Astronomy and Astrophysics Supplement Series, Vol. 117, May II 1996, 13-18
A simple method to compute white dwarf luminosity functions
E. García-Berro
Send offprint requests to: E. García-Berro
, M. Hernanz
,
J. Isern
, G. Chabrier
, L. Segretain
and R. Mochkovitch 
Departament de Física Aplicada, Universitat
Politècnica de Catalunya, Jordi Girona Salgado s/n,
Mòdul B-5, Campus Nord, 08034 Barcelona, Spain
Centre d'Estudis Avançats de Blanes, C.S.I.C.,
Camí de Santa Bàrbara, 17300 Blanes, Spain
Groupe d'Astrophysique, CNRS, Ecole Normale
Supérieure de Lyon, 69394 Lyon Cedex 07, France
Institut d'Astrophysique de Paris, CNRS, 98 bis Bd.
Arago, 75014 Paris, France
Received May 9; accepted October 2, 1995
Abstract:
The luminosity function of white dwarfs can be used to obtain helpful information about the properties of the Galaxy and allows one to discriminate among different models of galactic evolution. In this paper we provide the necessary tools to construct theoretical luminosity functions for any star formation rate, any initial mass function, and any relationship between the mass of the white dwarf and the mass of the progenitor.Key words: white dwarfs --- stars: evolution --- luminosity function
web@edpsciences.com


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