Chromosphere-corona transition region models with magnetic field and fluid flow

Details Chromosphere-corona transition region models with magnetic field and fluid flow Chromosphere-corona transition region models with magnetic field and fluid flow

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...249..340a&link_type=abstract

Astrophysical Journal, Part 1, vol. 249, Oct. 1, 1981, p. 340-348.

Astronomy and Astrophysics

Astrophysics

72

Atmospheric Heat Budget, Chromosphere, Magnetohydrodynamic Flow, Solar Atmosphere, Solar Corona, Solar Magnetic Field, Atmospheric Heating, Conductive Heat Transfer, Coronal Holes, Magnetic Field Configurations, Radiative Heat Transfer, Solar Temperature, Transition

Scientific paper

Energy balance models of the chromosphere-corona transition region are computed for a segment of average sun network using assumed magnetic field geometry. The energy fluxes considered include radiation, conduction, enthalpy, and gravitational potential energy, but do not include mechanical heating. Two classes of models are considered: conduction driven and flow driven. In the former class, the thermal conductive flux vanishes at the base of the transition region, and in the latter class the thermal conductive flux increases with depth or remains constant. The conduction driven models require primarily outflow, whereas the flow driven models require downflow. Flow-driven models give best overall agreement with observations for T between 300,000 and 1,000,000 K, but neither class of models is satisfactory for T less than 100,000 K. It is concluded however, that the flow-driven models have ample energy supply even in the low transition region, and there is no apparent need for additional energy sources.

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