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
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/85208
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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 |
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http://sedici.unlp.edu.ar/handle/10915/85208 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
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info:eu-repo/semantics/altIdentifier/issn/0004-6264 info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/pst009 |
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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) |
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openAccess |
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http://creativecommons.org/licenses/by-nc-sa/4.0/ Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) |
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application/pdf |
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