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Transcript of Russian-Italian Mission (RIM) 1993 - … A.M. Galper Rome 11.05.09.
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Russian-Italian Mission(RIM)
1993 - …
A.M. Galper
Rome 11.05.09
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Bari Florence Frascati
Italy:TriesteNaple
sRome CNR, Florence
St. Petersburg
Russia:
Germany:Siegen
Sweden:KTH, Stockholm
RIM-PAMELARIM-PAMELA
Moscow
Moscow
Italy:
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THE COSMIC RAY NUCLEI AND THE CENTRAL NERVOUS SYSTEM EXPERIMENTS ONBOARD OF THE SPACE STATIONS MIR AND ISS
(RIM—0)
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Practical aspects of the LF-phenomenon
The cosmonauts must be ready to LF phenomenon during space flight, especially if it is the long space flight out of the earth magnetosphere.
LF phenomenon's, which systematically will be arising especially before slipping cosmonauts, can to bring up to tiredness condition and to decreasing of the operational capability.
LF phenomenon capable to exert on operational capability.
The low sensitivity to LF phenomenon is a good property for future crewmembers of the Mars missions.
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Detector part of the SilEye apparatus
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0.001
0.01
0.1
1
0.1 1 10 100
LET (keV/k)
Prob
abili
ty L
F
before LF
after LF
The fraction of particles that occurred in the LF-
window (1.2–0.2 sec. before a registered LF signal) and “anti-LF” window (defined, being 0.2–1.2 s after the LF)
as a functions of LET
Sergey Avdeev on Mir with the SilEye-2 detector mounted on the side of his head and the mask with LED’s in front of
his eyes.
SilEye-2
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The ALTEINO experiment. On the left is shown the
electroencephalograph Halley, on the right the cosmic ray detector
AST.
The scheme of the electroencephalograph electrodes connections
Experiment “SilEye-3/Alteino” (April – May 2002, ISS)
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A schematic view of the cosmonaut with the ALTEA system
1. Detector system consists of an helmet shaped mechanical structure holding 12 active silicon telescopes, assembled in 6 independent units;
2. Electrodes of the EEG system with 24 monopolar channels plus 4 bipolar channels.
3. Visual Stimulator
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References
1. Bidoli, V., et al., Nuclear Instruments and Methods A, 1999, 424, 414.2. S.Avdeev, et all Acta Astronautica May 2002, vol 50/8 pp 511-525.3. Casolino, M., et al., Nature 422 (2003) 680.
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Experiment NINA(RIM--1)
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Experiments NINA 1,2
Scientific interest: Study of the nuclear and isotopic component of cosmic rays:
H - Fe --> 10--200 MeV/n (full containment)
Choice of the orbit: POLAR
so to be able to encounter differentfamilies of cosmic rays: galactic, albedo, trapped
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• Launch: 10 July 1998
• Space - Base Baikonur
• End of mission: • 13th April
1999.
Satellite RESURS-01 n.4:PERIOD ~ 100 min.ALTITUDE ~ 840 km INCLINATION 98.7 deg.
MASS 2500 kg
The detectora silicon wafer 6x6 cm2 , 380 m thick with 16 strips, 3.6 mm wide in X -Y views. 32 wafers arranged in 16 planes, 1.4 cm apart. In total almost 12 mm of silicon.Lateral and Bottom AC for Full Containment mass resolution <0.15 amu for He, <0.1 amu for H energy resolution < 1 MeV
NINA mission
NINA-2 missionSatellite MITA:PERIOD ~ 100 min.ALTITUDE ~ 400 km INCLINATION 87.3 deg.MASS 170 kg
• Launch: 14 July 2000• Space - Base Plesetsk• End of mission: 15th August 2001.
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ZENIT rocket Baikonur, Kazakhstan July 10 1998
COSMOS rocket
Plesetsk, Russia July 15 2000
NINA2-MITA
Sun-Earthpointing,89°, 440 km, 90’
Last scientific data in August 10, 2001, at 240 km altitude
NINA-RESURS
Earthpointing, 97°, 810 km, 100’
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Solar Energetic Particles
• 9 SEP events have been detected by NINA in October 1998 -- April 1999, and analyzed;
• 14 SEP events have been detected by NINA-2 in October 2000 – August 2001
• 3He/4He ratios and energy spectra determined;
• 7 Nov. 1998 event 3He-enriched[3He/4He=(0.33± 0.006)]
• All SEPs present a 3He/4He higher than coronal values;
• Possible presence of deuterium on 24 Nov. 1998 and 19 July 2001
• nuclear interactions, which could contribute to the 3He content in SEPs
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7 Nov. 1998 event3He/4He= 0.33 ± 0.006
[10--50 MeV/n]
3He-enriched
The 3He and 4He spectral indexes are:
The 3He/4He ratio increases with energy. Its low-energy extrapolation (~ 10-4) is consistent with ULEIS (ACE) [Mason, Mazur & Dwyer, ApJ, 525, L133, 1999] in the interval 0.2--2 MeV/n, which reported a value < 6x10-4.
