Models for stellar coronae: Numerical methods and examples - Comparison with the minimum flux corona theory - Differences between hydrostatic and dynamic models

Details Models for stellar coronae: Numerical methods and examples - Comparison with the minimum flux corona theory - Differences between hydrostatic and dynamic models Models for stellar coronae: Numerical methods and examples - Comparison with the minimum flux corona theory - Differences between hydrostatic and dynamic models

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....98..230h&link_type=abstract

Astronomy and Astrophysics, vol. 98, no. 2, May 1981, p. 230-247.

Astronomy and Astrophysics

Astrophysics

27

Plasma Heating, Stellar Coronas, Stellar Models, Supergiant Stars, B Stars, Boundary Value Problems, Energy Transfer, O Stars, Stellar Mass Ejection

Scientific paper

A numerical method for the calculation of models of stellar coronae by the solution of the coupled equations of motion, continuity and energy balance is introduced. The method considers the equations as a two-boundary value problem, with the only free parameter being the flux of mechanical energy deep in the photosphere and the position of the transition region being determined by the solution. It is found that moderate fluxes of mechanical energy produce an extended solar type corona, while larger fluxes lead to a hydrostatic corona 0.03 stellar radii thick, which can partially account for observations of OB supergiants. Comparison of coronal models for a typical OB supergiant calculated using the iterative two-boundary value method and using the minimum flux corona theory applied to an isothermal spherically symmetric corona reveal that the minimum flux corona theory is consistent with a corona heated by a mechanism specified in detail, and may be used to predict to within 30% the mechanical energy flux at the transition region. Finally, dynamic and static stellar models are calculated for the same mechanical energy flux using the two-boundary values method to illustrate the importance of properly including energy losses due to mass flow beyond the temperature maximum, which is not done in the initial value problem.

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