SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion
- Autores
- Qian, S. B.; Jiang, L. Q.; Fernández Lajús, Eduardo; Soonthornthum, B.; Zhu, L. Y.; Zhao, E. G.; He, J. J.; Liao, W. P.; Wang, J. J.; Liu, L.; Rattanasoon, S.; Aukkaravittayapun, S.; Zhou, X.; Liu, N. P.
- Año de publicación
- 2015
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- SDSS J001641-000925 is the first red dwarf contact binary star with an orbital period of 0.19856 days that is one of the shortest known periods among M-dwarf binary systems. The orbital period was detected to be decreasing rapidly at a rate of P ∼ 8 s yr-1. This indicated that SDSS J001641-000925 was undergoing coalescence via a dynamical mass transfer or loss and thus this red dwarf contact binary is dynamically unstable. To understand the properties of the period change, we monitored the binary system photometrically from 2011 September 2 to 2014 October 1 by using several telescopes in the world and 25 eclipse times were determined. It is discovered that the rapid decrease of the orbital period is not true. This is contrary to the prediction that the system is merging driven by rapid mass transfer or loss. Our preliminary analysis suggests that the observed minus calculated (O-C) diagram shows a cyclic oscillation with an amplitude of 0.00255 days and a period of 5.7 yr. The cyclic variation can be explained by the light travel time effect via the presence of a cool stellar companion with a mass of M3 sin i′ ∼ 0.14 M⊙. The orbital separation between the third body and the central binary is about 2.8AU. These results reveal that the rarity of red dwarf contact binaries could not be explained by rapidly dynamical destruction and the presence of the third body helps to form the red dwarf contact binary.
Facultad de Ciencias Astronómicas y Geofísicas
Instituto de Astrofísica de La Plata - Materia
-
Ciencias Astronómicas
binaries: close
binaries: eclipsing
stars: evolution
stars: individual (SDSS J001641-000925) - Nivel de accesibilidad
- acceso abierto
- Condiciones de uso
- http://creativecommons.org/licenses/by-nc-sa/4.0/
- Repositorio
.jpg)
- Institución
- Universidad Nacional de La Plata
- OAI Identificador
- oai:sedici.unlp.edu.ar:10915/86141
Ver los metadatos del registro completo
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SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companionQian, S. B.Jiang, L. Q.Fernández Lajús, EduardoSoonthornthum, B.Zhu, L. Y.Zhao, E. G.He, J. J.Liao, W. P.Wang, J. J.Liu, L.Rattanasoon, S.Aukkaravittayapun, S.Zhou, X.Liu, N. P.Ciencias Astronómicasbinaries: closebinaries: eclipsingstars: evolutionstars: individual (SDSS J001641-000925)SDSS J001641-000925 is the first red dwarf contact binary star with an orbital period of 0.19856 days that is one of the shortest known periods among M-dwarf binary systems. The orbital period was detected to be decreasing rapidly at a rate of P ∼ 8 s yr<SUP>-1</SUP>. This indicated that SDSS J001641-000925 was undergoing coalescence via a dynamical mass transfer or loss and thus this red dwarf contact binary is dynamically unstable. To understand the properties of the period change, we monitored the binary system photometrically from 2011 September 2 to 2014 October 1 by using several telescopes in the world and 25 eclipse times were determined. It is discovered that the rapid decrease of the orbital period is not true. This is contrary to the prediction that the system is merging driven by rapid mass transfer or loss. Our preliminary analysis suggests that the observed minus calculated (O-C) diagram shows a cyclic oscillation with an amplitude of 0.00255 days and a period of 5.7 yr. The cyclic variation can be explained by the light travel time effect via the presence of a cool stellar companion with a mass of M<SUB>3</SUB> sin i′ ∼ 0.14 M⊙. The orbital separation between the third body and the central binary is about 2.8AU. These results reveal that the rarity of red dwarf contact binaries could not be explained by rapidly dynamical destruction and the presence of the third body helps to form the red dwarf contact binary.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plata2015info: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/10915/86141enginfo:eu-repo/semantics/altIdentifier/issn/2041-8205info:eu-repo/semantics/altIdentifier/doi/10.1088/2041-8205/798/2/L42info: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:UNLP2025-09-29T11:16:59Zoai:sedici.unlp.edu.ar:10915/86141Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:16:59.342SEDICI (UNLP) - Universidad Nacional de La Platafalse |
| dc.title.none.fl_str_mv |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| title |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| spellingShingle |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion Qian, S. B. Ciencias Astronómicas binaries: close binaries: eclipsing stars: evolution stars: individual (SDSS J001641-000925) |
