The transition region structure of Kappa Ceti

Details The transition region structure of Kappa Ceti The transition region structure of Kappa Ceti

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....99..141f&link_type=abstract

Astronomy and Astrophysics, vol. 99, no. 1, June 1981, p. 141-143.

Astronomy and Astrophysics

Astrophysics

4

Chromosphere, Dwarf Stars, Stellar Atmospheres, Stellar Spectra, Ultraviolet Spectra, Atmospheric Heat Budget, Emission Spectra, Iue, Line Spectra, Stellar Coronas

Scientific paper

Ultraviolet emission lines of Kappa Ceti (HD 20630), obtained with the IUE satellite, are analyzed in order to study the higher chromospheric, transition region and the low corona structure. Three models are derived for the emission measurement distribution, and the best fit model has a pressure of log Pe equals 14.96 at log Te equals 5.2, since the pressure-temperature distribution is more linear and the region height is approximately 800 km, which is consistent with the assumptions made initially. The energy balance shows that the transport of energy by conduction is negligible when compared with the radiation losses, which, at all heights, are greater than those from the sun.

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