The Analysis of Solar Energetic Particles

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<strong>The</strong> spectral kneeEllison andRamaty, , 1985:spectrum turnover may resultsfrom adiabaticdeceleration inthe expandingblast wave, shocklifetimescomparable toparticleacceleration time,shock sizecomparable toparticle diffusionlengthLeft: A spectrum from spacecraft and the neutron monitor network in the 29September 1989 event with Eo = 1 GeV. Right: spectra from the 20 April 1998event with Eo = 15 MeV. (Reames, 2000). Proton intensities below ~50 MeV aresimilar in the both events.
Left: Wind/EPACT hourly averaged abundance ratios normalized toreference coronal values, during 20.04.1998 event [Reames[Reames, , 1995].Right: Simulation <strong>of</strong> these abundances [Ng et al., 1999]D. V. Reames, 2000.
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: Proton intensity is shown at the sh
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 46 and 47: Timing of 20 Jan. 2005X7.1/2B, N12W
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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