The acceleration and heating of the solar wind have been studied for decades using satellite observations and models. However, the exact mechanism that leads to solar wind heating and acceleration is poorly understood. In order to improve the understanding of the physical mechanisms that are involved in these processes a combination of modeling and observational analysis is required. Recent models constrained by satellite observations show that wave heating in the low-frequency (MHD), and high-frequency (ion-cyclotron) range may provide the necessary momentum and heat input to coronal plasma and produce the solar wind. This review is focused on the results of several recent solar modeling studies that include waves explicitly in the MHD and the kinetic regime. The current status of the understanding of the solar wind acceleration and heating by waves is reviewed.
Keywords: Multi-fluid models, MHD models, Waves, Solar wind, Hybrid models
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Since a Living Reviews in Solar Physics article may evolve over time, please cite the access <date>, which uniquely identifies the version of the article you are referring to:
"Wave Modeling of the Solar Wind",
Living Rev. Solar Phys. 7, (2010), 4. URL (cited on <date>):
|Title||Wave Modeling of the Solar Wind|
|Date||accepted 9 September 2010, published 15 October 2010|
|Date||accepted 28 November 2013, published 28 November 2013|
|Changes||Minor revision to add recent studies (26 new references and 3 figures).
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