RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Autores
Sarotsakulchai, Thawicharat; Qian, Sheng Bang; Soonthornthum, Boonrucksar; Fernandez Lajus, Eduardo Eusebio; Liu, Nian Ping; Zhou, Xiao; Zhang, Jia; Liao, Wen Ping; Reichart, Daniel E.; Haislip, Joshua B.; Kouprianov, Vladimir V.; Poshyachinda, Saran
Año de publicación
2019
Idioma
inglés
Tipo de recurso
artículo
Estado
versión publicada
Descripción
New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M1 ∼ 0.52 M and M2 ∼ 0.82 M). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10−9 d yr−1 is superimposed on a cyclic variation(A3 = 0.0054 d and P3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deepernormal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.
Fil: Sarotsakulchai, Thawicharat. University of Chinese Academy of Sciences; China. National Astronomical Research Institute of Thailand; Tailandia. Chinese Academy of Sciences; República de China
Fil: Qian, Sheng Bang. Chinese Academy of Sciences; República de China. University of Chinese Academy of Sciences; China
Fil: Soonthornthum, Boonrucksar. National Astronomical Research Institute of Thailand; Tailandia
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Liu, Nian Ping. Chinese Academy of Sciences; República de China
Fil: Zhou, Xiao. Chinese Academy of Sciences; República de China
Fil: Zhang, Jia. Chinese Academy of Sciences; República de China
Fil: Liao, Wen Ping. Chinese Academy of Sciences; República de China
Fil: Reichart, Daniel E.. University of North Carolina; Estados Unidos
Fil: Haislip, Joshua B.. University of North Carolina; Estados Unidos
Fil: Kouprianov, Vladimir V.. University of North Carolina; Estados Unidos
Fil: Poshyachinda, Saran. National Astronomical Research Institute of Thailand; Tailandia
Materia
BINARIES: CLOSE
BINARIES: ECLIPSING
STARS: EVOLUTION
STARS: INDIVIDUAL (RW DORADUS)
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:11336/125623
Acceder
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network_acronym_str CONICETDig
repository_id_str 3498
network_name_str CONICET Digital (CONICET)
spelling RW Doradus: A solar-type shallow contact binary with a new orbital period investigationSarotsakulchai, ThawicharatQian, Sheng BangSoonthornthum, BoonrucksarFernandez Lajus, Eduardo EusebioLiu, Nian PingZhou, XiaoZhang, JiaLiao, Wen PingReichart, Daniel E.Haislip, Joshua B.Kouprianov, Vladimir V.Poshyachinda, SaranBINARIES: CLOSEBINARIES: ECLIPSINGSTARS: EVOLUTIONSTARS: INDIVIDUAL (RW DORADUS)https://purl.org/becyt/ford/1.3https://purl.org/becyt/ford/1New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M1 ∼ 0.52 M and M2 ∼ 0.82 M). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10−9 d yr−1 is superimposed on a cyclic variation(A3 = 0.0054 d and P3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deepernormal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.Fil: Sarotsakulchai, Thawicharat. University of Chinese Academy of Sciences; China. National Astronomical Research Institute of Thailand; Tailandia. Chinese Academy of Sciences; República de ChinaFil: Qian, Sheng Bang. Chinese Academy of Sciences; República de China. University of Chinese Academy of Sciences; ChinaFil: Soonthornthum, Boonrucksar. National Astronomical Research Institute of Thailand; TailandiaFil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; ArgentinaFil: Liu, Nian Ping. Chinese Academy of Sciences; República de ChinaFil: Zhou, Xiao. Chinese Academy of Sciences; República de ChinaFil: Zhang, Jia. Chinese Academy of Sciences; República de ChinaFil: Liao, Wen Ping. Chinese Academy of Sciences; República de ChinaFil: Reichart, Daniel E.. University of North Carolina; Estados UnidosFil: Haislip, Joshua B.. University of North Carolina; Estados UnidosFil: Kouprianov, Vladimir V.. University of North Carolina; Estados UnidosFil: Poshyachinda, Saran. National Astronomical Research Institute of Thailand; TailandiaAstronomical Soc Japan2019-01-23info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdfapplication/pdfhttp://hdl.handle.net/11336/125623Sarotsakulchai, Thawicharat; Qian, Sheng Bang; Soonthornthum, Boonrucksar; Fernandez Lajus, Eduardo Eusebio; Liu, Nian Ping; et al.; RW Doradus: A solar-type shallow contact binary with a new orbital period investigation; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 71; 2; 23-1-2019; 1-130004-6264CONICET DigitalCONICETenginfo:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/pasj/article/71/2/34/5305914?searchresult=1info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/psy149info:eu-repo/semantics/openAccesshttps://creativecommons.org/licenses/by-nc-sa/2.5/ar/reponame:CONICET Digital (CONICET)instname:Consejo Nacional de Investigaciones Científicas y Técnicas2025-09-03T10:10:42Zoai:ri.conicet.gov.ar:11336/125623instacron: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:34982025-09-03 10:10:42.696CONICET Digital (CONICET) - Consejo Nacional de Investigaciones Científicas y Técnicasfalse
dc.title.none.fl_str_mv RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
title RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
spellingShingle RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
Sarotsakulchai, Thawicharat
BINARIES: CLOSE
BINARIES: ECLIPSING
STARS: EVOLUTION
STARS: INDIVIDUAL (RW DORADUS)
title_short RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
title_full RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
title_fullStr RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
title_full_unstemmed RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
title_sort RW Doradus: A solar-type shallow contact binary with a new orbital period investigation
dc.creator.none.fl_str_mv Sarotsakulchai, Thawicharat
Qian, Sheng Bang
Soonthornthum, Boonrucksar
Fernandez Lajus, Eduardo Eusebio
Liu, Nian Ping
Zhou, Xiao
Zhang, Jia
Liao, Wen Ping
Reichart, Daniel E.
