The white-dwarf color-luminosity relation and its intrinsic width

Details The white-dwarf color-luminosity relation and its intrinsic width The white-dwarf color-luminosity relation and its intrinsic width

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985pasp...97..827g&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 97, Sept. 1985, p. 827-834.

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13

Hertzsprung-Russell Diagram, Stellar Color, Stellar Luminosity, Stellar Parallax, White Dwarf Stars, Astrometry, Error Analysis, Radii, Star Distribution

Scientific paper

The high quality of the United States Naval Observatory trigonometric parallaxes, and the unique temperature-color relation found for multichannel spectrophotometry permit a detailed reexamination of the relation between color and luminosity, and therefore radius, for white dwarfs. The mean white-dwarf radius is 0.0124 R_sun;, based on theoretical fluxes from hydrogen model atmospheres. The cosmic scatter is about 12% in radius, appreciably less than found in other studies, but it is not zero. The scatter is close to that derived by Koester and Weidemann from surface gravities determined from the Balmer jump in hydrogen atmospheres at log g = 8. The masses lie within the range 0.47 to 0.71 M_sun;. The single definitely overluminous white dwarf is EG 11 (0135-05).

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