Abstract
The heating mechanism of the Sun's corona is of central importance in Solar Physics research. In this paper it is assumed that the heat is deposited in a regular time dependent manner and the temperature, density and pressure variations as well as the plasma flows created, are investigated. It is assumed that the magnetic field is strong, so that the dynamics reduce to a one dimensional problem along the field. In addition, if the radiative time in the corona is much longer than the sound travel time then the plasma evolves isobarically. The variations of the frequency of the time-dependent heating supply are investigated and a critical value is found above which a hot corona can be maintained and below which the plasma temperature cools to chromospheric values. The implications of time-dependent heating upon the forthcoming SOHO observations are also discussed.
Original language | English |
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Pages (from-to) | 181-186 |
Number of pages | 6 |
Journal | Astrophysical Letters and Communications |
Volume | 34 |
Issue number | 1-6 |
Publication status | Published - 1 Dec 1996 |