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

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Presentation transcript:

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

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

Radiation storms in several 100’s keV particles flux variations

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

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

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

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

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

Galactic cosmic rays Earth’s Radiation Environment

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

Solar energetic particles Earth’s Radiation Environment

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

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

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

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

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

Тatiana radiation storm Tatiana

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

SEP penetration

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

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

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

SEP penetration at low altitudes Kp- dependence Evening

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

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

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

Radiation belts Earth’s radiation environment

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

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

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

SEP trapping

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

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

Proton belt variations The new proton belts Impulsive acceleration or nonadiabatic process? > 1MeV >14 MeV

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

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

Geostationary radiation storms vs LEO polar radiation storms

Coronas-F Daily averaged data

GOESInner zone Solar protons cause radiation storms at LEO

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

SEP doses effects

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

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

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

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

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

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

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

Thank you

The new proton belt formation

Polar LEO flux GEO flux Dst Polar LEO radiation storm at low latitudes

Inner zone Solar protons GOES Daily averaged

Conclusions 1.Solar extreme events (SEE) can really cause the drastic changes in the earth’s radiation environment, but their value depends on their geoefficiency

Bengin,et al,1992 Mir doses during the solar flares Doses increased in several times because of penetration of SEP at LEO. Kp «Mir» data October 19, 1989 :

ISS doses during Oct.- Nov.’ 03 LEO – GEO measurements disageement ?