Energy balance of stellar coronae. I. Methods and examples

Journal Article · Sun Aug 15 04:00:00 EDT 1982 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160213· OSTI ID:6699246

Hammer, R

Simplified theoretical models of open regions in hot stellar coronae are considered. The energy balance is described by thermal conduction, optically thin radiation, stellar wind, and mechanical heating. In order to avoid unnecessary free parameters, such models should fulfill appropriate boundary conditions at the base of the atmosphere, at the critical point, and at infinity. Then, in the simplest case, they are determined by four parameters; namely, by the stellar mass and radius and by the amount and location of coronal heating. The dependence of the models on the boundary conditions is investigated. In particular, it is shown that the boundary condition which restricts the temperature at infinity can often be replaced by a relation at the critical point. This leads to a new, efficient method for solving the boundary value problem. Several examples of solutions are presented, and the energy balance is discussed as a function of height.

• Research Organization: Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, and Institut fuer Astronomie und Astrophysik der Universitaet Wuezburg, FRG
• OSTI ID: 6699246
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 259:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
BOUNDARY CONDITIONS
BOUNDARY-VALUE PROBLEMS
ENERGY BALANCE
ENERGY TRANSFER
HEAT TRANSFER
MATHEMATICAL MODELS
STAR MODELS
STELLAR ATMOSPHERES
STELLAR RADIATION
STELLAR WINDS
THERMAL CONDUCTION