Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion

Conventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models chara...

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Autores principales: Althaus, Leandro Gabriel, Serenelli, Aldo Marcelo, Benvenuto, Omar Gustavo
Formato: Articulo
Lenguaje:Inglés
Publicado: 2001
Materias:
Ciencias Astronómicas
astrofísica
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/2056
http://iopscience.iop.org/article/10.1086/321414/meta
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-2056
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
astrofísica
spellingShingle Ciencias Astronómicas
astrofísica
Althaus, Leandro Gabriel
Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
topic_facet Ciencias Astronómicas
astrofísica
description Conventional wisdom indicates that a millisecond pulsar is recycled during the mass transfer stage in a binary system. Usually, the companion to the pulsar is a low-mass white dwarf. If zero ages are set at the end of mass transfer, the ages of both objects should be the same. Available models characterized by dominant hydrogen burning lead to a strong discrepancy between the ages of PSR B1855]09 and its white dwarf companion. We interpret such a discrepancy as a direct consequence of ignoring element di usion in the stellar models. We show that in the frame of models in which di usion is properly accounted for, ages naturally come into a nice agreement. Consequently, we do not have to invoke any ad hoc mass loss or exotic mechanisms to account for the ages of the stars that belong to the binary system PSR B1855]09.
format Articulo
Articulo
author Althaus, Leandro Gabriel
Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
author_facet Althaus, Leandro Gabriel
Serenelli, Aldo Marcelo
Benvenuto, Omar Gustavo
author_sort Althaus, Leandro Gabriel
title Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_short Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_full Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_fullStr Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_full_unstemmed Formation and evolution of a 0.242 <i>M</i><SUB>⊙</SUB> solar masses helium white dwarfs in presence of element diffusion
title_sort formation and evolution of a 0.242 <i>m</i><sub>⊙</sub> solar masses helium white dwarfs in presence of element diffusion
publishDate 2001
url http://sedici.unlp.edu.ar/handle/10915/2056
http://iopscience.iop.org/article/10.1086/321414/meta
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