1. From Geo- to Heliophysical Year: Results of CORONAS-F Space Mission International Conference «50 Years of International Geophysical Year and Electronic Geophysical Year» September 16-19, 2007, Suzdal _______________________________________________ Sun CORONAS-F Solar-Terrestrial Physics

2. From First Satellite to Solar Space Observatory 1957-2007 2007 International Heliophysical Year 50 Years of the First Satellite 1957 International Geophysical Year

3. http://forecast.izmiran.ru Тел. (495) 775-43-57 (496 – 7) 51-19-34 Geophysical Forecast Center of IZMIRAN Every day TV forecasts of the Center Space Weather and its influence on the human activity

4. CORONAS-F Satellite

5. Время существования: July31, 2001 - December 6 2005 (4 года и 4 месяца) The Height of the Orbit ~ 500 км Orbital Period ~ 95 мин Inclination ~83° Investigations of the 23 rd Solar Cycle on CORONAS Satellites Wolf Numbers  **************  CORONAS-F  *********  CORONAS-I 1996 2001 2007

6. X-Ray Imaging of the Sun Simultaneous images in two spectral lines Images in the different spectral lines, corresponding to the various layers of the solar atmosphere Powerful active region and flare on the solar limb

7. Morphology of the solar activity Powerful flares and ejections on November 26, 2003

8. SOHO/LASCO New phenomena in the solar corona Plasma formations in solar corona with temperatures up to 20 MK. Coronal Mass Ejections CORONAS-F/SPIRIT

9. Magnetic Heating of the Solar Corona The sunspot number  7 keV 20 keV  Quit corona Heated corona New data on the heating of the solar corona and on the spectra of X-ray emission influencing on the Earth atmosphere.  10 keV

10. Global Oscillation of the Sun Global oscillations of the Sun have been studied and the dependence of its amplitude from the wavelength of observation have been established.

11. Solar Flares – the most powerful explosive phenomena in Solar system

12. The reconstruction of the magnetic field structure in the solar corona during the most powerful flare on September 7, 2005. Fundamental processes of the solar flare nature

13. 60-100 keV 40-60 keV 20-40 keV 15-40 keV Flare on October 29, 2003. Background Linear polarization of the hard X-ray emission in solar flares and generation of the beams of accelerated particles. beams

14. Atomic processes in solar flares For the first time the spectral lines of atomic transitions of solar plasma ions 1s-np и 1s 2 – snp with high value of quantum number n have been recorded Some new spectral lines in solar flares have been detected

15. The accelerating and nuclear processes in solar flares have been studied. For the first time the positrons from decay of the charged peonies have been recorded. A chemical composition of the solar atmosphere, gamma emission from the decay of the peonies, nuclear gamma lines from the most powerful flare, the spectra of relativistic protons up to 14 GeV have been studied. Nuclear gamma lines in solar flares

16. The contribution of the solar flare UV emission into the total solar emission flux influencing on the Earth.

17. Corona Mass Ejection – the most powerful and geo- effective phenomena in “Sun-Earth” system. SOHO CORONAS-F

18. Coronal Mass Ejection on the small heights were observed for the first time.

19. Coronal Mass Ejection on the small heights were observed for the first time.

20. Coronal Mass Ejection on the small heights were observed for the first time.

21. Extreme events in “Sun-Earth” system September, 2005 The manifestations of the solar extreme events in near-Earth space have been recorded and studied. October-November, 2003 January, 2005 Longitudinal asymmetry in localization of active regions on the Sun

22. Neutrons 200  400 MeV Gamma Emission E = 4  7 MeV Solar flare on October 28, 2003 Solar flare on November 4, 2003 Gamma emission and energetic neutrons from the powerful solar flares in near-Earth space

23. Radiation Environment in near-Earth space Oct 29 Oct 28, 2003 Radiation belts of electrons The motion of the Radiation belts inside the magnetosphere Distance to the Earth     

24. Maps of the Solar Cosmic Ray Intensities in Radiation Belts during Severe Magnetic Storms of October-November 2003 (night side, altitude 450 km) Protons 1.5-3 MeV Electrons 1.5-3 MeV Protons 14-26 MeV Electrons 3-6 MeV

25. Maps of the Solar Cosmic Ray Intensities in Radiation Belts during Severe Magnetic Storms of October-November 2003 (night side, altitude 450 km)

26. Variations of the Proton and Electron Fluxes in period of October 20 – November 5, 2003 (coordinates L-t)

27. Dynamics of the external Radiation belt during severe magnetic storms

28. Structural Reconstruction of the Magnetosphere Radiation Belt disappearance Destruction of the regular structure of the magnetic field and the region of trapped orbits of the particles During Severe Magnetic Storms

29. Maps of the energetic particle precipitation from the magnetosphere to the upper atmosphere of the Earth 1- Radiation belts 2- precipitation of the particles The precipitation of the energetic particles from the Radiation belts into atmosphere in near-equatorial regions of the globe. The enhancements of the background radiation is up to 30%, the life time of these precipitations is up to 8 days.

30. Maps of the luminescence of the upper night atmosphere in x-rays

31. Maps of the luminescence of the upper night atmosphere in x-rays (23.03.2002-23.09.2002)

32. The transmission of the solar x-ray emission by Earth atmosphere. Sun

33. CORONAS-F Cooperation Phys. Lebedev Inst. coronas.izmiran.ru ROSCOSMOS Russian Academy of Sciences