Background Spectra and Velocity Dispersion of Solar Energetic Particles

Details Background Spectra and Velocity Dispersion of Solar Energetic Particles Background Spectra and Velocity Dispersion of Solar Energetic Particles

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh33b..01v&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH33B-01

Physics

7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration

Scientific paper

Solar Energetic Particle event onset times have been traditionally studied by using the velocity dispersion analysis. Those studies often report non-nominal path lengths for the first observed particles. The derived apparent path lengths can vary between 0.5 AU and 3 AU, while the distribution tends to peak at the nominal range of the expected path lengths (1-1.5 AU, spacecraft at 1 AU). Unlike the traditional studies, the recently introduced simulation approach to the onset research takes into account the effect of the interplanetary scattering on the arrival time of the first particles. These studies have shown that scattering can easily explain the large apparent path lengths. So far, the main focus of the simulation studies has been in the particle transport. In this study, we focus on the effect of the background spectrum to the observed velocity dispersion. This is achieved by overlaying a simulated event on backgrounds of different spectral shapes and relative intensities, emulating various onset conditions. The validity of the traditional onset analysis in various backgrounds is discussed.

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