1. Yu. D. Kotov and CORONAS-PHOTON team Scientific objectives and observational capabilities of "Coronas-Photon" project Federal Space Agency Russian Academy of Science Principal Organization: Moscow Engineering Physics Institute (Technical University) TitleTitle

2. Russian program CORONAS КОРОНАС  Комплексные ОРбитальные Околоземные Наблюдения Активности Солнца CORONAS  Complex ORbital ObservatioN of Activity of Sun CORONAS-I с 03.1994 по 12.2000 (IZMIRAN, CB“Yuznoe”) CORONAS-F с 07.2001 по 12.2005 ----||---- CORONAS-F с 07.2001 по 12.2005 ----||---- CORONAS-PHOTON 2008  (Astrophysics Institute CORONAS-PHOTON 2008  (Astrophysics Institute of MEPhI, NIIEM, VNIIEM)

3. 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)

4. Magnetic field dominates plasma creates intricate structure/ heats Magnetic structure as it is seen in UV TRACE

5. Generation of gamma-rays in the solar atmosphere be accelerated particles

6. Electromagnetic radiation spectrum from intense solar flare

11. Cycle 24 Maximum The panel is split down the middle on whether it will be bigger than average or smaller than average, namely: Will peak at a sunspot number of 140(±20) in October, 2011 Or Will peak at a sunspot number of 90(±10) in August, 2012 –An average solar cycle peaks at 114 –The next cycle will be neither extreme, nor average

12. CONSENSUS STATEMENT OF THE SOLAR CYCLE 24 PREDICTION PANEL March 20, 2007 The Solar Cycle 24 Prediction Panel anticipates the solar minimum marking the onset of Cycle 24 will occur in March, 2008 (±6 months). The panel reached this conclusion due to the absence of expected signatures of minimum-like conditions on the Sun at the time of the panel meeting in March, 2007: there have been no high-latitude sunspots observed with the expected Cycle 24 polarity; the configuration of the large scale white- light corona has not yet relaxed to a simple dipole; the heliospheric current sheet has not yet flattened; and activity measures, such as cosmic ray flux, radio flux, and sunspot number, have not yet reached typical solar minimum values. In light of the expected long interval until the onset of Cycle 24, the Prediction Panel has been unable to resolve a sufficient number of questions to reach a single, consensus prediction for the amplitude of the cycle. The deliberations of the panel supported two possible peak amplitudes for the smoothed International Sunspot Number (Ri): Ri = 140 ±20 and Ri = 90 ±10. Important questions to be resolved in the year following solar minimum will lead to a consensus decision by the panel. The panel agrees solar maximum will occur near October, 2011 for the large cycle (Ri=140) case and August, 2012 for the small cycle (Ri=90) prediction.

14. A National Solar Observatory map of observed magnetic fields correlates closely with the NCAR model of the fields. Both images show the longitudinal averages of the fields. (Courtesy Mausumi Dikpati, Giuliana de Toma, Peter Gilman, Oran White, and Charles Arge). Scientists for years have known about the current of plasma, or the meridional flow, which moves at about 20 meters (66 feet) per second near the surface. But they had not previously connected it to sunspot activity. New model Mausumi Dikpati and colleagues (Geophys. Research Letters, March 3,2007)

15. Latitude distribution of the flares

16. As the plasma current approaches the poles, it sinks about 200,000 kilometers down into the Sun’s interior and starts its return journey back to the equator The Great Conveyor Belt is a massive circulating current of fire (hot plasma) within the Sun. It has two branches, north and south, each taking about 40 years to perform one complete circuit. Researchers believe the turning of the belt controls the sunspot cycle, and that's why the slowdown is important. " Normally, the conveyor belt moves about 1 meter per second-walking pace," says Hathaway. "That's how it has been since the late 19th century." In recent years, however, the belt has decelerated to 0.75 m/sec in the north and 0.35 m/sec in the south. "We've never seen speeds so low." According to theory and observation, the speed of the belt foretells the intensity of sunspot activity about 20 years in the future. A slow belt means lower solar activity; a fast belt means stronger activity. "The slowdown we see now means that Solar Cycle 25, peaking around the year 2022, could be one of the weakest in centuries," says Hathaway

17. Предсказания: Активность на 50% больше, чем в 23 цикле. Начало цикла в конце 2007 или начале 2008. Максимум в 2012 BUT! Phys. Rev. Lett. 98 131101 Arnab Rai Choudhuri and colleagues from the Indian Institute of Science in Bangalore and the Chinese Academy of Sciences in Beijing calculate that the next cycle (known as cycle 24) will be about 35% weaker than cycle 23 (11 April 2007)

