Past political opportunities: Intercosmos 1967 no launch payments .
-
Upload
joella-harvey -
Category
Documents
-
view
215 -
download
0
Transcript of Past political opportunities: Intercosmos 1967 no launch payments .
Past political opportunities:
Intercosmos 1967 no launch payments http://www.cbk.pan.wroc.pl/body/publikacje/2005/PTA_Solar_htm.html
Kapustin YarSounding rockets
7 launches
19701971197719791980198119831984
PlesetskOrbital
missions3 launches
1994
Coronas-I
1995Interball-Tail
2001Coronas-F
The First Polish Space experiment
Pin-hole cameras
SphinX soft X-ray spectrophotometerThe Team: PI Janusz Sylwester
Mirek Kowalinski : Project ManagerJarek Bakała: Project ConstructorSzymon Gburek: Project Scientist
Marek Siarkowski, Barbara Sylwester, Zbigniew Kordylewski, Piotr Podgórski,
Witold Trzebiński, Stefan Płocieniak, Anna Kępa•FIAN: Dr. Sergey Kuzin, TESIS PI
•MEPhI: Yury Kotov, CORONAS-Photon PM
•AI CzAS: Dr. Franta Farnik•Prof. Fabio Reale, INAFA, Palermo University
Prof. Ken Phillips, UCL, London http
://w
ww
.cbk
.pan
.wro
c.pl
/bod
y/pu
blik
acje
/200
8/S
phin
X.p
df
CORONAS-F
CORONAS-F launch, orbit & pointing31 July 2001, polar orbit, 95min, ~500 kmsemi-Sun-synchronous
x10,
SS-14 Cyclone
http://coronas.izmiran.rssi.ru/F/instruments
RT-2/G
RT-2/S
RT-2/GA
PINGUIN
KONUS-RF
PHOKA
TESIS STEP-F
Magnetometer
pressure vessel
N-2M
KONUS-RF-anti
Launch is fixed to the last week of 2008 !
SphinX
Instruments for registration of gamma-radiation and neutrons
Instrument Measured radiation Organizations Weight kg High energy
radiation spectrometer
NATALYA-2M
Gamma-rays spectroscopy 0.3 – 2000MeV;
Neutrons 20 – 300MeV
Moscow Engineering-
Physics Institute (MEPhI)
PI Yu.D.Kotov
360.0
Solar flare and GRB
spectrometer KONUS-RF
Hard X-ray & gamma-ray spectroscopy with high temporal resolution (0.0112) MeV
Ioffe Physical-Technical Institute,
PI E.P.Mazets
31.5
Hard X-ray polarimeter
PENGUIN-M
Soft X-rays 1 – 10keV Hard-X-ray polarization 20–150keV Spectroscopy 0.15 – 5MeV;
Ioffe Physical-Technical Institute,
MEPhI PI A.S.Glyanenko
29.5
Fast X-ray monitor FXM
Hard X-ray with sub-msec temporal resolution 20 – 500keV
MEPhI PI V.N.Yurov
10.5
Low energy gamma-ray
spectrometer RT - 2
Hard X-ray spectroscopy: Phoswich NaI(Tl)/CsI(Na) 15 – 150keV; 100–2000keV CZT - detector 10-100keV
TATA Institute of Fundamental
Research (TIFR), ISRO and others
PI. A.R.Rao
68.0
Full Solar disk UV & soft X-ray monitorsInstrument Radiation bands Temporal resolution Detector type
SphinXSpace Res. Center,PolandPI J. Sylwester P.N. Lebedev PI, Russia MEPhI, Russia
Soft X-rays0.5 keV– 15 keV
Solar disk radiation monitoring up to 10 msec
Pure Si PIN-diode 500μm thick, aperture 19.96, 0.397 and 0.0785 mm2 (Amptek, USA)
PHOKAMEPhI, RussiaPI A.Kochemasov
4 channels (nm) Visible, FUV & XUV <1100; 116-125; 27-37 & <11
Solar disk radiation monitoring 2 secOccultation mode 0.1 sec
AXUV-100G 10mmx10mm(International Radiation Detectors, CA, USA)
SOKOLIZMIRAN, RussiaPI V.D.Kuznetsov
7 Visible & NUV channels (nm)1500, 1100, 850, 650, 500, 350, 280 (bandwidth <10%)
Solar disk radiation monitoring 30 sec
Photodiodes with filter (effect. square
TESIS assembly of instrumentsTESIS assembly of instruments for XUV imaging spectroscopy of the Sun
Name of channel
Parameter
FeXX XUV
telescope
HeII XUV
telescope-coronagraph
WF XUVwide
field telescope-
coronagraph
Mg XII spectro-
heliometer
XUV spectro-
heliometer
SphinX Solar
Photometer in X-rays
Spectral band, ?
