Theoretical luminosity functions of red and black dwarfs

Astronomy and Astrophysics – Astronomy

Scientific paper

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Dwarf Stars, Stellar Evolution, Stellar Luminosity, Stellar Mass, Stellar Spectrophotometry, Electron Gas, Infrared Astronomy, Mass Spectra, Spaceborne Telescopes, Spectral Energy Distribution

Scientific paper

Theoretical luminosity functions of low-mass stars are calculated in several photometric passbands at both visual and infrared wavelengths. The calculations are based on the concept that stars are born throughout the life of the galaxy with a power-law mass spectrum down to masses of order 0.01 solar mass. Stars in which the ratio of the mass to the solar mass is in the range 0.085-0.5 (red dwarfs) first contract along their Hayashi tracks and then settle down on the main sequence. Stars with masses smaller than 0.085 solar mass (black dwarfs) are not capable of igniting the hydrogen in their cores but continue to contract along their Hayashi tracks until the electron gas in their interior becomes completely degenerate. The results are used to predict the number of black dwarfs that should be observable with future space telescopes. They are also used to derive mass-to-light ratios in different photometric passbands, which can be used to predict the surface brightness of the halos of external galaxies at visual and infrared wavelengths.

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