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Coronas-Photon Project The RT-2 experiment. CORONAS-PHOTON mission is the third satellite of the Russian CORONAS program on the Solar activity observations.

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Presentation on theme: "Coronas-Photon Project The RT-2 experiment. CORONAS-PHOTON mission is the third satellite of the Russian CORONAS program on the Solar activity observations."— Presentation transcript:

1 Coronas-Photon Project The RT-2 experiment

2 CORONAS-PHOTON mission is the third satellite of the Russian CORONAS program on the Solar activity observations. The main goal of the CORONAS- PHOTON mission is the study of the Solar flare hard electromagnetic radiation in the wide energy range from Extreme UV up to high energy gamma - radiation (~2000MeV)

3 RT-2/G RT-2/S RT-2/GA PINGUIN KONUS-RF PHOKA TESIS STEP-F Magnetometer pressure vessel N-2M KONUS-RF-anti

4 CORONAS-PHOTON mission summary

5 Instruments for optics and X-ray radiation

6 Satellite CORONAS – PHOTON (METEOR type) Weight <2250kg Launcher: Cyclon-3M Cosmodrome: Plesetsk Orbit: Circular km. Inclination 82.5 deg Nominal mission lifetime 3 years Extended 5 years Telemetry 8.2 GHz; Onboard memory 1.0Gbyte Data transmission rate 7.68Mbits/sec Launch: Januray 30, Orbit and Launcher

7 Effective areas

8 launch date Solar activity

9 NaI(Tl) CsI(Na) PMT Dynodechain 3 detectors (2 phoswich + 1 CZT & CMOS) 1 electronics box

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12 Aschwanden, solar flares E th = keV  = (10 – 20 keV)  = (30 – 50 keV) Width typically 100 s at high energies Use Lin et al. 20 keV flux for flare frequency

13 Solar Hard X-ray Observations

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16 RT-2/S, GRT-2/CZTRT-2/E Weight (kg)15, Power (W)8, 885 Dimension (mm)250 X 230 X X 230 X X 190 X 200 Detectors Type NaI(Tl)+CsI(Na) CZTGdOS CMOS Thickness (mm) Size (mm)117.6 dia 40 X 40 (3 numbers)24 X 24 ReadoutPMT768 pixels 256X256pixels Effective area (cm 2 ) Energy resolution18%8 % NIL Energy range 15 – 150 keV 25 – 150 keV 10 – 100 keV 25 – 100 keV 25 – 200 keV Time Resolution 1s + 100s sp. 100 ms + 10 s sp. 10 ms + 1 s sp. 1 s 100s imaging 1s 100 s imaging

17 RT-2 / S & RT-2/CZT Detector Modules

18 Det_1 (P) RT2-S Det_2 (P) RT2-G Det_3 (CZT) Processing Electronics Detector interface Satellite interface Total Satellite Payload

19 Design (RT-2CZT) CAM Assembly Collimator Assembly Detector Housing CZT Detectors FZP (2 pairs) CMOS CCD instead Of 1 CZT module

20 Coded Mask Imaging Concept Multiple pin-hole MASK Mask casts shadow on detector plane Shift of shadow pattern encodes source location Cross correlation of mask pattern with shadow recovers shift and locates sources

21 Fresnel’s Zone Plate It is made up of Tungstun of 1 mm thickness and alternate solid and hollow regions with flanges to support the overall structure. r n = (n) 1/2 x r 1 where, r 1 = radius of innermost disc

22 Implementation of Zone Plate MissionEnergyAngular Resolution INTEGRAL (CAM) 3-35 keV3’Astrophysics SWIFT (CAM) keV5’Astrophysics RHESSI (RM)3-17 MeV2’’-180’’Solar Physics RT-2 (FZP) keV2’’Solar Physics

23 CMOS CCD Detector RadEye 1Premium quality 25 by 50 mm active area 5,24,288 pixels (512 x 1024) Pixel size and intrinsic resolution 48µm (Silicon Photodiodes) Dark current (at 23°C) – 4000 e - /s Noise (at 1 fps) – 150 e - /s Frame rate – 0.01 to 4.5fps Operating temperature – 0 to 50°C Dark current doubles approx. every 8°C Threshold about 150 keV 30 keV with processing; cooling; low noise

24 Burst frequency (per day) Counts in RT-2 (10 s) Comments Solar max Solar min Micro-flares Flare statistics Flare spectrum (CZT: 1000 Or 5000 ??) Time resolved spectrum Configuration Concentrate on > 25 keV flares Wide bandwidth required: one Phoswich Change to > 25 keV CZT: Coarse imaging (correct to a few Arcmin to as low an energy threshold as possible) Imaging: A few arcseconds, particularly at high energies RT-2/S: keV; upto counts/s; M class flares RT-2/G: keV; upto counts/s; X class flares (use Aluminum window) RT-2/CZT: Three CZT detectors; upto 100,000 cts/s CZT1: keV; CAM; 2 arcminutes CZT2: keV; CAM. 2 arcminutes CZT3: keV; FZP 1 arcminutes One CMOS detector: keV FZP 2 arcseconds

25 Salient Features … Fastest time resolution : 0.3 ms (event mode; maximum 2500 counts/s) Normal mode: 8 channel counts : 10 ms All spectra : 1 s Total 6 kbytes in spectral mode 32 kbytes in event mode (7800 events)

26 Modes Debug mode - by command Solar Quiet mode - by command (100 s; 1 s) Solar flare mode - onboard intelligence (10 s; 0.1 s) SAA mode – by good/bad signal Earth occultation mode – by light/shadow signal

27 Data management RT-2/S & G 1 s count rates s spectrum throughout. 100 ms count + 10 s spectrum from 1 hr of flare data (threshold from > 25 keV counts) 10 ms count + 1 s spectrum from 20 minutes flare data CZT: 1 s count s image throughout CMOS: 1 s count s image for 1 hr of flare data.

28 Thanks


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