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Principle Investigator: Dr. Yu.D. Kotov Tel/fax (007-095)-3240616 E-mail: kotov@mephi.ru

Launch date: end of 2007, from Plesetsk (Russia). Space Research Program. RUSSIAN SATELLITE PROJECT "CORONAS-PHOTON" FOR THE STUDY OF SOLAR FLARE HARD RADIATIONS. Russian Aviation and Space Agency Russian Academy of Science Principal Organization: Moscow Engineering Physics Institute.

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Principle Investigator: Dr. Yu.D. Kotov Tel/fax (007-095)-3240616 E-mail: kotov@mephi.ru

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  1. Launch date: end of 2007, from Plesetsk (Russia) Space Research Program RUSSIAN SATELLITE PROJECT "CORONAS-PHOTON" FOR THE STUDY OF SOLAR FLARE HARD RADIATIONS Russian Aviation and Space Agency Russian Academy of Science Principal Organization: Moscow Engineering Physics Institute Principle Investigator: Dr. Yu.D. Kotov Tel/fax (007-095)-3240616 E-mail: kotov@mephi.ru

  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). It is adopted as a part of the Russian Federal Program of Fundamental Space Researches.The project is a part of International Living With the Star (ILWS) program. Goal of the project: Investigation of the process of energy accumulation and its transformation to the energy of accelerated particles during solar flares, study of the acceleration mechanisms, propagation and interaction of the fast particles in the solar atmosphere.

  3. Main objectives of the mission • Direct solar flare radiation • Study of the temporal dynamic of hard electromagnetic radiation from full disk in a wide energy range from EUV to 2000MeV; • Study of spatial and temporal dynamics of hot plasma regions in Solar atmosphere by observation of X- ray/XUV radiation; • XUV full Sun spectroscopy; • Nuclear gamma-lines spectroscopy of Solar activity regions; • Detection of solar neutrons with energies higher 20MeV; • Measurement of linear polarization and rapid variability of hard X-ray emission during the flares; • Monitoring of the Solar extreme ultra-violet (EUV), soft and hard X-ray emissions;

  4. CORONAS-PHOTON missionscientific Payload: • High energy radiation spectrometer NATALYAGamma-rays spectroscopy 0.3 – 2000MeV;Neutrons 20 – 300MeV • Low energy gamma-ray spectrometerRT - 2Phoswich mode: 15 – 150keV; Spectrometric mode: 100 – 2000keV • Hard X-ray polarimeter PENGUIN-M(X-ray radiation 1 – 10keV; X-ray polarization 20 – 150keV; X-ray & gamma-ray spectroscopy 0.15 – 5MeV) • Fast X-ray monitor FXM(Hard X-ray with sub-msec temporal resolution 20 – 500keV) • Solar flare and cosmic gamma-burst spectrometer KONUS-RF(Hard X-ray & gamma-ray spectroscopy with high temporal resolution (0.0112)MeV) • XUV TeleScope/ Imaging Spectrometer TESIS • Multi-channel Extreme ultra-violet and Soft X-ray monitorPHOKA (Timing of the full disk radiation in 7 spectral windows from 10nm to visual band ) • Energetic particle analyzerELECTRON-M-PESCA(e : 0.2 – 2MeV p : 1.0 – 150MeV α : 1.5 – 50MeV/nucleon Nuclei (Z <26) 2.0 – 50MeV/nucleon) • Energetic particle telescopeSTEP-F(e : 0.15 – 10MeV p : 4.0 – 62MeV α : 15.5 – 245.5MeV)

  5. Orbit and Launcher Circular 500 km; Period 95 min (60 min Sun/orbit) Orbit inclination 82°5 ; 2 weeks/ 3 months full Sun orbits Launcher: Cyclon-3M Launching date 2007 Lifetime 3 –5 years Weight satellite: 1900 kg; scientific payload: 540 kg

  6. Overview of TESIS instruments The goal of the experiment “TESIS” is to study the structure and the dynamics of the solar atmosphere over a broad range of heights and temperatures using full sun XUV spectroscopic imaging. Lebedev Physical Institute of the Russian Academy of Sciences The main emitting ions and wavelengths Ion Wavelength, Å T, ºK HeII 304,8 5*104 SiXI 304.3 1.6*106 FeVIII-FeXX 132; 1. & 12*106 MgXII 8.418; 8.423 (1-2)*107 Spectroheliograms 280 to 330 (0.05- 12)*106

  7. Main parameters of TESIS channels

  8. Optical layout of the XUV telescopes of TESIS instrument Artificial moon 304A 132A Entrance filter Detector Shutter Multilayer mirror Pointing and focusing mechanism

  9. Wide field EUV Telescope:

  10. MgXII spectrogeliograph synthetic quartz 2d=8.501 A 80x120 mm

  11. Typical image given by the spectroheliograph

  12. Deep spectroheliogram to show a large extension of 304 emissions

  13. SphinXSolar Photometer in X-ray PI – Janusz Sylwester SRC PAS

  14. Main features of the TESIS experiment • Full disk spectroscopic imaging: 4 EUV channels 1 MgXII channels • Simultaneous observations in all spectral channels • Temporal resolution up to 0.5 sec • XUV observations of the corona, up to 5 solar radius • Full Sun spectroheliograms in 280- 330 A • Ritchey-Chrétien Wide FOV 304 telescope • SphinX Solar Photometer in X-rays • Study of the upper Earth atmosphere • Observation of space debris

  15. On board computing and data collection features • 50MIPS DSP • 128MB data RAM • Up to 4 Ch. Simultaneously + SphinX • 8 sec readout time (2Kx2K image) • Update on board S/W • Loose less data compression algorithm (c.r. 2-4) • JPEG like data compressionalgorithm (c.r. 10-???) • 500 MB/day data rate

  16. TESIS Coronas-Photon doing electrical tests at  MEPhI  Sept 2005

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