3He --> = 2.5 ± 0.64He --> = 3.7 ± 0.3
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Galactic Cosmic RaysCosmic ray abundances, with the odd-even effect, the peaks at C and O, and the relative depression of the light elements Li, Be and B
Very good agreement among SIS, CRIS and NINA results
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Trapped particles mass reconstruction
The mass reconstruction confirms the presence of ‘real’ H and He isotopes in Radiation Belts. 3He is more abundant than 4He
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Albedo particlesEnergy spectrum of protons of albedo origin was measured at different geomagnetic locationBehaviour of the proton flux as a function of altitude and longitude out of the South Atlantic Anomaly was studiedNINA and NINA-2 measurements revealed that 2H, 3H, 3He and 4He are a significant portion of the secondary flux above the atmosphere
L-shell<3, B>0.26 G
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References
V.Bidoli, M. Casolino, M.De Pascale et al Isotope composition of secondary hydrogen and helium above the atmosphere Journal of Geophysical Research , 108, A5, 1211, 2003 •V.Bidoli, M. Casolino, M.De Pascale et al Energy spectrum of secondary protons above the atmosphere measured by the instruments NINA and NINA-2 Annales Geophysicae, 20, issue 10 (2002), 1693 (PDF) •A.Bakaldin, A.Galper, S Koldashov et al Geomagnetically trapped light isotopes observed with the detector NINA Journal of Geophysical Research, 107, N. A8 (2002), 1-8 •A. Bakaldin, A. Galper, S. Koldashov et al Light Isotope Abundances in Solar Energetic Particles measured by the Space Instrument NINA The Astrophysical Journal, 577:513–523, 2002 astro-ph/0106390 ,
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Space experiment onboard small size satellite of Lavochkin Association
The project “MONICA”:
“Monitor of cosmic ray nuclei and ions”
Russian participants:Moscow Engineering Physics Institute (State University) – Leading instituteLebedev Physical Institute of RASIoffe Physical-Technical Institute of RASJoint Institute for Nuclear Research
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Scientific objectives of MONICA experiment
Measurement of ionic charge states, as well as elemental, isotope composition and energy spectra of SEP fluxes from He to Ni in 10-300 MeV/n energy range for individual SEP events (including small impulsive SEP events). Measurement of ACR ion ionic charge and isotope composition, including new elements and isotopes, which have been observed on ACE (sulfur, isotopes of oxygen and neon and others); measurement of ACR energy spectra.Measurement of GCR and ACR fluxes modulation with the purpose of study of conditions of particle propagation in heliosphere.
Study of CR penetration into Earth magnetosphere under conditions of its strong disturbances during the solar-magnetosphere events.
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The technique of CR ion charge measurement: The usage of Earth magnetic field as a separator of ion charge state
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MONICA physical scheme
D1–D14 - silicon strip detectors
Detector Thicknesses:
D1, D2 – 100 µm
D3-D5 – 300 µm
D6-D14 – 1000 µm
SAC, AC – scintillation anticoincidence detectors
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Physical and technical characteristics of MONICA spectrometer
Geometry factor 100 cm2sr
Aperture 45
Angle resolution 1
Energy range
H
CNO
Fe
7-70 MeV
15-150 MeV/n
25-290 MeV/n
Energy resolution 1%
Mass resolution
H
CNO
Fe
0.02
0.08
0.2
Resolution time 50 ns
Dead time <1 ms
Outline dimensions 650650300 mm(preliminary)
Mass 40 kg
Power consumption Not more
then 80 W
Power supply voltage 27 V
Matter in aperture Not more
then 0.05 g/cm2
Mass memory 1 Gbyte
Information downloads
not less than one per day
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Small Size Satellite
Star Sensors
Place for scientific instrumentation
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Experiment PAMELA (RIM--2)
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MAGNETIC SPECTROMETER PAMELA1, 3, 7- TIME OF FLIGHT SYSTEM;2, 4- ANTICOINCIDENCE SYSTEM;5- SILICON STRIP TRACKER (SIX DOUBLE PLATES);6- MAGNET (FIVE SECTIONS); 8- SILICON STRIP IMAGING CALORIMETER;9- ANTICOINCIDENCE SCINTILLATOR; 10- NEUTRON DETECTOR; 11- HERMOCONTAINER.
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PAMELA Spectrometer
Shower tail catcherShower tail catcherScintillatorScintillator
ToFToF
Magnetic Magnetic spectrometespectrometerr
CalorimeterCalorimeter
AnticoincidenceAnticoincidenceshieldshield
Neutron DetectorNeutron Detector
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The Launch Resurs-DK1 № 1 15/06/06
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36 GV interacting proton
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PAMELA statusFirst switch-on on June 21st 2006
Detectors in nominal conditions (no problems due to the launch)Tested different trigger and hardware configurationsCommissioning phase successfull
May 7th 2009:PAMELA ON for 1058 days8023 files3728 downlinks13.5 TB
PAMELA in continuous data-acquisition mode
Experiment PAMELA will continue till the end of 2011
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Project GAMMA--400(RIM--3)
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GAMMA-400
FIELDS OF INVESTIGATIONS-The investigation of the nature of physical processes in astrophysical objects, responsible for the generation of high energy gamma-rays (1 GeV…3 TeV).
