Electron and proton heating by solar wind turbulence
By Ben Breech, William H. Matthaeus, S. Cranmer, J. Kasper, S. Oughton. 2009
156 citations recorded by the source corpus.
[1] Previous formulations of heating and transport associated with strong magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electrons and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both electrons and protons and is exchanged between them via collisions. Comparison to available Ulysses data shows that a reasonable accounting for the data is provided when (1) the energy exchange timescale is very long and (2) the deposition of heat due to turbulence is divided, with 60% going to proton heating and 40% into electron heating. Heat conduction, determined here by an empirical fit, plays a major role in describing the electron data.
Subfields: Astronomy and Astrophysics, Molecular Biology
View Paper: https://www.semanticscholar.org/paper/4cb86bac6dbf3d850cefb5606662baef6182f304
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In Astronomy and Astrophysics
- A. A. Ballegooijen
- S. Cranmer
- S. Saar
- E. DeLuca
- Mahboubeh Asgari-Targhi
- G. Aulanier
- S. Gibson
- Eckart Marsch
In Molecular Biology
Citations in the corpus
- HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, methodology): “For the reference modelq≈ 0.3 in the corona (solidcurve), similar to the value of 0.5 used by Breech et al. (2009) in their model of the solar wind.”
- TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, methodology): “We also setα0 = 0.5 based on the turbulent transport models of Breech et al. (2009).”