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Radiation Storms in the Near Space Environment

Radiation Storms in the Near Space Environment. Mikhail Panasyuk , Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University. Intensification of solar activity. Solar storms, Radiation storms, Geomagnetic storms. Radiation storms in several 100’s keV

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Radiation Storms in the Near Space Environment

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  1. Radiation Storms in the Near Space Environment Mikhail Panasyuk, Skobeltsyn Institute of Nuclear Physics of Lomonosov Moscow State University

  2. Intensification of solar activity Solar storms, Radiation storms, Geomagnetic storms

  3. Radiation storms in several 100’s keV particles flux variations

  4. Topics to search Where are these guys from? - radiation belt; - SEP events; - ionosphere What kind of physical mechanisms for acceleration and transport are dominated during extreme events? - radial diffusion; - local rapid acceleration; - injection ; - local losses

  5. Earth’s radiation environment Galactic cosmic rays Solar energetic particles Radiation belts

  6. Energetic particles instruments onboard Coronas-F • SONG (Solar Neutrons and Gamma- rays) • MKL (Monitor of the cosmic rays) • SKI-3 (Cosmic ray nuclei detector)

  7. CORONAS-F: MKL,SKI, SONG, instruments: Electrons~ 0.3 -12 МeV& Protons ~ 1 - > 200 МэВ Ions р -Mg with 2 -30 MeV/nucl X, gamma –rays with ~ 0.03 - 200 МэВ Neutrons Skobeltsyn Institute of Nuclear Physics

  8. CORONAS – F gave us new results on: • SEP generation during solar flares; • SEP penetration; • dynamics of proton and electron radiation belts.

  9. Earth’s Radiation Environment Galactic cosmic rays

  10. Cosmic rays inside the magnetosphere Coronas-F Oct-Nov’03 event : GCR: -Forbush effect up to ~ 30% -Semiduirnal variations up to ~10-15 %. SP NM GOES -SEP: increasing;

  11. Earth’s Radiation Environment Solar energetic particles

  12. SEP radiation storm • Acceleration at solar flare site; • Propagation in IPM with modulation, acceleration by CME shocks; • Penetration inside the magnetosphere and partial trapping(?)

  13. Oct. – Nov.’03 CORONAS-F data 2,3-4,2 MeV/nucl AR 484 H He Short time delay, quick-time front, large anisotropy and absence of dispersion (during ~12 h). Λ is large 4,4-19 MeV/nucl H He

  14. Oct. – Nov.’03 CORONAS-F data 2,3-4,2 MeV/nucl H AR 486 He Free particles propagation with modulation by a shock wave 4,4-19 MeV/nucl H He

  15. Oct. – Nov.’03 CORONAS-F data 2,3-4,2 MeV/nucl H AR 486 He 2 –days flux increase, diffusion propagation, Λ is extermely small 4,4-19 MeV/nucl H He

  16. October- November’03 radiation storm CORONAS-F / solar gamma-rays,neutrons The second – delayed phase Pion-decay production The first phase Shock-wave acceleration

  17. Tatiana radiation storm 20.01.05 Тatiana

  18. Две фазы вспышки в  - излучении. Tatiana radiation storm CORONAS-F / solar gamma-rays,neutrons Gamma –rays with > 60 MeV as a result of interactions of > 200 MeV protons

  19. SEP penetration

  20. October- November’03 Radiation Storm SEP penetration at low altitudes – low-latitude boundary of SEP penetration b SEP Satellite’s orbit

  21. Transmission function during quiet/stormy magnetosphere Effective rigidity of penetrating particles decreases during magnetic storm periods b

  22. October- November’03 Radiation Storm SEP penetration at low altitudes

  23. October- November’03 Radiation Storm SEP penetration at low altitudes Kp- dependence Evening

  24. October- November’03 Radiation Storm SEP penetration at low altitudes Dst -dependence Evening

  25. October- November’03 Radiation Storm SEP penetration at low altitudes MLT - dependence Morning Evening Morning Evening Neither Kp or Dst indexes are not representative for a global distribution of SEP penetration Dst Kp

  26. October- November’03 Radiation Storm SEP penetration at low altitudes Variation of proton penetration boundary during isolated substorm Coronas-Fdata, Skobeltsyn Institute of Nuclear Physics Substorm activity as a regulator of SEP’s penetration

  27. Earth’s radiation environment Radiation belts

  28. October- November Radiation Storm Radiation belt dynamics Electron radiation belts Dynamics of relativistic electron belts

  29. October- November Radiation Storm Energetic electrons & protons dynamics /Coronas F data Oct.,29 Electron radiation belts Oct.,28 Inward movement of RB Redistribution plus acceleration of energetic radiation inside the traping region Coronas-F data, Skobeltsyn Institute of Nuclear Physics

  30. Electron belt variations 3 phases: SEE injection, depletion, then new RB formation

  31. SEP trapping

  32. Solar energetic particles as a source of RB population Ejection of SEP inside the RB really exists 10 MeV protons There are some doubts that this source is important for the quiet-time structure of the RB

  33. Solar energetic particles as a source of RB population One should expect the life-time of SEP particles to be very small because of their high rigidity (see Alfven criteria). Therefore, the probability of observing SEP particles inside the RB is small Criteria for stable trapping: L/M ~ LB/B= <<1 L - larmour radius, M –magnetic field line curvature, B - magnetic field magnitude

  34. Proton belt variations The new proton belts > 1MeV 6-12.11.03 23-30.11.03 >14 MeV Impulsive acceleration or nonadiabatic process?

  35. Proton belt variations 2 phases: -SEP injection, then -new proton belt formation

  36. Proton belt variations • 3 phases: • -SEP injection, • depletion, • then • -new proton belt • formation

  37. Geostationary radiation storms vs LEO polar radiation storms

  38. Daily averaged data Coronas-F

  39. Solar protons cause radiation storms at LEO GOES Inner zone

  40. Intensity of radiation storm at LEO polar orbits on daily averaged time scale is mainly dependent on SEP penetration at low latitudes than on effects of RB’s particles redistribution or (and) acceleration at low latitudes

  41. SEP doses effects

  42. October- November Radiation Storm ISS dosimetry ISS/SRC,R16 data, SINP, IMBP

  43. October- November Radiation Storm ISS dosimetry DB-8 ISS/SRC,R16 data, SINP, IMBP R16

  44. October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data October,03 ISS Solar particles dose effect : 140mrad

  45. October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data October,89 October,03 ISS Solar particles dose effect : 140mrad

  46. October- November’ 03 vs October’ 89 Radiation Storms: ISS/R16 data October,89 MIR Solar particles dose effect (total): 3070mrad October,04 ISS Solar particles dose effect : 140mrad

  47. Calculated ISS doses vs initial orbital parameters Oct., 28, 2003 Dose DB-8 detector onboard ISS Longitude

  48. Conclusions • SEE for LEO: -Intensification of electron component of RB & -Enhancement of proton (ion) fluxes due to SEP penetration

  49. Thank you

  50. The new proton belt formation

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