Heat transfer in the corona and transition region

Details Heat transfer in the corona and transition region Heat transfer in the corona and transition region

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975soph...44..315g&link_type=abstract

Solar Physics, vol. 44, Oct. 1975, p. 315-329.

Physics

3

Atmospheric Models, Chromosphere, Heat Transfer, Solar Atmosphere, Solar Corona, Astronomical Models, Atmospheric Heat Budget, Solar Magnetic Field, Solar Physics, Solar Prominences, Temperature Distribution

Scientific paper

The temperature distribution in the solar corona in quiet regions where the magnetic field is closed and in the chromosphere-corona transition region is analyzed on the basis of a static model of heat transfer in closed magnetic flux tubes. In this model, all the generated heat is radiated away, although conduction transfers much of the heat to the transition region prior to emission. It is shown that the rate of conductive transfer depends on the cross section of the flux tube as it passes through the chromosphere and transition region, and that only the heating per unit area of the sun's surface is needed to establish conditions in the corona and transition region. For the observed heating rate, coronal and transition-region densities, emissions, and EUV radiation distributions are computed and found to agree closely with observations. Optimum maximum temperatures are obtained when heating is concentrated in the highest regions of the flux tubes. It is noted that the equation of heat balance has some solutions where temperature oscillates with distance; these do not apply to the normal corona, but may be relevant to prominences.

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