On the magnetic structure of the quiet transition region

Details On the magnetic structure of the quiet transition region On the magnetic structure of the quiet transition region

May 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..105...35d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 105, May 1986, p. 35-45.

Physics

159

Chromosphere, Magnetic Field Configurations, Solar Corona, Solar Magnetic Field, Fine Structure, Lines Of Force, Transition

Scientific paper

Existing models of the quiet chromosphere-corona transition region predict a distribution of emission measure over temperature that agrees with observation for a T greater than about 100,000 K. These 'network' models assume that all magnetic field lines that emerge from the photosphere extend into and are in thermal contact with the corona. It is shown that the observed fine-scale structure of the photospheric magnetic network instead suggests a two-component picture in which magnetic funnels that open into the corona emerge from only a fraction of the network. The gas that makes up the hotter transition region is mostly contained within these funnels, as in standard models, but, because the funnels are more constricted in our picture, the heat flowing into the cooler transition region from the corona is reduced by up to an order of magnitude. The remainder of the network is occupied by a population of low-lying loops with lengths less than about 10,000 km. It is proposed that the cooler transition region is mainly located within such loops, which are magnetically insulated from the corona and must, therefore, be heated internally. The fine-scale structure of ultraviolet spectroheliograms is consistent with this proposal, and theoretical models of internally heated loops can explain the behavior of the emission measure below a T of aobut 100,000 K.

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