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
- Institución
- Consejo Nacional de Investigaciones Científicas y Técnicas
- OAI Identificador
- oai:ri.conicet.gov.ar:11336/10893
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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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1844614337325432832 |
score |
13.070432 |