Intrinsic chromospheric emission from Zeta Aurigae binaries

Details Intrinsic chromospheric emission from Zeta Aurigae binaries Intrinsic chromospheric emission from Zeta Aurigae binaries

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.258..473e&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 258, no. 3, p. 473-475.

Physics

5

B Stars, Chromosphere, Eclipsing Binary Stars, Emission Spectra, K Stars, Supergiant Stars, Dwarf Stars, Iron, Iue, Stellar Color, Stellar Spectra

Scientific paper

The question of whether the eclipses of Zeta Aur binaries reveal information about the chromospheres of single stars is addressed. It is concluded that Al II 2669 A, and the fluorescent iron lines, as well as CI II 2325 A are formed by the intrinsic thermal processes of the chromospheres of the K supergiant components of the Zeta Aur binaries. That these lines have roughly the same intensities as in single stars is a strong indication that the B components of Zeta Aur binaries do not alter the thermal physics of the chromosphere much, at least not in the bulk of the gas which forms the dominant chromospheric emission in normal stars.

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