COSMIC RAYS IN THE SOLAR ENVIRONMENT

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COSMIC RAYS INTHE SOLAR ENVIRONMENT

• José Fco. Valdés-Galicia
• Departamento de Investigaciones Solares y
  Planetarias
• Instituto de Geofísica
• Universidad Nacional Autónoma de México

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THE HELIOSPHERE
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A Birds eye view of the Solar Interior
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SUNSPOTS
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SOLAR TOTAL IRRADIANCE
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Solar minimum
Solar maximum
Xray images
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THE SOLAR CORONA
1973
1991
1994
1980
It must be very hot otherwise it wouldnt be so
extended
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SOLAR ATMOSPHERE TEMPERATURES
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THE BALLERINA SKIRT
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The ballerina skirt trough the solar cycle
Maximum
During maximum the ballerina skirt reverses
polarity for the next minimum. The magnetic cycle
of the Sun (Hale) takes 22 years.
Minimum
Minimum
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THE HELIOSPRERE IN 3-D
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THE END OF THE HELIOSPHERE
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Fermilab
LHC ? CERN
1part per Km2-century
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THE HELIOSPHERE
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COSMIC RAY TRANSPORT IN THE HELIOSPHERE (FOKKER-PL
ANCK)

• f(r, E, t). CR distribution function
• r position E Energy t time
• a) Convection and magnetic drift due to gradient
  and curvature
• of HMF
• b) Adiabatic cooling
• c) Diffusion (HMF irregularities)
• d) Additional sources (acc at Terminal Shock)

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Potgieter Ferreira(2004)
(Valdés-Galicia et al., 2005)

• (K?? , K? ) from numerical
• simulations
• Boundary at 90 AU

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Flares and Coronal Mass Ejections
15 Ene, 1996, LASCO-C3 en SOHO

• Flares are short duration solar explosions that
  emit in visible, UV, XRays, ? rays, energetic
  particles.
• CMEs are expulsions of great ammount of plasma
  generating shock waves.
• Flares and CMEs are quasi-simultaneous.

Bastille day flare July 14, 2000
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Solar Flare model
Masuda et al. 1994
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Evidence Positron anihilation e,
e- (0.511MeV) Neutron capture lines 1H(n,?)2H
(2.223 MeV) Gamma ray lines (nuclear
deexitation) 160(6.129 MeV) 12C(4.438MeV) Gamma
rays from ?o , ? decay (peak ?o at 70 MeV)
ENERGETIC PROTONS ? NUCLEAR REACTIONS IN FLARES
protons and electrons transport is governed by
electromagnetic fields in the Sun and
interplanetary medium. Neutrons Do Not ? they
preserve information from the acceleration site.
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EVENT ON 7 SEPTEMBER 2005
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SUMMARY

• GCR with E ?1011 eV are modulated by the solar
  activity (anticorrelation)
• GCR intensity has cycles of 11y (activity) and
  22y (magnetic)
• Solar modulation of GCR results from an interplay
  of
• DRIFT ? GRADIENT AND CURVATURE OF HMF
• DIFFUSION ? MAGNETIC TURBULENCE
• CONVECTION ? TURBULENCE IS CARRIED BY SOLAR WIND
• ADIABATIC DECELERATION ? SOLAR WIND EXPANSION
• Besides electromagnetic radiation, the Sun emmits
  energetic particles (ps, es, ?s, ns).
• Solar Neutrons preserve information of the
  acceleration site.

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CALL FOR PAPERS January 2007