The Analysis of Solar Energetic Particles

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Timing <strong>of</strong> 20 Jan. 2005X7.1/2B, N12W58, AR 10720, 0636 – 0701 - 0726 UTSONG: gamma E>200-300 MeV 0645 – 0649 UTHX (RHESSI)max 0646±1 min0.8-7 MeV max 06474-7 MeV (incl.γ-lines) start 0644, max 0646Type II start 064415.4 GHz (n~3x10 12 cm -3 ) max 0644Relativistic protons arrived at the Earth at 0649 UTand peaked at 0654± 2 min
20 January, 2005, first arriving particles3.E+0559002.E+054900J(el),cm -2 s -1 sr -1 MeV -12.E+051.E+055.E+04390029001900900NM South Pole, %0.E+006 6.5 7 7.5 8U sw =800 km/s,L=1.05 AU20 Jan. 2005, UTEl, 175-315 keV, ACENM South Pole-100P,2 GeVβδT, , min0.95 9.2El,0.74250 keV 11.8
Page 1 and 2: WP13000: Solar Particle Emission An
Page 3 and 4: The Analysis of Solar Energetic Par
Page 5 and 6: Marisa Storini - IFSI/INAF Athens -
Page 13 and 14: Energy spectrum of solarcosmic rays
Page 15 and 16: Is it possible to make anyconclusio
Page 17 and 18: Energy spectrum in the maximum of t
Page 19 and 20: Acceleration mechanisms‣ Shock ac
Page 21 and 22: dJ22−(σ+2) /(σ−1)∝(E+2Em 0c
Page 23 and 24: Panel (a) shows superposed intensit
Page 25 and 26: Proton intensity is shown at the sh
Page 27 and 28: Left: Wind/EPACT hourly averaged ab
Page 29 and 30: Taken fromJ.-I. Sakai andC. de Jage
Page 31 and 32: Particle acceleration in the DC ele
Page 33 and 34: Fast-drift bursts (type III) can be
Page 35 and 36: GLE 20 January 2005Contribution at
Page 38 and 39: Vashenyuk et al. 200520 January, 20
Page 40 and 41: Direction to the sourceof solar pro
Page 42 and 43: 1.E+14Dif. spectra of protons20 Jan
Page 44 and 45: 20 January 2005.Numerical solutiono
Page 48 and 49: Gopalswamyet al. (29 th ICRC,)Left:
Page 50 and 51: Height, solar radii abovephotospher
Page 52 and 53: 20 January 2005. Resume II‣ SEPs
Page 54 and 55: CONCLUSION‣ Energy spectra of SEP

The Analysis of Solar Energetic Particles

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