The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation

Autores
García, Federico; Zhang, Guobao; Méndez, Mariano R.
Año de publicación
2013
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
We analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the ossi X-ray Timing Explorer ( RXTE). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From the analysis of time-resolved spectra during the cooling phase of the bursts, we found that the relation between the bolometric flux and the temperature is very different from the canonical F ∝ T⁴ relation which is expected if the apparent emitting area on the surface of the neutron star remains constant. The flux-temperature relation can be fitted using a broken power law, with indices ν₁ = 2.0 ± 0.3 and ν₂ = 5.72 ± 0.06. The departure from the F ∝ T⁴ relation during the cooling phase of the X-ray bursts in 4U 1820-30 could be due to changes in the emitting area of the neutron star while the atmosphere cools down, variations in the colour-correction factor due to chemical evolution, or the presence of a source of heat, e.g. residual hydrogen nuclear burning, playing an important role when the burst emission ceases.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
Materia
Astronomía
stars: individual: 4U 1820−30
stars: neutron
X-rays: binaries
X-rays: bursts
Nivel de accesibilidad
acceso abierto
Condiciones de uso
http://creativecommons.org/licenses/by-nc-sa/4.0/
Repositorio
SEDICI (UNLP)
Institución
Universidad Nacional de La Plata
OAI Identificador
oai:sedici.unlp.edu.ar:10915/127272
Acceder
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oai_identifier_str oai:sedici.unlp.edu.ar:10915/127272
network_acronym_str SEDICI
repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relationGarcía, FedericoZhang, GuobaoMéndez, Mariano R.Astronomíastars: individual: 4U 1820−30stars: neutronX-rays: binariesX-rays: burstsWe analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the <i>ossi X-ray Timing Explorer</i> (<i> RXTE</i>). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From the analysis of time-resolved spectra during the cooling phase of the bursts, we found that the relation between the bolometric flux and the temperature is very different from the canonical F ∝ T⁴ relation which is expected if the apparent emitting area on the surface of the neutron star remains constant. The flux-temperature relation can be fitted using a broken power law, with indices ν₁ = 2.0 ± 0.3 and ν₂ = 5.72 ± 0.06. The departure from the F ∝ T⁴ relation during the cooling phase of the X-ray bursts in 4U 1820-30 could be due to changes in the emitting area of the neutron star while the atmosphere cools down, variations in the colour-correction factor due to chemical evolution, or the presence of a source of heat, e.g. residual hydrogen nuclear burning, playing an important role when the burst emission ceases.Facultad de Ciencias Astronómicas y GeofísicasInstituto Argentino de Radioastronomía2013-03info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf3266-3271http://sedici.unlp.edu.ar/handle/10915/127272enginfo:eu-repo/semantics/altIdentifier/issn/0035-8711info:eu-repo/semantics/altIdentifier/issn/1365-2966info:eu-repo/semantics/altIdentifier/arxiv/1301.1035info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sts583info:eu-repo/semantics/openAccesshttp://creativecommons.org/licenses/by-nc-sa/4.0/Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)reponame:SEDICI (UNLP)instname:Universidad Nacional de La Platainstacron:UNLP2025-11-12T10:54:59Zoai:sedici.unlp.edu.ar:10915/127272Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-11-12 10:54:59.447SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
title The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
spellingShingle The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
García, Federico
Astronomía
stars: individual: 4U 1820−30
stars: neutron
X-rays: binaries
X-rays: bursts
title_short The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
title_full The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
title_fullStr The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
title_full_unstemmed The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
title_sort The cooling phase of Type I X-ray bursts observed with RXTE in 4U 1820−30 does not follow the canonical F ∝ T⁴ relation
dc.creator.none.fl_str_mv García, Federico
Zhang, Guobao
Méndez, Mariano R.
author García, Federico
author_facet García, Federico
Zhang, Guobao
Méndez, Mariano R.
author_role author
author2 Zhang, Guobao
Méndez, Mariano R.
author2_role author
author
dc.subject.none.fl_str_mv Astronomía
stars: individual: 4U 1820−30
stars: neutron
X-rays: binaries
X-rays: bursts
topic Astronomía
stars: individual: 4U 1820−30
stars: neutron
X-rays: binaries
X-rays: bursts
dc.description.none.fl_txt_mv We analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the <i>ossi X-ray Timing Explorer</i> (<i> RXTE</i>). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From the analysis of time-resolved spectra during the cooling phase of the bursts, we found that the relation between the bolometric flux and the temperature is very different from the canonical F ∝ T⁴ relation which is expected if the apparent emitting area on the surface of the neutron star remains constant. The flux-temperature relation can be fitted using a broken power law, with indices ν₁ = 2.0 ± 0.3 and ν₂ = 5.72 ± 0.06. The departure from the F ∝ T⁴ relation during the cooling phase of the X-ray bursts in 4U 1820-30 could be due to changes in the emitting area of the neutron star while the atmosphere cools down, variations in the colour-correction factor due to chemical evolution, or the presence of a source of heat, e.g. residual hydrogen nuclear burning, playing an important role when the burst emission ceases.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto Argentino de Radioastronomía
description We analysed the complete set of bursts from the neutron star low-mass X-ray binary 4U 1820-30 detected with the <i>ossi X-ray Timing Explorer</i> (<i> RXTE</i>). We found that all are photospheric radius expansion bursts, and have similar duration, peak flux and fluence. From the analysis of time-resolved spectra during the cooling phase of the bursts, we found that the relation between the bolometric flux and the temperature is very different from the canonical F ∝ T⁴ relation which is expected if the apparent emitting area on the surface of the neutron star remains constant. The flux-temperature relation can be fitted using a broken power law, with indices ν₁ = 2.0 ± 0.3 and ν₂ = 5.72 ± 0.06. The departure from the F ∝ T⁴ relation during the cooling phase of the X-ray bursts in 4U 1820-30 could be due to changes in the emitting area of the neutron star while the atmosphere cools down, variations in the colour-correction factor due to chemical evolution, or the presence of a source of heat, e.g. residual hydrogen nuclear burning, playing an important role when the burst emission ceases.
publishDate 2013
dc.date.none.fl_str_mv 2013-03
dc.type.none.fl_str_mv info:eu-repo/semantics/article
info:eu-repo/semantics/publishedVersion
Articulo
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://sedici.unlp.edu.ar/handle/10915/127272
url http://sedici.unlp.edu.ar/handle/10915/127272
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0035-8711
info:eu-repo/semantics/altIdentifier/issn/1365-2966
info:eu-repo/semantics/altIdentifier/arxiv/1301.1035
info:eu-repo/semantics/altIdentifier/doi/10.1093/mnras/sts583
dc.rights.none.fl_str_mv info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
eu_rights_str_mv openAccess
rights_invalid_str_mv http://creativecommons.org/licenses/by-nc-sa/4.0/
Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
dc.format.none.fl_str_mv application/pdf
3266-3271
dc.source.none.fl_str_mv reponame:SEDICI (UNLP)
instname:Universidad Nacional de La Plata
instacron:UNLP
reponame_str SEDICI (UNLP)
collection SEDICI (UNLP)
instname_str Universidad Nacional de La Plata
instacron_str UNLP
institution UNLP
repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
repository.mail.fl_str_mv alira@sedici.unlp.edu.ar
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score 13.24909

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