Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11b1654a&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #SH11B-1654
Astronomy and Astrophysics
Astrophysics
[7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles
Scientific paper
The solar wind electrons are characterized by a superposition of three distinctive populations namely, core, halo, and strahl components. The core represents a thermal component which is usually characterized by a Maxwellian-like distribution. However, the halo sometimes departs from isotropy or builds a suprathermal extension becoming a non-thermal population; whereas the strahl is always observed as a field-aligned, streaming non-thermal component which departs drastically from a Maxwellian-like distribution. We have recently began to study the evolution of the electron distribution function in the solar corona and the solar wind using a modified version of the existing Fokker-Planck code. Our version of the code has a 1D spatial dependence (along the background magnetic field) and a 2D velocity dependence (in v-parallel and v-perpendicular) that includes the mirror-force due the spatial inhomogeneity of the background magnetic field (using the Parker-spiral field), and also including the quasilinear diffusion in velocity space due to wave-particle interaction of these electrons with whistler turbulence in the solar wind. Our final goal is to be able to use in-situ modeling of local observed distributions at 1AU as a boundary condition (from Cluster or Wind, which Dr. Vinas will provide as a CoI in both missions) and some modeling which include the collisional effects in the lower regions of the solar corona to investigate in full the spatial-temporal and velocity evolution of the electron distributions by integrating backward to the Sun. Such prediction capabilities will be usefull to predict the kind of distribution functions that Solar Probe Plus will detect at 9.5Ro from the Sun. We hope that the results we obtain from this study will shed some light into what are the mechanism that regulate and shape the electron velocity distributions in the solar wind and solar corona.
Airapetian Vladimir
Viñas Adolfo F.
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