18. W.Dean Persell, April 2007

21. Satellite CORONAS – PHOTON (METEOR type) Weight <2250kg Launcher: Cyclon-3M Cosmodrome: Plesetsk Orbit: Circular 550±10 km. Inclination 82.5 deg Nominal mission lifetime 3 years extended 5 years Telemetry 8.2 GHz; Onboard memory 1.0Gbyte Launching date at the summer season of the 2008 Orbit and Launcher

22. CORONAS-PHOTON Spacecraft Orientation of longitudinal axis to the Sun direction (day part of orbit) Pointing accuracy  10' (nominal)* Posteriori pointing accuracy  1.5' Destabilization of the longitudinal axis during the shadow part of the orbit  0.3'/sec Angular disturbance is less than 0.005 deg/s * Signals from instrument TESIS will be used to get: transverse axes stabilization longitudinal axis stabilization ≤0.5 deg ≤3′ Accuracy of time registration 1 msec

23. Scientific payload Instruments for registration of gamma- radiation and neutrons Seven Full Solar disk UV & soft X-ray monitors TESIS assembly of instruments for XUV imaging spectroscopy of the Sun Instruments for charge particle measurements Simi-imaging RT-2 X-ray monitor + Magnetometer

24. Российские участники проекта «КОРОНАС-ФОТОН » (создание научной аппаратуры)  Московский инженерно-физический институт (МИФИ), Москва - головной  Научно-исследовательский институт ядерной физики МГУ (НИИЯФ МГУ), Москва  Физико-технический институт РАН (ФТИ РАН), Санкт-Петербург  Физический институт РАН (ФИ РАН), Москва  Институт земного магнетизма, ионосферы и распространения радиоволн РАН (ИЗМИРАН), Троицк  Институт космических исследований РАН (ИКИ РАН), Москва

25. Зарубежные участники проекта «КОРОНАС-ФОТОН » (создание научной аппаратуры)  Харьковский национальный университет (ХНУ), Харьков, Украина  Taтa институт фундаментальных исследований (ТИФР), Мумбай, Индия  Сцинтилляционные детекторы США  Полупроводниковые детекторы CZT Израиль  Многоканальная электроника Норвегия  Центр космических исследований Польской академии наук (ЦКИ ПАН), Вроцлав, Польша  Полупроводниковый детектор США

27. Full Solar disk UV & soft X-ray monitors InstrumentRadiation bandsTemporal resolutionDetector type SphinX Space Res. Center, Poland PI J. Sylwester P.N. Lebedev PI, Russia MEPhI, Russia Soft X-rays 0.5 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 mm 2 (Amptek, USA) PHOKA Russia MEPhI, PI A.Kochemasov 4 channels (nm) Visible, FUV & XUV <1100; 116- 125; 27-37 & <11 Solar disk radiation monitoring 2 sec Occultation mode 0.1 sec AXUV-100G 10mmx10mm (International Radiation Detectors, CA, USA) SOKOL Russia, IZMIRAN, PI 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

28. TESIS assembly of instruments TESIS assembly of instruments for XUV imaging spectroscopy of the Sun It is advanced version of the SPIRIT instrument Kuzin S. et al; Cospar meeting 2006 talk E2.1 009 - 06

29. 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

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

32. Ground segment CORONAS-PHOTON project

33. NATALYA-2M

34. Energy channels of Natalya-2M instrument (defined by trigger mode)Channel Energy region, MeV Effective area, cm 2 Energy resolution ΔE/E Timing X-ray and gamma-rays R0,3 – 292010% (662 keV) measured 1 ms L2 – 109005% (2,5 MeV) measured 1 sec M7 – 2008006% (10 MeV) calculated 1 sec H50 – 200075032% (500 MeV) calculated 1 sec Neutrons N (neutrons)20 – 30037 – 120–32 sec

35. Data readout from the high-energy radiation spectrometer NATALYA-2M

36. Data readout from spectrometer KONUS-RF Two detectors based on NaI(Tl) scintillator Ø127x76.2 mm

37. Gamma-line response NATALYA-2M L-mode 1.0-10.0 MeV

38. neutron/gamma pulse shape discrimination 3D diagram of energy output verses pulse shape parameter in CsI(Tl) detector 14 MeV neutron beam calibration

39. Anticoincidence counter NaI(Tl) detector of scattering X-rays PTF counter to scatter X-rays Proportional counters Anticoincidence counter Pinguin-M (disassembled)

