Volume 441, Number 2, October II 2005
|Page(s)||689 - 694|
|Section||Stellar structure and evolution|
|Published online||19 September 2005|
Mass-radius relations for massive white dwarf stars
Departament de Física Aplicada, Universitat Politècnica de Catalunya, Av. del Canal Olímpic, s/n, 08860 Castelldefels, Spain e-mail: [leandro;garcia]@fa.upc.es
2 Institut d'Estudis Espacials de Catalunya, Ed. Nexus, c/Gran Capità 2, 08034 Barcelona, Spain e-mail: email@example.com
3 Institut de Ciències de l'Espai, C.S.I.C., Campus UAB, Facultat de Ciències, Torre C-5, 08193 Bellaterra, Spain
4 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, (1900) La Plata, Argentina e-mail: firstname.lastname@example.org
5 Instituto de Astrofísica La Plata, IALP, CONICET, Argentina
Accepted: 18 July 2005
We present detailed theoretical mass-radius relations for massive white dwarf stars with oxygen-neon cores. This work is motivated by recent observational evidence about the existence of white dwarf stars with very high surface gravities. Our results are based on evolutionary calculations that take into account the chemical composition expected from the evolutionary history of massive white dwarf progenitors. We present theoretical mass-radius relations for stellar mass values ranging from 1.06 to with a step of and effective temperatures from 150 000 K to ≈5000 K. A novel aspect predicted by our calculations is that the mass-radius relation for the most massive white dwarfs exhibits a marked dependence on the neutrino luminosity. Extensive tabulations for massive white dwarfs, accessible from our web site, are presented as well.
Key words: stars: evolution / stars: white dwarfs / stars: fundamental parameters
© ESO, 2005
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