Statistics – Computation
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640718o&link_type=abstract
American Astronomical Society, AAS Meeting #216, #407.18; Bulletin of the American Astronomical Society, Vol. 41, p.862
Statistics
Computation
Scientific paper
Turbulent MHD waves have been suggested as a possible mechanism to heat and accelerate the plasma in the solar corona and solar wind. Heating is achieved by wave energy dissipation and acceleration is due to the wave pressure gradient force. Here we present a self-consistent model describing these processes, which is based on a wave transport equation for low frequency Alfven waves coupled to the 3D MHD equations (Sokolov et. al. 2009). This allows the exchange of momentum and energy between the wave field and the background plasma. In a recently developed computational model, the coupled system of wave transport equation and the MHD equations is solved. The coupling is achieved by constructing a frequency grid in each spatial cell, allowing the detailed description of the wave energy spectral evolution, making the model effectively 4D. The model is based on an existing global solar corona model (Cohen et. al. 2005). In this work we examined the possible effects of Alfven wave turbulence by imposing inner boundary conditions for the wave energy spectral density by assuming a Kolmogorov - type frequency dependence, and a surface distribution derived from observable quantities. We found that Alfven wave pressure is sufficient to drive the solar wind. Different assumptions regarding the total wave energy at the surface are discussed and compared.
der Holst Bart van
for Space Environment Modeling Center
Gombosi Tamas I.
Manchester Ward B.
Oran Rona
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