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COSMIC RAYS IN THE SOLAR ENVIRONMENT

COSMIC RAYS IN THE SOLAR ENVIRONMENT. José Fco. Valdés-Galicia Departamento de Investigaciones Solares y Planetarias Instituto de Geofísica Universidad Nacional Autónoma de México. THE HELIOSPHERE. A Bird´s eye view of the Solar Interior. SUNSPOTS. SOLAR TOTAL IRRADIANCE. Solar minimum.

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COSMIC RAYS IN THE SOLAR ENVIRONMENT

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  1. COSMIC RAYS INTHE SOLAR ENVIRONMENT José Fco. Valdés-Galicia Departamento de Investigaciones Solares y Planetarias Instituto de Geofísica Universidad Nacional Autónoma de México

  2. THE HELIOSPHERE

  3. A Bird´s eye view of the Solar Interior

  4. SUNSPOTS

  5. SOLAR TOTAL IRRADIANCE

  6. Solar minimum Solar maximum Xray images

  7. THE SOLAR CORONA 1973 1991 1994 1980 It must be very hot otherwise it wouldn´t be so extended

  8. SOLAR ATMOSPHERE TEMPERATURES

  9. THE “BALLERINA SKIRT”

  10. 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

  11. THE HELIOSPRERE IN 3-D

  12. THE END OF THE HELIOSPHERE

  13. Fermilab LHC  CERN 1part per Km2-century

  14. THE HELIOSPHERE

  15. COSMIC RAY TRANSPORT IN THE HELIOSPHERE (FOKKER-PLANCK) • 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)

  16. Potgieter & Ferreira(2004) (Valdés-Galicia et al., 2005) • (K , K ) from numerical • simulations • Boundary at 90 AU

  17. 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

  18. Solar Flare model Masuda et al. 1994

  19. 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.

  20. Solar Neutron Telescope World Network

  21. EVENT ON 7 SEPTEMBER 2005

  22. 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 (p´s, e´s, ´s, n´s). • Solar Neutrons preserve information of the acceleration site.

  23. http://www.icrc2007.unam.mx icrc2007@icrc2007.unam.mx CALL FOR PAPERS January 2007

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