Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries

Autores
Sravan, N.; Valsecchi, F.; Kalogera, V.; Althaus, Leandro Gabriel
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
Although not nearly as numerous as binaries with two white dwarfs, eccentric neutron star–white dwarf (NS–WD) binaries are important gravitational-wave (GW) sources for the next generation of space-based detectors sensitive to low frequency waves. Here we investigate periastron precession in these sources as a result of general relativistic, tidal, and rotational effects; such precession is expected to be detectable for at least some of the detected binaries of this type. Currently, two eccentric NS–WD binaries are known in the galactic field, PSR J1141−6545 and PSR B2303+46, both of which have orbits too wide to be relevant in their current state to GW observations. However, population synthesis studies predict the existence of a significant Galactic population of such systems. Though small in most of these systems, we find that tidally induced periastron precession becomes important when tides contribute to more than 3% of the total precession rate. For these systems, accounting for tides when analyzing periastron precession rate measurements can improve estimates of the inferred WD component mass and, in some cases, will prevent us from misclassifying the object. However, such systems are rare, due to rapid orbital decay. To aid the inclusion of tidal effects when using periastron precession as a mass measurement tool, we derive a function that relates the WD radius and periastron precession constant to the WD mass.
Fil: Sravan, N.. Northwestern University; Estados Unidos
Fil: Valsecchi, F.. Northwestern University; Estados Unidos
Fil: Kalogera, V.. Northwestern University; Estados Unidos
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
Materia
White Dwarves
Gravitational Waves
Psr B2303+46 Psr J1141–6545
Nivel de accesibilidad
acceso abierto
Condiciones de uso
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
Repositorio
CONICET Digital (CONICET)
Institución
Consejo Nacional de Investigaciones Científicas y Técnicas
OAI Identificador
oai:ri.conicet.gov.ar:11336/10893

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spelling Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf BinariesSravan, N.Valsecchi, F.Kalogera, V.Althaus, Leandro GabrielWhite DwarvesGravitational WavesPsr B2303+46 Psr J1141–6545https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1Although not nearly as numerous as binaries with two white dwarfs, eccentric neutron star–white dwarf (NS–WD) binaries are important gravitational-wave (GW) sources for the next generation of space-based detectors sensitive to low frequency waves. Here we investigate periastron precession in these sources as a result of general relativistic, tidal, and rotational effects; such precession is expected to be detectable for at least some of the detected binaries of this type. Currently, two eccentric NS–WD binaries are known in the galactic field, PSR J1141−6545 and PSR B2303+46, both of which have orbits too wide to be relevant in their current state to GW observations. However, population synthesis studies predict the existence of a significant Galactic population of such systems. Though small in most of these systems, we find that tidally induced periastron precession becomes important when tides contribute to more than 3% of the total precession rate. For these systems, accounting for tides when analyzing periastron precession rate measurements can improve estimates of the inferred WD component mass and, in some cases, will prevent us from misclassifying the object. However, such systems are rare, due to rapid orbital decay. To aid the inclusion of tidal effects when using periastron precession as a mass measurement tool, we derive a function that relates the WD radius and periastron precession constant to the WD mass.Fil: Sravan, N.. Northwestern University; Estados UnidosFil: Valsecchi, F.. Northwestern University; Estados UnidosFil: Kalogera, V.. Northwestern University; Estados UnidosFil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; ArgentinaIop Publishing2014-08info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10893Sravan, N.; Valsecchi, F.; Kalogera, V.; Althaus, Leandro Gabriel; Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries; Iop Publishing; Astrophysical Journal; 792; 2; 8-2014; 1-130004-637X1538-4357enginfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/792/2/138info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/792/2/138/metainfo:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1401.0831info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-29T10:32:23Zoai:ri.conicet.gov.ar:11336/10893instacron:CONICETInstitucionalhttp://ri.conicet.gov.ar/Organismo científico-tecnológicoNo correspondehttp://ri.conicet.gov.ar/oai/requestdasensio@conicet.gov.ar; lcarlino@conicet.gov.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:34982025-09-29 10:32:24.059CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
title Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
spellingShingle Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
Sravan, N.
White Dwarves
Gravitational Waves
Psr B2303+46 Psr J1141–6545
title_short Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
title_full Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
title_fullStr Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
title_full_unstemmed Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
title_sort Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries
dc.creator.none.fl_str_mv Sravan, N.
Valsecchi, F.
Kalogera, V.
Althaus, Leandro Gabriel
author Sravan, N.
author_facet Sravan, N.
Valsecchi, F.
Kalogera, V.
Althaus, Leandro Gabriel
author_role author
author2 Valsecchi, F.
Kalogera, V.
