The discovery of binary white dwarfs that will merge within 500 Myr
- Autores
- Kilic, M.; Brown, W.R.; Allende Prieto, C.; Kenyon, S.J.; Panei, Jorge Alejandro
- Año de publicación
- 2010
- Idioma
- inglés
- Tipo de recurso
- artículo
- Estado
- versión publicada
- Descripción
- We present radial velocity observations of four extremely low-mass (0.2 M⊙) white dwarfs (WDs). All four stars show peak-to-peak radial velocity variations of 540-710kms-1 with 1.0-5.9hr periods. The optical photometry rules out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus, the invisible companions are most likely WDs. Two of the systems are the shortest period binary WDs yet discovered. Due to the loss of angular momentum through gravitational radiation, three of the systems will merge within 500Myr. The remaining system will merge within a Hubble time. The mass functions for three of the systems imply companions more massive than 0.46 M⊙; thus, those are carbon/oxygen core WDs. The unknown inclination angles prohibit a definitive conclusion about the future of these systems. However, the chance of a supernova Ia event is only 1%-5%. These systems are likely to form single R Coronae Borealis stars, providing evidence for a WD + WD merger mechanism for these unusual objects. One of the systems, SDSS J105353.89+520031.0, has a 70% chance of having a low-mass WD companion. This system will probably form a single helium-enriched subdwarf O star. All four WD systems have unusual mass ratios of ≤0.2-0.8 that may also lead to the formation of AM CVn systems.
Facultad de Ciencias Astronómicas y Geofísicas - Materia
-
Ciencias Astronómicas
Stars: low-mass
White dwarfs
SDSS J082212.57+275307.4
SDSS J084910.13+044528.7
SDSS J105353.89+520031.0
SDSS J143633.29+501026.8 - 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:10915/82486
Ver los metadatos del registro completo
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The discovery of binary white dwarfs that will merge within 500 MyrKilic, M.Brown, W.R.Allende Prieto, C.Kenyon, S.J.Panei, Jorge AlejandroCiencias AstronómicasStars: low-massWhite dwarfsSDSS J082212.57+275307.4SDSS J084910.13+044528.7SDSS J105353.89+520031.0SDSS J143633.29+501026.8We present radial velocity observations of four extremely low-mass (0.2 M⊙) white dwarfs (WDs). All four stars show peak-to-peak radial velocity variations of 540-710kms-1 with 1.0-5.9hr periods. The optical photometry rules out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus, the invisible companions are most likely WDs. Two of the systems are the shortest period binary WDs yet discovered. Due to the loss of angular momentum through gravitational radiation, three of the systems will merge within 500Myr. The remaining system will merge within a Hubble time. The mass functions for three of the systems imply companions more massive than 0.46 M⊙; thus, those are carbon/oxygen core WDs. The unknown inclination angles prohibit a definitive conclusion about the future of these systems. However, the chance of a supernova Ia event is only 1%-5%. These systems are likely to form single R Coronae Borealis stars, providing evidence for a WD + WD merger mechanism for these unusual objects. One of the systems, SDSS J105353.89+520031.0, has a 70% chance of having a low-mass WD companion. This system will probably form a single helium-enriched subdwarf O star. All four WD systems have unusual mass ratios of ≤0.2-0.8 that may also lead to the formation of AM CVn systems.Facultad de Ciencias Astronómicas y Geofísicas2010-05-14info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionArticulohttp://purl.org/coar/resource_type/c_6501info:ar-repo/semantics/articuloapplication/pdf122-130http://sedici.unlp.edu.ar/handle/10915/82486enginfo:eu-repo/semantics/altIdentifier/issn/0004637Xinfo:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637x/716/1/122info: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:UNLP2025-09-29T11:15:31Zoai:sedici.unlp.edu.ar:10915/82486Institucionalhttp://sedici.unlp.edu.ar/Universidad públicaNo correspondehttp://sedici.unlp.edu.ar/oai/snrdalira@sedici.unlp.edu.arArgentinaNo correspondeNo correspondeNo correspondeopendoar:13292025-09-29 11:15:32.172SEDICI (UNLP) - Universidad Nacional de La Platafalse |
dc.title.none.fl_str_mv |
The discovery of binary white dwarfs that will merge within 500 Myr |
title |
The discovery of binary white dwarfs that will merge within 500 Myr |
spellingShingle |
