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Temperature Structure of the Chromosphere-Corona Transition Region

Published online by Cambridge University Press:  12 April 2016

G. Elwert  and
P. K. Raju
G. Elwert
Affiliation:
Lehrstuhl für Theoretische Astrophysik, Tübingen, Germany
P. K. Raju
Affiliation:
Lehrstuhl für Theoretische Astrophysik, Tübingen, Germany

Extract

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Starting from the formula for line intensities E for a spherically symmetric atmosphere, considering the pressure parameter P0 = NeTe to be constant the inverse temperature gradient can be determined by taking it out from the integral for E. In this way Dupree and Goldberg (1967) found that the temperature gradient varies considerably whereas the conductive flux factor F=Te5/2(dTe/dh) is nearly constant for Te above 105 K. The best fit was obtained by using photospheric abundances. As the inverse temperature gradient varies considerably in the line forming region, it is, however, not satisfactory to take it out from the integral.

Type
Section IV / The Solar Soft X-Ray Spectrum
Information
International Astronomical Union Colloquium , Volume 14: Special Issue: Ultraviolet and X-Ray Spectroscopy of Astrophysical and Laboratory Plasmas , November 1972 , pp. 670 - 671
Copyright
Copyright © Reidel 1972

References

Dupree, A. K. and Goldberg, L.: 1967, Solar Phys. 1, 229.CrossRefGoogle Scholar
Jordan, C.: 1969, Monthly Noties Roy. Astron. Soc. 142, 499.Google Scholar