Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...151...69h&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 151, no. 1, Oct. 1985, p. 69-78.
Astronomy and Astrophysics
Astrophysics
22
Faculae, Gas Heating, Magnetic Flux, Solar Atmosphere, Solar Magnetic Field, Solar Temperature, Gas Ionization, Magnetohydrodynamics, Radiative Heat Transfer, Solar Oscillations
Scientific paper
The idea that magnetic elements in the photosphere and lower chromosphere of the sun are heated by downflowing gas is quantitatively examined. The time-dependent hydromagnetic equations are solved numerically in the slender flux tube approximation. Viscous terms are retained, and the radiative exchange of heat between the flux tube and the ambient medium are included. Hydrogen ionization and its thermodynamic consequences are treated self-consistently. Starting from a state of hydrostatic and thermal equilibrium, the temporal response due to the onset of a downflow in the tube is studied. After a transient phase lasting a few minutes, a stationary state results that is substantially hotter than the ambient medium over a fairly large height range. Chapman's facular model can be reproduced remarkably well by adjusting the mass flux entering the tube at the upper boundary. The results are comparatively insensitive to viscosity (nu less than or equal to 10 to the 12th sq cm/s), while radiative heat exchange is significant. Some observational implications are discussed, and it is suggested that the necessary mass flux could be provided by overstable oscillations during their downflow phase.
Hasan Sirajul S.
Schuessler Manfred
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