Journal
ASTROPHYSICAL JOURNAL
Volume 784, Issue 2, Pages -Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/784/2/120
Keywords
magnetohydrodynamics (MHD); solar wind; turbulence; waves
Categories
Funding
- NASA's LWS TR&T and HTP programs
- Center for Integrated Space Weather Modeling
- NASA Solar Probe Plus Observatory Scientist contract
- Texas Advanced Computing Center (TACC) in Austin
- NASA Advanced Supercomputing Division (NAS) at Ames Research Center
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Although the mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still being actively investigated, it is largely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process. Verdini et al. presented a model for heating and accelerating the solar wind based on the turbulent dissipation of Alfven waves. We first use a time-dependent model of the solar wind to reproduce one of Verdini et al.'s solutions; then, we extend its application to the case where the energy equation includes thermal conduction and radiation losses, and the upper chromosphere is part of the computational domain. Using this model, we explore the parameter space and describe the characteristics of a fast solar wind solution. We discuss how this formulation may be applied to a three-dimensional MHD model of the corona and solar wind.
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