Analyses of archival data for cool dwarfs. 1: The solar B-V problem reconsidered

Details Analyses of archival data for cool dwarfs. 1: The solar B-V problem reconsidered Analyses of archival data for cool dwarfs. 1: The solar B-V problem reconsidered

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasp..106..444t&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 106, no. 699, p. 444-451

Astronomy and Astrophysics

Astronomy

26

Astronomical Models, Balmer Series, Calibrating, Cool Stars, Dwarf Stars, H Alpha Line, H Beta Line, Solar Spectra, Stellar Color, Astronomical Spectroscopy, Color-Color Diagram, Gravitational Effects, Mathematical Models, Metallicity, Spectral Bands

Scientific paper

In a previous paper, Taylor has found that the solar value of (R-I)c is 0.337 +/- 0.0024 mag. This result can be converted to a value of solar (B-V) by combining it with blanketing corrections and a Hyades color-color relation. The latter are derived and discussed in this paper. The resulting value of solar (B-V) turns out ot be 0.633 +/- 0.009 mag. Annoyingly, this datum differs from the mean of a number of previous results at better than 99.5% confidence. A survey of the problem reveals a wavelength boundary: hydrogen beta and hydrogen alpha yield the result quoted above, while spectroscopy at wavelengths shortward of hydrogen beta yields an average value of solar (B-V) = 0.665 +/- 0.003 mag. The Balmer-line derivations are largely blanketing insensitive, so for the present, it seems defensible to assume that the Balmer-line result is correct and that its short-wavelength counterparts are affected by some unknown property of the solar blanketing.

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