| タイトル | Heating of the stellar corona |
| 本文（外部サイト） | http://hdl.handle.net/2060/19870011440 |
| 著者（英） | Parker, E. N. |
| 著者所属（英） | Chicago Univ. |
| 発行日 | 1986-12-01 |
| 言語 | eng |
| 内容記述 | The present state of development of the theory of coronal heating is summarized. Coronal heating is the general cause of stellar X-ray emission, and it is also the cause of stellar mass loss in most stars. Hence a quantitive theory of coronal heating is an essential part of X-ray astronomy, and the development of a correct theory of coronal heating should be a primary concern of X-ray astronomers. The magnetohydrodynamical effects involved in coronal heating are not without interest in their own right, representing phenomena largely unknown in the terrestrial laboratory. Until these effects can be evaluated and assembled into a comprehensive theory of coronal heating for at least one star, the interpretation of the X-ray emissions of all stars is a phenomenological study at best, based on arbitrary organization and display of X-ray luminosity against bolometric luminosity, rotation rate, etc. The sun provides the one opportunity to pursue the exotic physical effects that combine to heat a stellar corona. |
| NASA分類 | SOLAR PHYSICS |
| レポートNO | 87N20873 |
| 権利 | No Copyright |
| URI | https://repository.exst.jaxa.jp/dspace/handle/a-is/151164 |
|
