High resolution EUV spectroscopy of 56 Pegasi (KO 2p + wd)

Details High resolution EUV spectroscopy of 56 Pegasi (KO 2p + wd) High resolution EUV spectroscopy of 56 Pegasi (KO 2p + wd)

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982esasp.176..161j&link_type=abstract

In ESA 3rd European IUE Conf. p 161-164 (SEE N83-11889 02-88)

Computer Science

2

Extreme Ultraviolet Radiation, Giant Stars, Late Stars, Stellar Radiation, Ultraviolet Spectroscopy, Chromosphere, Iue, Resonance Lines, Stellar Coronas, Stellar Luminosity, Stellar Structure, Stellar Winds

Scientific paper

The hypothesis that X-ray and UV emission by 56 Pegasi (K0II p + wd) originates in a conventional chromosphere, transition region and corona, as opposed to Schindler's hypothesis of accretion of the cool stellar wind onto the white dwarf companion, is discussed. Analysis of IUE data indicates that within the uncertainties associated with determining the stellar radius and abundances, the chromosphere, transition region, and corona of 56 Peg are similar to that of Beta Draconis both in structure and energy balance. The accretion hypothesis is not a unique explanation of the observed spectral properties and the white dwarf companion may not play a direct role. Furthermore, 56 Peg, according to current values of V-R and luminosity class, is on the nonsolar side of the Linsky-Haisch dividing line whereas Beta Draconis is on the solar side.

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