40. Three RT-2 detectors The Tantalum Coded Mask is coded by open and close pattern of squares of size 2.5mm. Its dimensions are 180 x180 x0.5mm. Mechanical slat collimator made up of Tantalum surrounded by a graded shield with viewing angles of 4º x 4º and 6º x 6º respectively. Four CDZ modules Two phoswich detectorsOne CZT detector

41. 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

42. Design characteristics of RT-2. Type Phoswich NaI(Tl)+CsI(Na) CZT Thickness (mm)3+255 Size (mm)117.6 dia 40 X 40 (4 numbers) ReadoutPMT1024 pixels (ASIC) Effective area (cm 2 ) (@60 keV) 10064 Energy resolution (@60 keV) 18%8 % Energy range 15 – 150 keV (extended 2 MeV) 10 – 100 keV Time Resolution (ms)10

43. Specifications of CZT detector Area 64 cm 2 Pixels 1024 Pixel size 2.5 mm X 2.5 mm (5 mm thick) Read-out ASIC based (8 chips of 128 channels) Imaging method Coded Aperture Mask (CAM)/ FZP Field of View 6 o X 6 o CAM 3 o X 1.5 oFZP Angular resolution 30 arcmin/ 30 arcsec Energy resolution 5% @ 100 keV (< 8%) Energy range 10 – 100 keV Up to 1 MeV (Photometric)

44. CZT: Hard X-ray detector of the future ….. Good energy resolution Good efficiency Pixelated : Moderate imaging Background estimation Avoids source confusion Background reduction Good spectroscopic detector Note: Used up to now only as a gamma-ray imager

45. Fresnel’s Zone Plate It is made up of Tantalum of 1 mm thickness and alternate solid and hollow regions with 4 flanges to support the overall structure.It is fabricated using MEMS. The deconvolution of source is done from the interference fringes formed by two zone plates.The radii of the annulus are governed by: r n = (n) 1/2 x r 1 where, r 1 = radius of innermost disc It has following advantages over contemporary decoding methods: (i)Very high order of precision of source location. (ii)Highly economical in terms of volume.

48. FXM YАlO3(Ce) YAP(Ce): Yttrium Aluminum Perovskite doped with Cerium (chemical formula YAlO3:Ce) is a non- hygroscopic, glasslike, inorganic scintillator with a high density, but a relatively low effective atomic number (36). The wavelength of maximum emission is 35 nm, the decay time is short, 27 ns, the light output is typically 40% of that of NaI(Tl) and the material is relatively stable over a wide temperature range. In intense flare temporal resolution up to 1ms dimensions of 13 mm in height and 68 mm in diameter

49. Multi-channel solar photometer SOKOL Continuous observations of the solar radiation intensity variations in range 280 - 1500 nm, relative intensity resolution 2х10 -6 of total solar intensity, observation angle - 2°. Technical parameters: radiation intensity is measured simultaneously in 7 optical spectrum bands by 8 photosensors: 280, 350, 500, 650, 850, 1100 and 1500 nanometers with the measuring bandwidth below 10% of the value of central wavelength. relative intensity resolution is 2х10 -6 of the total solar radiation intensity. temporal resolution of intensity measurements - 30 sec. spacial resolution is not available. photometer observation angle - 2°. precision of the photometer orientation towards the center of the solar disk is 5 arc. min. the photometer consists of the photosensors unit PU and electronics unit EU. Dimensions: PU - 130х130х510 mm. Weight: 5.2 kg. View of instrument

50. PHOKA bands

51. STEP-F instrument is able to register fluxes of: electrons 0.4 – 14.3 MeV; protons of 9.8 – 61.0 MeV; alpha-particles of 37.0 – 246.0 MeV. The detector block includes two identical silicon position-sensitive detectors and two scintillation detectors. Each silicon detector has the size of 45×45 mm and 350 μm thickness. Scintillation detectors are based on CsI(Tl) crystals and viewed by large area photodiodes. The average telescope field of view is 97×97°. The size of each of 36 matrix square elements of semiconductor detector is 7.3×7.3 mm, which allows to receive the average angular resolution in telescope total field of view about 8°. The effective area of each semiconductor detector is 20 сm 2, scintillation detectors is 36 and 49 сm 2. Geometric factor of STEP-F instrument is 20 сm 2 ·str.

52. STEP-F D1: Si, h = 0.03 cm 45×45 mm D2: Si, h = 0.03 cm 45×45 mm D3: CsI(Tl), h = 1.3 cm 60×60 mm D4: CsI(Tl), h = 1.0 cm 70×70 mm D1, D2 – silicon position-sensitive totally depleted pin-detectors; D3, D4 – scintillation detectors.