Haislip, Joshua B.
Kouprianov, Vladimir V.
Poshyachinda, Saran
author Sarotsakulchai, Thawicharat
author_facet Sarotsakulchai, Thawicharat
Qian, Sheng Bang
Soonthornthum, Boonrucksar
Fernandez Lajus, Eduardo Eusebio
Liu, Nian Ping
Zhou, Xiao
Zhang, Jia
Liao, Wen Ping
Reichart, Daniel E.
Haislip, Joshua B.
Kouprianov, Vladimir V.
Poshyachinda, Saran
author_role author
author2 Qian, Sheng Bang
Soonthornthum, Boonrucksar
Fernandez Lajus, Eduardo Eusebio
Liu, Nian Ping
Zhou, Xiao
Zhang, Jia
Liao, Wen Ping
Reichart, Daniel E.
Haislip, Joshua B.
Kouprianov, Vladimir V.
Poshyachinda, Saran
author2_role author
author
author
author
author
author
author
author
author
author
author
dc.subject.none.fl_str_mv BINARIES: CLOSE
BINARIES: ECLIPSING
STARS: EVOLUTION
STARS: INDIVIDUAL (RW DORADUS)
topic BINARIES: CLOSE
BINARIES: ECLIPSING
STARS: EVOLUTION
STARS: INDIVIDUAL (RW DORADUS)
purl_subject.fl_str_mv https://purl.org/becyt/ford/1.3
https://purl.org/becyt/ford/1
dc.description.none.fl_txt_mv New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M1 ∼ 0.52 M and M2 ∼ 0.82 M). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10−9 d yr−1 is superimposed on a cyclic variation(A3 = 0.0054 d and P3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deepernormal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.
Fil: Sarotsakulchai, Thawicharat. University of Chinese Academy of Sciences; China. National Astronomical Research Institute of Thailand; Tailandia. Chinese Academy of Sciences; República de China
Fil: Qian, Sheng Bang. Chinese Academy of Sciences; República de China. University of Chinese Academy of Sciences; China
Fil: Soonthornthum, Boonrucksar. National Astronomical Research Institute of Thailand; Tailandia
Fil: Fernandez Lajus, Eduardo Eusebio. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina
Fil: Liu, Nian Ping. Chinese Academy of Sciences; República de China
Fil: Zhou, Xiao. Chinese Academy of Sciences; República de China
Fil: Zhang, Jia. Chinese Academy of Sciences; República de China
Fil: Liao, Wen Ping. Chinese Academy of Sciences; República de China
Fil: Reichart, Daniel E.. University of North Carolina; Estados Unidos
Fil: Haislip, Joshua B.. University of North Carolina; Estados Unidos
Fil: Kouprianov, Vladimir V.. University of North Carolina; Estados Unidos
Fil: Poshyachinda, Saran. National Astronomical Research Institute of Thailand; Tailandia
description New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M1 ∼ 0.52 M and M2 ∼ 0.82 M). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10−9 d yr−1 is superimposed on a cyclic variation(A3 = 0.0054 d and P3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deepernormal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.
publishDate 2019
dc.date.none.fl_str_mv 2019-01-23
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/11336/125623
Sarotsakulchai, Thawicharat; Qian, Sheng Bang; Soonthornthum, Boonrucksar; Fernandez Lajus, Eduardo Eusebio; Liu, Nian Ping; et al.; RW Doradus: A solar-type shallow contact binary with a new orbital period investigation; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 71; 2; 23-1-2019; 1-13
0004-6264
CONICET Digital
CONICET
url http://hdl.handle.net/11336/125623
identifier_str_mv Sarotsakulchai, Thawicharat; Qian, Sheng Bang; Soonthornthum, Boonrucksar; Fernandez Lajus, Eduardo Eusebio; Liu, Nian Ping; et al.; RW Doradus: A solar-type shallow contact binary with a new orbital period investigation; Astronomical Soc Japan; Publications Of The Astronomical Society Of Japan; 71; 2; 23-1-2019; 1-13
0004-6264
CONICET Digital
CONICET
dc.language.none.fl_str_mv eng
language eng
dc.relation.none.fl_str_mv info:eu-repo/semantics/altIdentifier/url/https://academic.oup.com/pasj/article/71/2/34/5305914?searchresult=1
info:eu-repo/semantics/altIdentifier/doi/10.1093/pasj/psy149
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 13.13397

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