Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii

Autores
Shi, Guang; Qian, Sheng Bang; Fernández Lajús, Eduardo
Año de publicación
2014
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
This work reports new photometric results of eclipsing cataclysmic variable V617 Sagittarii (V617 Sgr). We analyzed the orbital period change of V617 Sgr by employing three new (since 2010) CCD eclipse timings along with all the available data from the literature. It was found that the orbital period of V617 Sgr undergoes an obvious long-term increase, which confirms the result revealed by Steiner et al. (2006). The rate of orbital period increase was calculated to be P = +2.14(0.05) × 10-7 d yr-1. This suggests the lifetime of the secondary star will end in a timescale of 0.97 × 106 yr faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 yr and an amplitude of 2.3 min may appear in the O - C diagram. Dominated by the wind-accretion mechanism, high mass transfer from the low mass secondary to the white dwarf is expected to continue in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |Mtr| was estimated to be in the range of about 2.2 × 10-7 to 5.2 × 10-7 M⊙ yr-1. Accordingly, the already massive (≥ 1.2 M⊙) white dwarf primary will process stable nuclear burning, accrete a fraction of the mass from its companion to reach the standard Chandrasekhar mass limit (≃ 1.38 M⊙), and ultimately produce a type Ia supernova (SN Ia) within about 4-8 × 105 yr or earlier.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
Materia
Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: evolution
stars: individual (V617 Sgr)
stars: winds, outflows
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:10915/85208

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oai_identifier_str oai:sedici.unlp.edu.ar:10915/85208
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repository_id_str 1329
network_name_str SEDICI (UNLP)
spelling Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 SagittariiShi, GuangQian, Sheng BangFernández Lajús, EduardoCiencias Astronómicasbinaries: closebinaries: eclipsingstars: evolutionstars: individual (V617 Sgr)stars: winds, outflowsThis work reports new photometric results of eclipsing cataclysmic variable V617 Sagittarii (V617 Sgr). We analyzed the orbital period change of V617 Sgr by employing three new (since 2010) CCD eclipse timings along with all the available data from the literature. It was found that the orbital period of V617 Sgr undergoes an obvious long-term increase, which confirms the result revealed by Steiner et al. (2006). The rate of orbital period increase was calculated to be P = +2.14(0.05) × 10<SUP>-7</SUP> d yr<SUP>-1</SUP>. This suggests the lifetime of the secondary star will end in a timescale of 0.97 × 10<SUP>6</SUP> yr faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 yr and an amplitude of 2.3 min may appear in the O - C diagram. Dominated by the wind-accretion mechanism, high mass transfer from the low mass secondary to the white dwarf is expected to continue in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M<SUB>tr</SUB>| was estimated to be in the range of about 2.2 × 10<SUP>-7</SUP> to 5.2 × 10<SUP>-7</SUP> M⊙ yr<SUP>-1</SUP>. Accordingly, the already massive (≥ 1.2 M⊙) white dwarf primary will process stable nuclear burning, accrete a fraction of the mass from its companion to reach the standard Chandrasekhar mass limit (≃ 1.38 M⊙), and ultimately produce a type Ia supernova (SN Ia) within about 4-8 × 10<SUP>5</SUP> yr or earlier.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2014info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfhttp://sedici.unlp.edu.ar/handle/10915/85208enginfo:eu-repo/semantics/altIdentifier/issn/0004-6264info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/pst009info: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:UNLP2025-09-29T11:16:24Zoai:sedici.unlp.edu.ar:10915/85208Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:25.265SEDICI (UNLP) - Universidad Nacional de La Platafalse
dc.title.none.fl_str_mv Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
spellingShingle Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
Shi, Guang
Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: evolution
stars: individual (V617 Sgr)
stars: winds, outflows
title_short Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_full Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_fullStr Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_full_unstemmed Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_sort Confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
dc.creator.none.fl_str_mv Shi, Guang
Qian, Sheng Bang
Fernández Lajús, Eduardo
author Shi, Guang
author_facet Shi, Guang
Qian, Sheng Bang
Fernández Lajús, Eduardo
author_role author
author2 Qian, Sheng Bang
Fernández Lajús, Eduardo
author2_role author
author
dc.subject.none.fl_str_mv Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: evolution
stars: individual (V617 Sgr)
stars: winds, outflows
topic Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: evolution
stars: individual (V617 Sgr)
stars: winds, outflows
dc.description.none.fl_txt_mv This work reports new photometric results of eclipsing cataclysmic variable V617 Sagittarii (V617 Sgr). We analyzed the orbital period change of V617 Sgr by employing three new (since 2010) CCD eclipse timings along with all the available data from the literature. It was found that the orbital period of V617 Sgr undergoes an obvious long-term increase, which confirms the result revealed by Steiner et al. (2006). The rate of orbital period increase was calculated to be P = +2.14(0.05) × 10<SUP>-7</SUP> d yr<SUP>-1</SUP>. This suggests the lifetime of the secondary star will end in a timescale of 0.97 × 10<SUP>6</SUP> yr faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 yr and an amplitude of 2.3 min may appear in the O - C diagram. Dominated by the wind-accretion mechanism, high mass transfer from the low mass secondary to the white dwarf is expected to continue in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M<SUB>tr</SUB>| was estimated to be in the range of about 2.2 × 10<SUP>-7</SUP> to 5.2 × 10<SUP>-7</SUP> M⊙ yr<SUP>-1</SUP>. Accordingly, the already massive (≥ 1.2 M⊙) white dwarf primary will process stable nuclear burning, accrete a fraction of the mass from its companion to reach the standard Chandrasekhar mass limit (≃ 1.38 M⊙), and ultimately produce a type Ia supernova (SN Ia) within about 4-8 × 10<SUP>5</SUP> yr or earlier.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata
description This work reports new photometric results of eclipsing cataclysmic variable V617 Sagittarii (V617 Sgr). We analyzed the orbital period change of V617 Sgr by employing three new (since 2010) CCD eclipse timings along with all the available data from the literature. It was found that the orbital period of V617 Sgr undergoes an obvious long-term increase, which confirms the result revealed by Steiner et al. (2006). The rate of orbital period increase was calculated to be P = +2.14(0.05) × 10<SUP>-7</SUP> d yr<SUP>-1</SUP>. This suggests the lifetime of the secondary star will end in a timescale of 0.97 × 10<SUP>6</SUP> yr faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 yr and an amplitude of 2.3 min may appear in the O - C diagram. Dominated by the wind-accretion mechanism, high mass transfer from the low mass secondary to the white dwarf is expected to continue in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M<SUB>tr</SUB>| was estimated to be in the range of about 2.2 × 10<SUP>-7</SUP> to 5.2 × 10<SUP>-7</SUP> M⊙ yr<SUP>-1</SUP>. Accordingly, the already massive (≥ 1.2 M⊙) white dwarf primary will process stable nuclear burning, accrete a fraction of the mass from its companion to reach the standard Chandrasekhar mass limit (≃ 1.38 M⊙), and ultimately produce a type Ia supernova (SN Ia) within about 4-8 × 10<SUP>5</SUP> yr or earlier.
publishDate 2014
dc.date.none.fl_str_mv 2014
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/10915/85208
url http://sedici.unlp.edu.ar/handle/10915/85208
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/issn/0004-6264
info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/pst009
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
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
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repository.name.fl_str_mv SEDICI (UNLP) - Universidad Nacional de La Plata
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