On the inability of magnetically constricted transition regions to account for the 10 to the 5th to 10 to the 6th K plasma in the quiet solar atmosphere

Details On the inability of magnetically constricted transition regions to account for the 10 to the 5th to 10 to the 6th K plasma in the quiet solar atmosphere On the inability of magnetically constricted transition regions to account for the 10 to the 5th to 10 to the 6th K plasma in the quiet solar atmosphere

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..112..255d&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 112, no. 2, 1987, p. 255-279.

Physics

27

Coronal Loops, Extreme Ultraviolet Radiation, Plasma Temperature, Solar Atmosphere, Solar Magnetic Field, Transition Points, Conductive Heat Transfer, Magnetic Flux, Stellar Models

Scientific paper

The authors re-examine static models of the atmosphere which incorporate not only conduction and radiation but also the effects of large magnetic constrictions. They find the structure of the plasma depends not only on the magnitude of the constriction but also on the tube's shape. The results show that no model with a constriction of order 100 can simultaneously (a) produce the variation of differential emission measure with temperature derived from measured line intensities and (b) satisfy the observed constraint (Reeves, 1976) that EUV emission from below ≈7×105K be confined to the supergranular network. This suggests that the bulk of the 105 - 106K plasma in the quiet solar atmosphere is magnetically isolated from the corona and heated internally. For any permitted tube shape, constriction factors of order 100 reduce the coronal conductive energy losses to the transition region to a value which is less than a third of the value for an unconstricted field.

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