Effect of improved H(-) opacity on the infrared flux method temperature scale and derived angular diameters - Use of a self-consistent calibration

Details Effect of improved H(-) opacity on the infrared flux method temperature scale and derived angular diameters - Use of a self-consistent calibration Effect of improved H(-) opacity on the infrared flux method temperature scale and derived angular diameters - Use of a self-consistent calibration

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...245..567b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 245, no. 2, May 1991, p. 567-574.

Astronomy and Astrophysics

Astrophysics

84

Cool Stars, Infrared Stars, Stellar Temperature, Diameters, Hydrogen Clouds, Opacity, Stellar Atmospheres

Scientific paper

The present study uses the infrared flux method (IRFM) to derive the stellar temperatures and angular diameters derived by Blackwell et al. (1990). The more accurate calculations of the H(-) opacity recommended by John (1988) are applied. A Vega self-consistent infrared calibration is derived using the IRFM. Relations are given to allow temperatures to be derived from measurements of V-K and B-V. The original temperatures are increased by up to 1.3 percent, and the angular diameters are decreased by up to 2.7 percent. The effect of uncertainties in the H(-) opacity and convection on determined values of angular diameter and Te is assessed. The chief remaining uncertainty arises from the absence of a well-established infrared calibration for Vega.

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