uz pojedine apstrakte. - Registar. ISBN 978-86-80019-85-7 1. Astronomska opservatorija (Beograd) a) - b) - - c) - - COBISS.SR-ID 246897420

XVIII Serbian Српска астрономска Astronomical Conference ...Olga Atanackovi¶c...

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