Partition of Proton and Electron Heating in the Solar Wind (Invited)

Details Partition of Proton and Electron Heating in the Solar Wind (Invited) Partition of Proton and Electron Heating in the Solar Wind (Invited)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh41e..01v&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH41E-01

Astronomy and Astrophysics

Astrophysics

[7509] Solar Physics, Astrophysics, And Astronomy / Corona

Scientific paper

The electron and proton temperature profiles in the solar wind are very nonadiabatic so that additional heat deposition is needed for both species. A possible heating source is the Kolmogorov-like dissipation of the Alfvén waves. It is still an open issue how turbulence partitions the heat between the electrons and protons (see, e.g., Stawarz et al., 2009 and Breech et al., 2009). Comparison of empirical electron temperature, derived from differential emission measure tomography (DEMT) applied to STEREO A and B EUVI images, with numerical solar wind models allows us to constrain this heating partition. The DEMT results cover the height range 1.035 to 1.225 Rsun. The densities are compared to the solar rotational tomography on LASCO-C2 data of SOHO to further constrain the wind acceleration and heating models. We specifically analyze the periods of Carrington rotations 2077 and 2095. We use the recently developed three-dimensional two-temperature solar wind model within the Space Weather Modeling Framework (SWMF), which includes the anisotropic electron thermal heat conduction, and the collisional heat transfer between the electrons and protons. The solar wind is assumed to be accelerated by the Alfvén waves, and we use Kolmogorov dissipation of these waves to heat both the protons and electrons.

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