Heating the Solar Wind Through Turbulence and Electron Heat Conduction Modelling

Details Heating the Solar Wind Through Turbulence and Electron Heat Conduction Modelling Heating the Solar Wind Through Turbulence and Electron Heat Conduction Modelling

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh41c..05b&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH41C-05

Mathematics

Logic

7859 Transport Processes, 7863 Turbulence (4490)

Scientific paper

We employ a turbulence transport model to explore the heating of the solar wind by turbulent dissipation, including, for the time, separate equations for heating of electrons and protons. Heating occurs through the deposition of internal energy from kinetic effects that terminate the MHD cascade at small scales. We utilize a simple transport model for three turbulence quantities -- the energy per unit mass, the cross helicity or Alfvénicity, and a similarity length scale. The model includes a von Karman -- Taylor phenomenological model for turbulent dissipation, which modifies the electron and proton temperatures. The involvement of the electron temperature raises several new and interesting issues; How should the electron heat flux be modeled? How long is the collision time between protons and electrons? How much turbulence dissipation goes into heating the electrons and how much goes into heating the protons? Using Voyager and Ulysses observational data, we begin to explore these issues. We find that the inclusion of electron conduction effects provides a more complete description of the solar wind plasma and may help explain the observed temperature profiles.

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