The Cepheid infrared period-luminosity relations

Details The Cepheid infrared period-luminosity relations The Cepheid infrared period-luminosity relations

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...348..673h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 348, Jan. 10, 1990, p. 673-681.

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Cepheid Variables, Infrared Spectra, Stellar Atmospheres, Stellar Luminosity, Distance, Periodic Variations, Stellar Magnitude

Scientific paper

The angular diameters of Cepheid variable stars derived by Hindsley and Bell (1989) are combined with model atmosphere calculations of infrared visual surface brightnesses to derive infrared light curves. While the shape of the light curves matches the observations very well, the calculated apparent magnitudes are about 0.1 mag too faint. Reasons for this discrepancy are given. The models predict that the brightest J magnitude occurs at about phase 0.1, while the brightest H and K occur at about phase 0.3, in agreement with observation. The Cepheid distances derived by Hindsley and Bell are used to obtain infrared period-luminosity relations, for the J, H, and K bands. These are compared with the results found by other authors. Mean colors are found as a function of phase and are used to convert the period, mean absolute visual magnitude relation to period, mean absolute infrared magnitude relations.

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