PLASMA FLOWS DUE TO TIME-DEPENDENT HEATING OF THE SOLAR CORONA

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 d eposited in a regular time dependent manner and the temperature, densi ty and pressure variations 85 well as the plasma flows created, are in vestigated. It is assumed that the magnetic field is strong, so that t he dynamics reduce to a one dimensional problem along the field. In ad dition, if the radiative time in the corona is much longer than the so und travel time then the plasma evolves isobarically. The variations o f the frequency of the time-dependent heating supply are investigated and a critical value is found above which a hot corona can be maintain ed and below which the plasma temperature cools to chromospheric value s. The implications of time-dependent heating upon the forthcoming SOH O observations are also discussed.