Althaus, Leandro Gabriel
author2_role author
author
author
dc.subject.none.fl_str_mv White Dwarves
Gravitational Waves
Psr B2303+46 Psr J1141–6545
topic White Dwarves
Gravitational Waves
Psr B2303+46 Psr J1141–6545
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv Although not nearly as numerous as binaries with two white dwarfs, eccentric neutron star–white dwarf (NS–WD) binaries are important gravitational-wave (GW) sources for the next generation of space-based detectors sensitive to low frequency waves. Here we investigate periastron precession in these sources as a result of general relativistic, tidal, and rotational effects; such precession is expected to be detectable for at least some of the detected binaries of this type. Currently, two eccentric NS–WD binaries are known in the galactic field, PSR J1141−6545 and PSR B2303+46, both of which have orbits too wide to be relevant in their current state to GW observations. However, population synthesis studies predict the existence of a significant Galactic population of such systems. Though small in most of these systems, we find that tidally induced periastron precession becomes important when tides contribute to more than 3% of the total precession rate. For these systems, accounting for tides when analyzing periastron precession rate measurements can improve estimates of the inferred WD component mass and, in some cases, will prevent us from misclassifying the object. However, such systems are rare, due to rapid orbital decay. To aid the inclusion of tidal effects when using periastron precession as a mass measurement tool, we derive a function that relates the WD radius and periastron precession constant to the WD mass.
Fil: Sravan, N.. Northwestern University; Estados Unidos
Fil: Valsecchi, F.. Northwestern University; Estados Unidos
Fil: Kalogera, V.. Northwestern University; Estados Unidos
Fil: Althaus, Leandro Gabriel. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico La Plata. Instituto de Astrofísica de La Plata; Argentina
description Although not nearly as numerous as binaries with two white dwarfs, eccentric neutron star–white dwarf (NS–WD) binaries are important gravitational-wave (GW) sources for the next generation of space-based detectors sensitive to low frequency waves. Here we investigate periastron precession in these sources as a result of general relativistic, tidal, and rotational effects; such precession is expected to be detectable for at least some of the detected binaries of this type. Currently, two eccentric NS–WD binaries are known in the galactic field, PSR J1141−6545 and PSR B2303+46, both of which have orbits too wide to be relevant in their current state to GW observations. However, population synthesis studies predict the existence of a significant Galactic population of such systems. Though small in most of these systems, we find that tidally induced periastron precession becomes important when tides contribute to more than 3% of the total precession rate. For these systems, accounting for tides when analyzing periastron precession rate measurements can improve estimates of the inferred WD component mass and, in some cases, will prevent us from misclassifying the object. However, such systems are rare, due to rapid orbital decay. To aid the inclusion of tidal effects when using periastron precession as a mass measurement tool, we derive a function that relates the WD radius and periastron precession constant to the WD mass.
publishDate 2014
dc.date.none.fl_str_mv 2014-08
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
http://purl.org/coar/resource_type/c_6501
info:ar-repo/semantics/articulo
format article
status_str publishedVersion
dc.identifier.none.fl_str_mv http://hdl.handle.net/11336/10893
Sravan, N.; Valsecchi, F.; Kalogera, V.; Althaus, Leandro Gabriel; Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries; Iop Publishing; Astrophysical Journal; 792; 2; 8-2014; 1-13
0004-637X
1538-4357
url http://hdl.handle.net/11336/10893
identifier_str_mv Sravan, N.; Valsecchi, F.; Kalogera, V.; Althaus, Leandro Gabriel; Importance of tides for periastron precession in eccentric Neutron Star-White Dwarf Binaries; Iop Publishing; Astrophysical Journal; 792; 2; 8-2014; 1-13
0004-637X
1538-4357
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637X/792/2/138
info:eu-repo/semantics/altIdentifier/url/http://iopscience.iop.org/article/10.1088/0004-637X/792/2/138/meta
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1401.0831
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
eu_rights_str_mv openAccess
rights_invalid_str_mv https://creativecommons.org/licenses/by-nc-sa/2.5/ar/
dc.format.none.fl_str_mv application/pdf
application/pdf
dc.publisher.none.fl_str_mv Iop Publishing
publisher.none.fl_str_mv Iop Publishing
dc.source.none.fl_str_mv reponame:CONICET Digital (CONICET)
instname:Consejo Nacional de Investigaciones Científicas y Técnicas
reponame_str CONICET Digital (CONICET)
collection CONICET Digital (CONICET)
instname_str Consejo Nacional de Investigaciones Científicas y Técnicas
repository.name.fl_str_mv CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicas
repository.mail.fl_str_mv dasensio@conicet.gov.ar; lcarlino@conicet.gov.ar
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