131-133 295-315 8.418-8.423 280-335 1- 10 keV
Field of view
Full disk: 60
60 in the field of 2.5
Corona up to 5 radii - 2.5
Full disk: 60
1.6 (cross to dispertion)
Spatial resolution, arcsec
1,7 4.4 2 3 (cross to dispertion)
256 channel
Spectral resolution
/~70 /~20 /~20 2*10-4 ? /pix 2*10-2 ? /pix Full Sun
It is advanced version of the SPIRIT instrument
http://www.tesis.lebedev.ru/
SphinX & TESIS
TESIS
SphinX
Instrument Measured radiation Organizations Weigh, kg
Energetic particle analyzer
ELECTRON-M
e : 0.2 – 2MeV p : 1.0 – 150MeV He: 1.5 – 50MeV/nucleon
Institute of nuclear physics of Moscow
State University; PI S.N.Kuznetsov
16.0
Energetic particle telescope STEP-F
e : 0.15 – 10MeV p : 4.0 – 62MeV He: 15.5 – 245.5MeV
Kharkov State University
PI I.I.Zalubovsky
7.5
Instruments for charge particle measurements
Magnetometer
SM-8M
three components of magnetic field in the range of –55 T … +55 T
FGU NPP “Geologorazvedka”, St-Petersburg, Russia;
MEPhI, Russia
PI V.N.Yurov
3-axis magnetometer
SphinX construction
• EUV filters (doubly aluminized Mylar)
• Photometer– Collimators (+-2.5 deg)
– Three apertures– D1, D2, D3
• Shutter– Stepper motor
• FFU– Filters– Targets– D4
• Electronics– Front end Amptek– Digital „our”
• Controller– Software– reprogramming
• Heat sink• Alignment mirror
Measurement channels
φ: 5 mmA: 13.0 mm2
8 μsUp to
60 000 cts/sFWHM: 490 eV
P h o t o m e t r i c FFU
φ: 4 mmA: 0.26 mm2
25 μsUp to
20 000 cts/sFWHM: 290 eV
φ: 4 mmA: 0.0052 mm2
25 μsUp to
20 000 cts/sFWHM: 290 eV
φ: 4 mmA: 13.0 mm2
25 μsUp to
20 000 cts/sFWHM: 290 eV
Detectors (four units): 256/1024 energy binsAmptek, Peltier cooled (-50 deg) Si PIN diodes.
Detectors’ support plate thermally connected to external heat radiator
via heat sink pipe.Photon arrival time measured to within 2μs (in
Time Stamping Mode)Much better energy resolution than gas
detectors2.5 % against 16%, low thermal noisehttp://www.carroll-ramsey.com/detect.htm
$4000
Expected total count rates
Courtesy; Marek Siarkowski
SphinX calibration BESSY synchrotron
RAS Meeting 9 May 2008 Janusz Sylwester, Poland: Ongoing and future solar X-ray experimenting
March 2nd 2008D3
Berlin February 26th 2008
How it looks from the tests
BESSY Berlin Synchrotron:- All detector linearity: perfect (0.1% ) over 0.8-14.5 keV; dynamic range 104.- absolute response known to better than 5% against reference synchrotron source.
- pile-up matrices known as measured from X-ray 4 crystal monochromator spectra
obtained at 8 energies between 1.5 and 8 keV
The BESSY synchrotron input spectrum (red) with overplotted response of SphinX D2 detector (black). Nominal effective areas have been used. The agreement is better than 5% in the energy
band where SphinX detectors are the most sensitive.
