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

From First Satellite to Solar Space Observatory 1957-2007

2007 International Heliophysical Year

50 Years of the First

Satellite

1957 International

Geophysical Year

http://forecast.izmiran.ruТел. Тел. ((495495)) 775-43-57 775-43-57 ((496496 – – 77)) 51-19-34 51-19-34

Geophysical Forecast Center of IZMIRAN

Every day TV forecasts of the Center

Space Weather and its influence on the human

activity

CORONAS-F Satellite

• 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 23rd Solar Cycle on

CORONAS Satellites

Wolf Numbers

**************

CORONAS-F*********CORONAS-I

1996 2001 2007

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

Morphology of the solar activity

Powerful flares and ejections on November 26, 2003

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

Magnetic Heating of the Solar Corona

The sunspot number

7 keV20 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

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.

Solar Flares – the most powerful explosive

phenomena in Solar system

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

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

Atomic processes in solar flares

For the first time the spectral lines of atomic transitions of solar plasma ions 1s-np и 1s2– snp with high value of quantum number n have been recorded

Some new spectral lines in solar flares have been detected

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

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

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

SOHO

CORONAS-F CORONAS-F

CORONAS-F

CORONAS-F

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

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

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

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

Neutrons200 400 MeV

Gamma EmissionE = 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

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

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

Electrons 3-6 MeV

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

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

Dynamics of the external Radiation belt during severe magnetic storms

300 301 302 303 304 305 306 307 308 309 310Д н и 2 0 0 3 г .

L

lgJe

(0.3

-0.6

МэВ

)

L

lgJe

(0.6

-1.5

МэВ

)

L

lgJe

(1.5

-3М

эВ)

8.5

4.0

2.4

1.7

1.3

1.18.5

4.0

2.4

1.7

1.3

8.5

4.0

2.4

1.7

1.3

1.1

1.1

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

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.

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

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

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

Sun

CORONAS-FCooperation

Phys. Lebedev Inst.coronas.izmiran.ru

ROSCOSMOS

Russian Academy of Sciences