Theoretical luminosity functions for halo white dwarfs

Details Theoretical luminosity functions for halo white dwarfs Theoretical luminosity functions for halo white dwarfs

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...233..456m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 233, no. 2, July 1990, p. 456-461. Research supported by CICYT.

Astronomy and Astrophysics

Astrophysics

12

Halos, Star Formation, Stellar Luminosity, White Dwarf Stars, Astronomical Models, Charge Coupled Devices, Stellar Evolution

Scientific paper

Theoretical luminosity functions for halo white dwarfs are computed in order to interpret the recent observations by Liebert et al. (1989) of white dwarfs with large tangential velocities. If the halo is assumed to have been made by a burst of star formation, the white dwarf luminosity function has an extremely sharp peak, which becomes a broad maximum when averaged in bins of one bolometric magnitude to allow comparison with the observations. The luminosity corresponding to this maximum rapidly decreases with halo age. The detection of halo white dwarfs beyond the cut-off of the disk luminosity function would therefore give an opportunity to estimate the time interval between halo and disk formation. Deep surveys in the red or infrared, which are not presently available, will be necessary for that purpose.

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