Solar near-relativistic electron observations as a proof of a back-scatter region beyond 1 AU during the 2000 February 18 event

Details Solar near-relativistic electron observations as a proof of a back-scatter region beyond 1 AU during the 2000 February 18 event Solar near-relativistic electron observations as a proof of a back-scatter region beyond 1 AU during the 2000 February 18 event

Sep 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...519a..36a&link_type=abstract

Astronomy and Astrophysics, Volume 519, id.A36

Astronomy and Astrophysics

Astrophysics

2

Sun: Particle Emission, Sun: Flares, Sun: Coronal Mass Ejections (Cmes), Interplanetary Medium

Scientific paper

Aims: We study the near-relativistic (NR; >30 keV) electron event observed on 2000 February 18 by near-Earth spacecraft. Previous works have explained this event by assuming that the propagation of NR electrons is essentially “scatter-free” at heliocentric radial distances r < 1 AU, and that beyond 1 AU particles are “back-scattered” by magnetic field irregularities. Methods: Our aim is to re-visit this interplanetary propagation scenario and infer the injection profile at the Sun by fitting the electron directional intensities observed by the Advanced Composition Explorer. Results: We use a Monte Carlo transport model to explore this approach. We assume that the interplanetary magnetic field is an Archimedean spiral and that the interplanetary transport of NR electrons is characterized by a large radial mean free path (λ_r > 0.5 AU) and anisotropic pitch-angle scattering for r <1 AU, and a small radial mean free path (λ_r < 0.5 AU) and isotropic scattering in the back-scatter region. Conclusions: The event cannot be explained without assuming a back-scatter region beyond 1 AU. The best fit is obtained by assuming λ_r = 3.2 AU in the inner heliosphere and a back-scatter region characterized by a small mean free path λr = 0.2 AU located beyond 1.2 AU.

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