The cooling of carbon-oxygen white dwarfs

Details The cooling of carbon-oxygen white dwarfs The cooling of carbon-oxygen white dwarfs

Sep 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....51..383s&link_type=abstract

Astronomy and Astrophysics, vol. 51, no. 3, Sept. 1976, p. 383-391.

Astronomy and Astrophysics

Astrophysics

51

Cooling, Stellar Evolution, Stellar Temperature, White Dwarf Stars, Crystallization, Latent Heat, Opacity, Stellar Luminosity, Stellar Mass, Stellar Models

Scientific paper

The cooling of 0.6-solar-mass white dwarfs composed of 50% C-12 and 50% O-16 by mass is calculated. The equation of state includes a detailed description of crystallization. The initial models are before the Harman-Seaton (1964) cooling sequence, and the final models have luminosities below one hundred-thousandth that of the sun. The observational effects of crystallization and latent heat of melting are found to be negligible. Debye cooling does not become effective for luminosities greater than one hundred-thousandth that of the sun and hence should not be observed. No paucity of cold white dwarfs is expected. The cooling curve is found to be insensitive to the opacity law.

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