SCIENTIFIC OBJECTIVES OF GAMMA-400 EXPERIMENT
-The investigation of the nature and properties of weak interacting massive dark matter particles, via the processes of their annihilation and possibly the decay on gamma and electron-positron pairs.
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GAMMA-TELESCOPE GAMMA-400PHYSICAL SCHEME
АС – anticoincidence detector;SАС – side anticoincidence
detector;C– convertor;S1, S2 – TOF scintillators;CD1 – CD3 – coordinate strip detectors;CC1,CC2 – coordinate calorimeters (8 layers:W convertor+strip detector);CC3 – PbWO4 coordinate calorimeter ;S3, S4 – trigger scintillators;SLD – scintillator Shower Leakage Detector;ND – neutron detectorр.
Trigger
S1 (1...5 m.i.p.)
Х
S2 (1...5 m.i.p.) ХS3 (>10 m.i.p.) ХS4 (>20 m.i.p.)
1000
CD1
CD3
C
ND
АС
600
300
CC1
800
SLD
S1 (TOF)
S2 (TOF)
SАСSАС
CD2
Gamma-quantum
CC2
CC3
S4
S3
~1500
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GAMMA-TELESCOPE GAMMA-400 (TRD variant)PHYSICAL SCHEME
TRD – transition radiation detector;АС – anticoincidence detector;SАС – side anticoincidence
detector;C– convertor;S1, S2 – TOF scintillators;CD1 – CD3 – coordinate strip detectors;CC1,CC2 – coordinate calorimeters (8 layers:W convertor+strip detector);CC3 – PbWO4 coordinate calorimeter ;S3, S4 – trigger scintillators;SLD – scintillator Shower Leakage Detector;ND – neutron detector.
~1500
1000
CD1
CD3
C
ND
АС
600
300
CC1
800
SLD
S1 (TOF)
S2 (TOF)
SАС
SАС
CD2
Gamma-quantum
CC2
CC3
S4
S3
TRD Trigger
S1 (1...5 m.i.p.)
Х
S2 (1...5 m.i.p.) ХS3 (>10 m.i.p.) ХS4 (>20 m.i.p.)
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“NAVIGATOR” SATELLITE
GAMMA-400
Apogee hight 300 000 km;Perigee hight 500 km;Inclination 51,8˚;Orbit duration 7 days.
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PRELIMINARY CHARACTERISTICS OF GAMMA-400 GAMMA-TELESCOPE
Converter thickness 0.8 r. l.
Sensitive area 1000 х 1000 mm2
Geometric factor ~ 0.7 m2
Coordinate precision 1 mm
Angular resolution 0,05
TOF resolution 200 ps
Calorimeter thickness ~ 25 X0
Energy range 1 GeV - 3 TeV
Energy resolution (100 ГэВ - 3 ТэВ) ~ 1 %
Dimentions 1,5×1,5×2,0 м3
Weight of the gamma-telescope ~ 1700 kg
Energy consumption 700 W
Transferred information volume 20 Gb /day
Duration of experiment 5 years
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ARINA instrument on board the Resurs-DK1
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Instrument ARINAOn the basis of multilayer scintillation detector.
Acceptance of ARINA 10-50 times higher than acceptance of instruments, used in earlier experiments for similar studies.
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Formation of particle bursts of seismic origin
6• ЭМИ – electromagnetic emission of seismic
origin;• Line – lower boundary of the radiation belt
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Т distributions on the data of various satellite experiments
Т =(Тequake-Тburst),
L<0.1, L =ILequake-LburstI,
-12 -8 -4 0 4 8 120
10
20
30
40
50
60
70
PET/SAMPEX
# ev
ents
T, hour
-12 -8 -4 0 4 8 120
10
20
30
40
MARIA-2/station Mir
# ev
ents
T, hour
-12 -8 -4 0 4 8 120
10
20
30
40
ELECTRON/Meteor-3
# ev
ents
T, hour
-12 -8 -4 0 4 8 120
10
20
30
40
50
60
70
80
GAMMA-1/GAMMA satellite
# ev
ents
T, hour
-12 -8 -4 0 4 8 120
10
20NINA/Resurs-01
# ev
ents
T, hour-12 -8 -4 0 4 8 12
10
20
30
40
50
ARINA Resurs-DK1
# ev
ents
T, hour
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ARINA. Events 13 November 2006particle burst (4h.20m.); earthquake М=5.0 (6h.30 m.)
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EEG signals in “SilEye-3 / Alteino”
Answer waves
Time between LF and peak of the wave, ms
M σ m
N75 71.6 9.5 2.5
P100 100.3 22.8 5.9
N145 145
EEG signal (11 LF)
EEG signal in Ground experiments (150 LF)In flight EEG signals parameters