Solar 3He-rich events and energy spectra of particles accelerated in two stages

Details Solar 3He-rich events and energy spectra of particles accelerated in two stages Solar 3He-rich events and energy spectra of particles accelerated in two stages

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003jgra..108.1031z&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 108, Issue A1, pp. SSH 6-1, CiteID 1031, DOI 10.1029/2002JA009358

Astronomy and Astrophysics

Astrophysics

2

Solar Physics, Astrophysics, And Astronomy: Energetic Particles (2114), And Astronomy: Corona, And Astronomy: Flares, And Astronomy: Magnetic Fields, Magnetospheric Physics: Plasma Waves And Instabilities

Scientific paper

Energy spectra of solar 3He-rich events are theoretically and parametrically investigated according to the two-stage acceleration model, which was proposed by Zhang [1995, 1999], and self-consistently explained various aspects of acceleration and enhancement including electrons, 3He, and heavy ions. First, an expression for the energy spectra of energetic particles is derived from the two-stage acceleration model. Then, it is shown that all species of particles approximately have power law form spectra. The spectral index (denoted by γ) is determined by the exponent of power spectrum of magnetic fluctuations (ν). Given a spectral index that is consistent with observations, differential fluxes (or intensities) are plotted versus energies for electrons, 3He, and some typical heavy ions: carbon (C), oxygen (O), silicon (Si), and iron (Fe). The results obtained from this model very closely approximate measurements shown by Reames et al. [1985] and Mason et al. [1994]. Furthermore, the magnetic fluctuations and particle heating can significantly affect the differential fluxes of solar energetic particles and may cause the energy spectra to be complicated and different from event to event.

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