The white dwarf mass-radius relation and its dependence on the hydrogen envelope

We present a study of the dependence of the mass–radius relation for DA white dwarf stars on the hydrogen envelope mass and the impact on the value of log g, and thus the determination of the stellar mass. We employ a set of full evolutionary carbon–oxygen core white dwarf sequences with white dwarf...

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Autores principales: Romero, Alejandra D., Kepler, S. O., Joyce, S. R. G., Lauffer, G. R., Córsico, Alejandro Hugo
Formato: Articulo
Lenguaje:Inglés
Publicado: 2019
Materias:
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/125354
Aporte de:
id I19-R120-10915-125354
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
Binaries: general
Stars: interiors
White dwarfs.
spellingShingle Ciencias Astronómicas
Binaries: general
Stars: interiors
White dwarfs.
Romero, Alejandra D.
Kepler, S. O.
Joyce, S. R. G.
Lauffer, G. R.
Córsico, Alejandro Hugo
The white dwarf mass-radius relation and its dependence on the hydrogen envelope
topic_facet Ciencias Astronómicas
Binaries: general
Stars: interiors
White dwarfs.
description We present a study of the dependence of the mass–radius relation for DA white dwarf stars on the hydrogen envelope mass and the impact on the value of log g, and thus the determination of the stellar mass. We employ a set of full evolutionary carbon–oxygen core white dwarf sequences with white dwarf mass between 0.493 and 1.05 M<sub>⊙</sub>. Computations of the pre-white-dwarf evolution uncovers an intrinsic dependence of the maximum mass of the hydrogen envelope on the stellar mass; i.e. it decreases when the total mass increases. We find that a reduction of the hydrogen envelope mass can lead to a reduction in the radius of the model of up to ∼12 per cent. This translates directly to an increase in log g for a fixed stellar mass, which can reach up to 0.11 dex, mainly overestimating the determinations of stellar mass from atmospheric parameters. Finally, we find a good agreement between the results from the theoretical mass–radius relation and observations from white dwarfs in binary systems. In particular, we find a thin hydrogen mass of M<sub>H</sub> ∼ 2 × 10⁻⁸ M<sub>⊙</sub>. for 40 Eridani B, in agreement with previous determinations. For Sirius B, the spectroscopic mass is 4.3 per cent lower than the dynamical mass. However, the values of mass and radius from gravitational redshift observations are compatible with the theoretical mass–radius relation for a thick hydrogen envelope of M<sub>H</sub> = 2 × 10⁻⁶ M<sub>⊙</sub>.
format Articulo
Articulo
author Romero, Alejandra D.
Kepler, S. O.
Joyce, S. R. G.
Lauffer, G. R.
Córsico, Alejandro Hugo
author_facet Romero, Alejandra D.
Kepler, S. O.
Joyce, S. R. G.
Lauffer, G. R.
Córsico, Alejandro Hugo
author_sort Romero, Alejandra D.
title The white dwarf mass-radius relation and its dependence on the hydrogen envelope
title_short The white dwarf mass-radius relation and its dependence on the hydrogen envelope
title_full The white dwarf mass-radius relation and its dependence on the hydrogen envelope
title_fullStr The white dwarf mass-radius relation and its dependence on the hydrogen envelope
title_full_unstemmed The white dwarf mass-radius relation and its dependence on the hydrogen envelope
title_sort white dwarf mass-radius relation and its dependence on the hydrogen envelope
publishDate 2019
url http://sedici.unlp.edu.ar/handle/10915/125354
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