| title_short |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| title_full |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| title_fullStr |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| title_full_unstemmed |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| title_sort |
SDSS J001641-000925: The first stable red dwarf contact binary with a close-in stellar companion |
| dc.creator.none.fl_str_mv |
Qian, S. B. Jiang, L. Q. Fernández Lajús, Eduardo Soonthornthum, B. Zhu, L. Y. Zhao, E. G. He, J. J. Liao, W. P. Wang, J. J. Liu, L. Rattanasoon, S. Aukkaravittayapun, S. Zhou, X. Liu, N. P. |
| author |
Qian, S. B. |
| author_facet |
Qian, S. B. Jiang, L. Q. Fernández Lajús, Eduardo Soonthornthum, B. Zhu, L. Y. Zhao, E. G. He, J. J. Liao, W. P. Wang, J. J. Liu, L. Rattanasoon, S. Aukkaravittayapun, S. Zhou, X. Liu, N. P. |
| author_role |
author |
| author2 |
Jiang, L. Q. Fernández Lajús, Eduardo Soonthornthum, B. Zhu, L. Y. Zhao, E. G. He, J. J. Liao, W. P. Wang, J. J. Liu, L. Rattanasoon, S. Aukkaravittayapun, S. Zhou, X. Liu, N. P. |
| author2_role |
author author author author author author author author author author author author author |
| dc.subject.none.fl_str_mv |
Ciencias Astronómicas binaries: close binaries: eclipsing stars: evolution stars: individual (SDSS J001641-000925) |
| topic |
Ciencias Astronómicas binaries: close binaries: eclipsing stars: evolution stars: individual (SDSS J001641-000925) |
| dc.description.none.fl_txt_mv |
SDSS J001641-000925 is the first red dwarf contact binary star with an orbital period of 0.19856 days that is one of the shortest known periods among M-dwarf binary systems. The orbital period was detected to be decreasing rapidly at a rate of P ∼ 8 s yr<SUP>-1</SUP>. This indicated that SDSS J001641-000925 was undergoing coalescence via a dynamical mass transfer or loss and thus this red dwarf contact binary is dynamically unstable. To understand the properties of the period change, we monitored the binary system photometrically from 2011 September 2 to 2014 October 1 by using several telescopes in the world and 25 eclipse times were determined. It is discovered that the rapid decrease of the orbital period is not true. This is contrary to the prediction that the system is merging driven by rapid mass transfer or loss. Our preliminary analysis suggests that the observed minus calculated (O-C) diagram shows a cyclic oscillation with an amplitude of 0.00255 days and a period of 5.7 yr. The cyclic variation can be explained by the light travel time effect via the presence of a cool stellar companion with a mass of M<SUB>3</SUB> sin i′ ∼ 0.14 M⊙. The orbital separation between the third body and the central binary is about 2.8AU. These results reveal that the rarity of red dwarf contact binaries could not be explained by rapidly dynamical destruction and the presence of the third body helps to form the red dwarf contact binary. Facultad de Ciencias Astronómicas y Geofísicas Instituto de Astrofísica de La Plata |
| description |
SDSS J001641-000925 is the first red dwarf contact binary star with an orbital period of 0.19856 days that is one of the shortest known periods among M-dwarf binary systems. The orbital period was detected to be decreasing rapidly at a rate of P ∼ 8 s yr<SUP>-1</SUP>. This indicated that SDSS J001641-000925 was undergoing coalescence via a dynamical mass transfer or loss and thus this red dwarf contact binary is dynamically unstable. To understand the properties of the period change, we monitored the binary system photometrically from 2011 September 2 to 2014 October 1 by using several telescopes in the world and 25 eclipse times were determined. It is discovered that the rapid decrease of the orbital period is not true. This is contrary to the prediction that the system is merging driven by rapid mass transfer or loss. Our preliminary analysis suggests that the observed minus calculated (O-C) diagram shows a cyclic oscillation with an amplitude of 0.00255 days and a period of 5.7 yr. The cyclic variation can be explained by the light travel time effect via the presence of a cool stellar companion with a mass of M<SUB>3</SUB> sin i′ ∼ 0.14 M⊙. The orbital separation between the third body and the central binary is about 2.8AU. These results reveal that the rarity of red dwarf contact binaries could not be explained by rapidly dynamical destruction and the presence of the third body helps to form the red dwarf contact binary. |
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2015 |
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2015 |
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