The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation

Aims. The internal structure constants k j and the radius of gyration are useful tools for investigating the apsidal motion and tidal evolution of close binaries and planetary systems. These parameters are available for various evolutionary phases but they are scarce for the late stages of stellar e...

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Detalles Bibliográficos
Autor: Claret dos Santos, Antonio
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2012
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/422829
Acceso en línea:http://hdl.handle.net/10261/422829
Access Level:acceso abierto
Palabra clave:Binaries: eclipsing
Stars: interiors
Stars: evolution
Stars: rotation
White dwarfs
Stars: neutron
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spelling The internal structure of neutron stars and white dwarfs, and the Jacobi virial equationClaret dos Santos, AntonioBinaries: eclipsingStars: interiorsStars: evolutionStars: rotationWhite dwarfsStars: neutronAims. The internal structure constants k j and the radius of gyration are useful tools for investigating the apsidal motion and tidal evolution of close binaries and planetary systems. These parameters are available for various evolutionary phases but they are scarce for the late stages of stellar evolution. To cover this gap, we present here the calculations of the apsidal-motion constants, the fractional radius of gyration, and the gravitational potential energy for two grids of cooling evolutionary sequences of white dwarfs and for neutron star models.Methods. The cooling sequences of white dwarfs were computed with LPCODE. An additional alternative to the white dwarf models was also adopted with the MESA code which allows non-stop calculations from the pre main-sequence (PMS) up to the white dwarf cooling sequences. Neutron star models were acquired from the NSCool/TOV subroutines. The apsidal-motion constants, the moment of inertia, and the gravitational potential energy were computed with a fourth-order Runge-Kutta method.Results. The parameters are made available for four cooling sequences of white dwarfs (DA and DB types): 0.52, 0.57, 0.837 and 1.0 M · and for neutron star models covering a mass range from 1.0 up to 2.183 M ·, in 0.1 mass step. We show that, contrary to previously established opinion, the product of the form-factors β and α, which are related to the moment of inertia, and gravitational potential energy, is not constant during some evolutionary phases. Regardless of the final products of stellar evolution (white dwarfs, neutron stars and perhaps black holes), we found that they recover the initial value of product αβ at the pre main-sequence phase (≈0.4). These results may have important consequences for the investigation of the Jacobi virial equation. © 2012 ESO.I would like to thank L. Althaus and D. Page for useful dis- cussions concerning the modelling of white dwarfs and neutron stars. B. Paxton and A. Dotter are particularly acknowledged for their help during the imple- mentation of MESA. I would also like to thank M. Benacquista, B. Rufino and V. Costa for their comments. The Spanish MEC (AYA2009-10394, AYA2009- 14000-C03-01) is gratefully acknowledged for its support during the develop- ment of this work. This research has made use of the SIMBAD database, oper- ated at the CDS, Strasbourg, France, and of NASA’s Astrophysics Data System Abstract Service.Peer reviewedEDP SciencesMinisterio de Educación y Ciencia (España)Ministerio de Ciencia e Innovación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]202620262012info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/422829reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/MEC//AYA2009-10394info:eu-repo/grantAgreement/MICINN//AYA2009-14000-C03-01http://dx.doi.org/10.1051/0004-6361/201219176Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/4228292026-05-22T06:33:51Z
dc.title.none.fl_str_mv The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
title The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
spellingShingle The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
Claret dos Santos, Antonio
Binaries: eclipsing
Stars: interiors
Stars: evolution
Stars: rotation
White dwarfs
Stars: neutron
title_short The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
title_full The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
title_fullStr The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
title_full_unstemmed The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
title_sort The internal structure of neutron stars and white dwarfs, and the Jacobi virial equation
dc.creator.none.fl_str_mv Claret dos Santos, Antonio
author Claret dos Santos, Antonio
author_facet Claret dos Santos, Antonio
author_role author
dc.contributor.none.fl_str_mv Ministerio de Educación y Ciencia (España)
Ministerio de Ciencia e Innovación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Binaries: eclipsing
Stars: interiors
Stars: evolution
Stars: rotation
White dwarfs
Stars: neutron
topic Binaries: eclipsing
Stars: interiors
Stars: evolution
Stars: rotation
White dwarfs
Stars: neutron
description Aims. The internal structure constants k j and the radius of gyration are useful tools for investigating the apsidal motion and tidal evolution of close binaries and planetary systems. These parameters are available for various evolutionary phases but they are scarce for the late stages of stellar evolution. To cover this gap, we present here the calculations of the apsidal-motion constants, the fractional radius of gyration, and the gravitational potential energy for two grids of cooling evolutionary sequences of white dwarfs and for neutron star models.
publishDate 2012
dc.date.none.fl_str_mv 2012
2026
2026
dc.type.none.fl_str_mv info:eu-repo/semantics/article
http://purl.org/coar/resource_type/c_6501
Publisher's version
info:eu-repo/semantics/publishedVersion
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/422829
url http://hdl.handle.net/10261/422829
dc.language.none.fl_str_mv Inglés
language_invalid_str_mv Inglés
dc.relation.none.fl_str_mv #PLACEHOLDER_PARENT_METADATA_VALUE#
#PLACEHOLDER_PARENT_METADATA_VALUE#
info:eu-repo/grantAgreement/MEC//AYA2009-10394
info:eu-repo/grantAgreement/MICINN//AYA2009-14000-C03-01
http://dx.doi.org/10.1051/0004-6361/201219176
Sí
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
eu_rights_str_mv openAccess
dc.publisher.none.fl_str_mv EDP Sciences
publisher.none.fl_str_mv EDP Sciences
dc.source.none.fl_str_mv reponame:DIGITAL.CSIC. Repositorio Institucional del CSIC
instname:Consejo Superior de Investigaciones Científicas (CSIC)
instname_str Consejo Superior de Investigaciones Científicas (CSIC)
reponame_str DIGITAL.CSIC. Repositorio Institucional del CSIC
collection DIGITAL.CSIC. Repositorio Institucional del CSIC
repository.name.fl_str_mv
repository.mail.fl_str_mv
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