The Analysis of Solar Energetic Particles

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Vashenyuk et al. 200520 January, 2005
‣The response of a neutron monitor to anisotropic flux of solarprotons (Shea(& Smart, 1982):20 GV(∆N N / N) j = ΣRc(dN/N)JJ ⎜⎜⎜⎜ (R) S(R) F ( (θ j (R)) A(R) d Rwhereis an effect at a given neutron monitor jJ || (R)is rigidity spectrum of SEP flux in the direction ofanisotropy axisS(R) is specific yield function (Debrunner(et al., 1984),F ( (θ j (R)) is pitch-angle distribution of SEPsθ j is pitch angle (angle between the anisotropy axis givenby Φ; Λ and asymptotic direction of a given neutron monitorat a given rigidity R)= 1 for allowed and 0 for forbidden trajectoriesA(R) = 1
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 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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