The measurement environment, bcgd: ~few cts/s up to 103 cts/s (SAA)
SAA Night RB RB Night Flare
CORONAS-FPrevious CORONAS-F
orbit Important pahases• S/C X-ray day• S/C optical day
• S/C optical night• S/C X-ray night
Terminator crossing
Time stamping mode D1, D2 or D3 rates < 103/s
• Time stamping mode from: D1, D2, D3, D4– 2 Bytes for processor time of the detector event start– 1 byte for the amplitude– Allows to determine the difference between events to
within 2 μs ~2/1000 accuracy– Absolute timing to within 0.001s against UT
Expected ratesD1= 103 events/s (event: Amplitude 1byte, time 2 bytes)-3 KB/sD2= 10 events/s, D3= 10 events/s, D4= 10 events/s
Total: 3Kbytes/s – can last for ~10000s (3 h) each dump – may cover 100% cycle with compression
Waiting time analysis – is the process at low count rate Poissonian?
Wheatland, The Astrophysical Journal, Volume 679, Issue 2, pp. 1621-1628, 2008
• Radioactive sources give an ideal example of the statistics
• To what degree the arrival times of photons from the „quiet” corona have „no memory” i.e they have the exponential waiting time distribution? (Models for flare statistics assume or predict that flares are independent events- however this is under question)
• The primary task for the initial part of the mission where the activity is expected to be low.
SphinX convolved spectra (Acoronal)
5 MK10 MK
25 MK
Si
S
ArCa
Fe
Ni
NiFe
O, Ne,Fe Shape depends on T
pure continuum
Predicted behaviour of activity during active phase of Coronas-Photon
http://science.nasa.gov/headlines/y2006/10may_longrange.htm
Recent GOES & RHESSI
Energy Calibration
• D1,D2,D3 solar induced fluorescence spectra of pure elements– During flares ~> M1– Until 10^6 cts collected for each detector– Approximately each month– If v. quiet condition then on the command from
the ground for 10 min
Terminator transit: Profile of Earth atmospecric absorption
• X-ray terminator crossing algorithm operational on board– Predict the entry/exit to within few seconds– Spectra 256 energy bins each 0.1 sec give at
least 1 km resolution in the vertical Earth absorption profile
– Time stamping or spectral mode depending on the flare flag
SphinX firstshttp://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The_Sp
hinX_Instrument_on_CORONAS-PHOTON • SphinX will measure absolute element abundances using line
features due to neon, magnesium, silicon, sulphur, argon, calcium, iron and nickel in various levels of solar activity (quiet Sun, active regions and flares). It should therefore be in a strong position to give a definitive answer to the continuing debate about the dependence of coronal abundances of elements on their first ionization potential, the so-called FIP effect.
• SphinX will obtain the first absolutely calibrated solar X-ray spectra in the 0.8--15 keV range. In particular this will help us to understand the RHESSI continuum observations in this difficult range.
• SphinX will also study quiet coronal heating processes via photon arrival time--distance analysis (the arrival time of an X-ray photon will be measured to a couple of microseconds); X-ray oscillations in the <1 to 500 s period range; and transient ionization in flares.
Instrument satus• Flight model at the Moscow „factory” undergoing final electro-
magnetic & teelmetry compatibility tests• On November 30, TESIS ( a mother instrument for SphinX) is
coming for a final maintenance tests to FIAN (MK+WT) will reload the flight programme
• The Coronas-Photon launch is expected before the end of 2008 a X-mas present?
• Ground sector of software v1 ready (Czech contribution under guidance od Szymon)– 2 mirror servers (Wrocław, Ondrejov)– Automatic data access to FIAN SphinX data stream (~12 hours
maximum delay if 2 dumps/24h)– Automatic reduction to Level2– Data publishing to the public access area (90% data will go there
decision taken by the duty scientist)– Automatic flare event catalogue creation start,max, end, class, Tmax,
Emmax, rise phase dur L, H, EMmax-Tmax delay– Auxiliary data available: GOES, RHESSI, SOXS
The FFU unit (filter-fluorescence unit)
Filter-Fluorescence Unit (FFU) layout
This unit will be active all the time: time stamping < 1000 cts/s or spectra (256 bins)