Generation and propagation of solar disturbances: a magnetohydrodynamic simulation
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 discussio...
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| Published in | Journal of atmospheric and solar-terrestrial physics Vol. 61; no. 1; pp. 109 - 117 |
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| Main Authors | , |
| Format | Journal Article |
| Language | English |
| Published |
Elsevier Ltd
1999
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| Online Access | Get full text |
| ISSN | 1364-6826 1879-1824 |
| DOI | 10.1016/S1364-6826(98)00121-7 |
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| Summary: | 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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| Bibliography: | ObjectType-Article-2 SourceType-Scholarly Journals-1 ObjectType-Feature-1 content type line 23 SourceType-Scholarly Journals-2 ObjectType-Feature-2 ObjectType-Conference Paper-1 SourceType-Conference Papers & Proceedings-1 ObjectType-Article-3 |
| ISSN: | 1364-6826 1879-1824 |
| DOI: | 10.1016/S1364-6826(98)00121-7 |