Generation and propagation of solar disturbances: a magnetohydrodynamic simulation

Details Generation and propagation of solar disturbances: a magnetohydrodynamic simulation Generation and propagation of solar disturbances: a magnetohydrodynamic simulation

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999jastp..61..109w&link_type=abstract

Journal of Atmospheric and Solar-Terrestrial Physics, Volume 61, Issue 1-2, p. 109-117.

Physics

Scientific paper

It has been recognized that there are three basic physical agents, namely (i) electromagnetic radiation, (ii) high-energy charged particles, and (iii) enhanced solar wind, resulting from solar activity, which affect the near-Earth and terrestrial environment. In this paper, we restrict our discussion to the subject of the enhanced solar wind. In this context, it is well-known that the most appropriate tool to investigate the generation and propagation of solar disturbances is magnetohydrodynamic (MHD) theory. The most recent progress during the period of the Solar Terrestrial Energy Program (STEP) in these aspects will be presented. In particular, the induced transport of momentum and energy, by coronal mass ejections (CMEs), from the solar surface to the Earths environment (i.e. at 1 AU) will be illustrated by using a self-consistent MHD model of streamer and flux-rope interactions.

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