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

Autores
Shi, Guang; Qian, Sheng Bang; Fernandez Lajus, Eduardo Eusebio
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 CCD eclipse timings since 2010 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 day/year. This suggests the lifetime of the secondary star will attain to the end in a timescale of 0.97 × 106 years faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 year and an amplitude of 2.3 minutes may present 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 sustain in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M˙tr| 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 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 years or earlier.
Fil: Shi, Guang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; China
Fil: Qian, Sheng Bang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
Materia
STAR EVOLUTION
ECLIPSE
STAR WIND
V617 SGR
SUPERNOVAE
STAR OUTFLOWS
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:11336/10868
Acceder
id CONICETDig_f2000c7fc24b45f7be2f39dfda3c5953
oai_identifier_str oai:ri.conicet.gov.ar:11336/10868
network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 SagittariiShi, GuangQian, Sheng BangFernandez Lajus, Eduardo EusebioSTAR EVOLUTIONECLIPSESTAR WINDV617 SGRSUPERNOVAESTAR OUTFLOWShttps://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1This 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 CCD eclipse timings since 2010 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 day/year. This suggests the lifetime of the secondary star will attain to the end in a timescale of 0.97 × 106 years faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 year and an amplitude of 2.3 minutes may present 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 sustain in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M˙tr| 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 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 years or earlier.Fil: Shi, Guang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; ChinaFil: Qian, Sheng Bang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; ChinaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaAstronomical Soc Japan2014-02info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/10868Shi, Guang; Qian, Sheng Bang; Fernandez Lajus, Eduardo Eusebio; The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 66; 1; 2-2014; 1-50004-62642053-051Xenginfo:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/pst009info:eu-repo/semantics/altIdentifier/url/http://pasj.oxfordjournals.org/content/66/1/8info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1310.4928info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-10-15T14:30:48Zoai:ri.conicet.gov.ar:11336/10868instacron: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:34982025-10-15 14:30:49.062CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
spellingShingle The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
Shi, Guang
STAR EVOLUTION
ECLIPSE
STAR WIND
V617 SGR
SUPERNOVAE
STAR OUTFLOWS
title_short The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_full The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_fullStr The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_full_unstemmed The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii
title_sort The 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
Fernandez Lajus, Eduardo Eusebio
author Shi, Guang
author_facet Shi, Guang
Qian, Sheng Bang
Fernandez Lajus, Eduardo Eusebio
author_role author
author2 Qian, Sheng Bang
Fernandez Lajus, Eduardo Eusebio
author2_role author
author
dc.subject.none.fl_str_mv STAR EVOLUTION
ECLIPSE
STAR WIND
V617 SGR
SUPERNOVAE
STAR OUTFLOWS
topic STAR EVOLUTION
ECLIPSE
STAR WIND
V617 SGR
SUPERNOVAE
STAR OUTFLOWS
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
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 CCD eclipse timings since 2010 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 day/year. This suggests the lifetime of the secondary star will attain to the end in a timescale of 0.97 × 106 years faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 year and an amplitude of 2.3 minutes may present 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 sustain in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M˙tr| 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 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 years or earlier.
Fil: Shi, Guang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; China
Fil: Qian, Sheng Bang. Chinese Academy Of Sciences; República de China. University of the Chinese Academy of Sciences; China
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto de Astrofísica de la Plata; Argentina. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina
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 CCD eclipse timings since 2010 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 day/year. This suggests the lifetime of the secondary star will attain to the end in a timescale of 0.97 × 106 years faster than that predicted previously. In particular, a cyclic variation with a period of 4.5 year and an amplitude of 2.3 minutes may present 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 sustain in the V Sge-type star V617 Sgr during its long-term evolution. The mass transfer rate |M˙tr| 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 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 years or earlier.
publishDate 2014
dc.date.none.fl_str_mv 2014-02
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/11336/10868
Shi, Guang; Qian, Sheng Bang; Fernandez Lajus, Eduardo Eusebio; The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 66; 1; 2-2014; 1-5
0004-6264
2053-051X
url http://hdl.handle.net/11336/10868
identifier_str_mv Shi, Guang; Qian, Sheng Bang; Fernandez Lajus, Eduardo Eusebio; The confirmation and revision on the orbital period change of the possible type Ia supernova progenitor V617 Sagittarii; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 66; 1; 2-2014; 1-5
0004-6264
2053-051X
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/pst009
info:eu-repo/semantics/altIdentifier/url/http://pasj.oxfordjournals.org/content/66/1/8
info:eu-repo/semantics/altIdentifier/url/https://arxiv.org/abs/1310.4928
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 Astronomical Soc Japan
publisher.none.fl_str_mv Astronomical Soc Japan
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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score 13.22299

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