The discovery of binary white dwarfs that will merge within 500 Myr Kilic, M. Ciencias Astronómicas Stars: low-mass White dwarfs SDSS J082212.57+275307.4 SDSS J084910.13+044528.7 SDSS J105353.89+520031.0 SDSS J143633.29+501026.8 |
title_short |
The discovery of binary white dwarfs that will merge within 500 Myr |
title_full |
The discovery of binary white dwarfs that will merge within 500 Myr |
title_fullStr |
The discovery of binary white dwarfs that will merge within 500 Myr |
title_full_unstemmed |
The discovery of binary white dwarfs that will merge within 500 Myr |
title_sort |
The discovery of binary white dwarfs that will merge within 500 Myr |
dc.creator.none.fl_str_mv |
Kilic, M. Brown, W.R. Allende Prieto, C. Kenyon, S.J. Panei, Jorge Alejandro |
author |
Kilic, M. |
author_facet |
Kilic, M. Brown, W.R. Allende Prieto, C. Kenyon, S.J. Panei, Jorge Alejandro |
author_role |
author |
author2 |
Brown, W.R. Allende Prieto, C. Kenyon, S.J. Panei, Jorge Alejandro |
author2_role |
author author author author |
dc.subject.none.fl_str_mv |
Ciencias Astronómicas Stars: low-mass White dwarfs SDSS J082212.57+275307.4 SDSS J084910.13+044528.7 SDSS J105353.89+520031.0 SDSS J143633.29+501026.8 |
topic |
Ciencias Astronómicas Stars: low-mass White dwarfs SDSS J082212.57+275307.4 SDSS J084910.13+044528.7 SDSS J105353.89+520031.0 SDSS J143633.29+501026.8 |
dc.description.none.fl_txt_mv |
We present radial velocity observations of four extremely low-mass (0.2 M⊙) white dwarfs (WDs). All four stars show peak-to-peak radial velocity variations of 540-710kms-1 with 1.0-5.9hr periods. The optical photometry rules out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus, the invisible companions are most likely WDs. Two of the systems are the shortest period binary WDs yet discovered. Due to the loss of angular momentum through gravitational radiation, three of the systems will merge within 500Myr. The remaining system will merge within a Hubble time. The mass functions for three of the systems imply companions more massive than 0.46 M⊙; thus, those are carbon/oxygen core WDs. The unknown inclination angles prohibit a definitive conclusion about the future of these systems. However, the chance of a supernova Ia event is only 1%-5%. These systems are likely to form single R Coronae Borealis stars, providing evidence for a WD + WD merger mechanism for these unusual objects. One of the systems, SDSS J105353.89+520031.0, has a 70% chance of having a low-mass WD companion. This system will probably form a single helium-enriched subdwarf O star. All four WD systems have unusual mass ratios of ≤0.2-0.8 that may also lead to the formation of AM CVn systems. Facultad de Ciencias Astronómicas y Geofísicas |
description |
We present radial velocity observations of four extremely low-mass (0.2 M⊙) white dwarfs (WDs). All four stars show peak-to-peak radial velocity variations of 540-710kms-1 with 1.0-5.9hr periods. The optical photometry rules out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus, the invisible companions are most likely WDs. Two of the systems are the shortest period binary WDs yet discovered. Due to the loss of angular momentum through gravitational radiation, three of the systems will merge within 500Myr. The remaining system will merge within a Hubble time. The mass functions for three of the systems imply companions more massive than 0.46 M⊙; thus, those are carbon/oxygen core WDs. The unknown inclination angles prohibit a definitive conclusion about the future of these systems. However, the chance of a supernova Ia event is only 1%-5%. These systems are likely to form single R Coronae Borealis stars, providing evidence for a WD + WD merger mechanism for these unusual objects. One of the systems, SDSS J105353.89+520031.0, has a 70% chance of having a low-mass WD companion. This system will probably form a single helium-enriched subdwarf O star. All four WD systems have unusual mass ratios of ≤0.2-0.8 that may also lead to the formation of AM CVn systems. |
publishDate |
2010 |
dc.date.none.fl_str_mv |
2010-05-14 |
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/10915/82486 |
url |
http://sedici.unlp.edu.ar/handle/10915/82486 |
dc.language.none.fl_str_mv |
eng |
language |
eng |
dc.relation.none.fl_str_mv |
info:eu-repo/semantics/altIdentifier/issn/0004637X info:eu-repo/semantics/altIdentifier/doi/10.1088/0004-637x/716/1/122 |
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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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