HR: 0800h
AN: SH51B-04    [Abstracts]
TI: Solar Particle Source Energy spectrum: Stochastic acceleration vs Neutral Current Sheet acceleration vs Shock Wave acceleration
AU: * PEREZ-PERAZA, J A
EM: perperaz@geofisica.unam.mx
AF: INSTITUTO DE GEOFISICA, UNAM, CIUDAD UNIVERSITARIA, COYOACAN, MEXICO, D.F 04510, Mexico
AU: GALLEGOS-CRUZ, A
EM: apoloniogallegos@yahoo.com.mx
AF: UPIICSA, I.P.N., Depto. de Ciencias Básicas, Té 950, Iztacalco, MEXICO, DF 08400, Mexico
AU: VASHENYUK, E V
EM: vashenyuk@pgi.kolsac.net.ru
AF: Polar Geophysical Institute, Apatity, Murmansk Region, 184209, Russian Federation
AU: MIROSHNICHENKO, L I
EM: leont1937@yahoo.com
AF: INSTITUTO DE GEOFISICA, UNAM, CIUDAD UNIVERSITARIA, COYOACAN, MEXICO, D.F 04510, Mexico
AB: It has been shown in a series of works that some solar particle events (SPE) are composed of two different relativistic populations, a Prompt Component (PC) and a Delayed Component (DC), each one with different energy spectrum behavior. The source spectra of the DC tend to be an inverse power law at the steady state situation, whereas the spectra of the PC are considerable deviated from such a power law. Here we attempt to reproduce the observational spectra of the PC and the DC on terms of different scenarios: (i) DC acceleration from magnetic merging in a Magnetic Neutral Current Sheet (MNCS). (ii) Stochastic acceleration of an injected population pre-accelerated in a MNCS. (iii) Stochastic acceleration with monoenergetic injection. (iv) Stochastic acceleration with monoenergetic injection, while undergoing adiabatic deceleration. We contrast our results with those assuming Shock Wave Acceleration. Results are illustrated for the case of the September 29, 1989, July 14, 2000, October 28, 2003 and January 20, 2005 Ground Level Events (GLE`s).
DE: 2114 Energetic particles (7514)
DE: 7514 Energetic particles (2114)
DE: 7845 Particle acceleration
DE: 7857 Stochastic phenomena (3235, 3265, 4475)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Joint Assembly