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Wave Modeling of the Solar Wind

Leon Ofman 
Catholic University of America
NASA Goddard Space Flight Center
Code 671
Greenbelt, MD 20771, U.S.A.

'External link'http://solar.cua.edu
This article has been revised on 28 November 2013 (see changes in detail).

Abstract

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: Solar wind, Waves, MHD models, Multi-fluid models, Hybrid models

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