Models for stellar coronae - The effects of coronal heating with long dissipation scale lengths

Details Models for stellar coronae - The effects of coronal heating with long dissipation scale lengths Models for stellar coronae - The effects of coronal heating with long dissipation scale lengths

Dec 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...116..296h&link_type=abstract

Astronomy and Astrophysics, vol. 116, no. 2, Dec. 1982, p. 296-302.

Astronomy and Astrophysics

Astrophysics

5

Heat Transfer, Stellar Coronas, Stellar Evolution, Stellar Models, Coronal Holes, Energy Dissipation, Solar Corona, Stellar Mass Ejection

Scientific paper

Calculations of coronal models with different dissipation scale lengths show that for the same flux of mechanical energy through the transition region longer dissipation scale lengths give a corona with a large coronal maximum temperature, which occurs further from the photosphere. The mass loss is substantially increased when the pressure of the transition region is decreased. When the dissipation scale length becomes very long the maximum coronal temperature and the mass loss decrease, but the maximum coronal temperature occurs at still greater distances from the photosphere. The increase in mass loss obtained with a longer dissipation scale length signifies that a greater fraction of the energy heating the corona goes into maintaining the stellar wind. It appears that heating in coronal holes beyond the base could explain the enhanced mass flux and the velocity measured in the high-speed streams of the solar wind. A comparison of the coronal models with different dissipation length scales with the predictions of the minimum flux corona theory shows that the predictions are good only if the heating of the corona occurs at its base.

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