Physics
Scientific paper
Mar 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990soph..126...69f&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 126, March 1990, p. 69-88.
Physics
19
Solar Magnetic Field, Solar Physics, Solar Temperature, Chromosphere, Helioseismology, Solar Corona, Solar Granulation
Scientific paper
Two-dimensional numerical models of the solar transition region are calculated using an inverse coordinates method which attains pressure equilibrium between the network magnetic field and the external comparatively field-free gas. The approach used (in which magnetic field lines become coordinate lines) simplifies the energy equation and free boundary problem. In order to examine the effects of self-consistent geometry on the thermal structure of the transition region network, four models are calculated, where the energy balance includes the effects of radiation, conduction, and enthalpy flux. It is confirmed that the lower branch of the emission measure curve cannot be explained within the single flux-tube model if the classical Spitzer thermal conductivity is used. However, by including a turbulent thermal conductivity as proposed by Cally (1990), transition region models are obtained for which the resulting emission measure curves exhibit the correct behavior, including the observed turn-up below about 200,000 K.
Cally Paul S.
Fiedler Russ A. S.
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