About: WD J1953−1019

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WD J1953−1019 is a hierarchical triple system of white dwarfs located at about 130 parsecs (about 420 light years) from the Earth. This is the first triple system of white dwarfs to be resolved. The three white dwarfs have an atmosphere of pure hydrogen and a mass of about 0.6 times that of the Sun.

Attributes	Values
rdf:type	Thing place dbo:Location schema:Place celestial body star
rdfs:label	J1953−1019 (fr) WD J1953−1019 (en)
rdfs:comment	J1953−1019 est un système triple de naines blanches situé à environ 130 parsecs (environ 420 années-lumière) de la Terre dans la constellation de l'Aigle. C'est le premier système triple de naines blanches à être résolu. Les trois naines blanches ont une atmosphère de pur hydrogène (DA) et une masse d'environ 0,6 fois celle du Soleil. L'âge de refroidissement est estimée à entre 40 et 290 millions d'années. Les trois étoiles proviendraient chacune d'une étoile qui avait une masse entre 1,6 et 2,6 fois celle du Soleil. (fr) WD J1953−1019 is a hierarchical triple system of white dwarfs located at about 130 parsecs (about 420 light years) from the Earth. This is the first triple system of white dwarfs to be resolved. The three white dwarfs have an atmosphere of pure hydrogen and a mass of about 0.6 times that of the Sun. (en)
foaf:name	WD J1953−1019 (en)
foaf:depiction
dcterms:subject	Aquila (constellation) Triple star systems White dwarfs
Wikipage page ID	60630610 (xsd:integer)
Wikipage revision ID	1073463500 (xsd:integer)
Link from a Wikipage to another Wikipage	Passband Barycenter Aquila (constellation) Triple star systems White dwarfs SDSS J0106−1000 Gemini (constellation) Aquila (constellation) WD J0651+2844 White dwarf Pan-STARRS Type Ia supernova Cetus (constellation) Gaia DR2 Chandrasekhar mass Lidov-Kozai oscillation
sameAs	WD J1953−1019 WD J1953−1019 WD J1953−1019
dbp:wikiPageUsesTemplate	dbt:Center dbt:Efn dbt:Notelist dbt:Reflist dbt:Short_description dbt:Starbox_astrometry dbt:Starbox_begin dbt:Starbox_catalog dbt:Starbox_character dbt:Starbox_detail dbt:Starbox_end dbt:Starbox_image dbt:Starbox_observe dbt:Starbox_reference dbt:Stars_of_Aquila dbt:Val dbt:· dbt:DEC dbt:RA
thumbnail	wiki-commons:Special:FilePath/J1953-1019_triple_system.jpg?width=300
appmag	17.180000 (xsd:double) 17.270000 (xsd:double) 17.280000 (xsd:double) 17.300000 (xsd:double)
appmag 1 passband	V (en)
appmag 2 passband	G (en)
appmag 3 passband	B (en)
appmag 4 passband	R (en)
class	DA (en)
component	A (en) B (en) C (en)
constell	Aquila (constellation)
dist pc	128.360000 (xsd:double) 130.370000 (xsd:double) 130.890000 (xsd:double)
epoch	2015.500000 (xsd:double)
mass	A: (en) B: (en) C: (en)
no heading	y (en)
prop mo dec	(en) −15.66 ± 0.12 (en) −16.10 ± 0.15 (en) −16.33 ± 0.11 (en)
prop mo ra	(en) −10.81 ± 0.25 (en) −10.94 ± 0.19 (en) −11.54 ± 0.18 (en)
Simbad	Gaia+DR2+4190499986125543168 (en) Gaia+DR2+4190499986125543296 (en) Gaia+DR2+4190500054845023488 (en)
temperature	A: (en) B: (en) C: (en)
type	White dwarf
has abstract	J1953−1019 est un système triple de naines blanches situé à environ 130 parsecs (environ 420 années-lumière) de la Terre dans la constellation de l'Aigle. C'est le premier système triple de naines blanches à être résolu. Les trois naines blanches ont une atmosphère de pur hydrogène (DA) et une masse d'environ 0,6 fois celle du Soleil. L'âge de refroidissement est estimée à entre 40 et 290 millions d'années. Les trois étoiles proviendraient chacune d'une étoile qui avait une masse entre 1,6 et 2,6 fois celle du Soleil. (fr) WD J1953−1019 is a hierarchical triple system of white dwarfs located at about 130 parsecs (about 420 light years) from the Earth. This is the first triple system of white dwarfs to be resolved. The three white dwarfs have an atmosphere of pure hydrogen and a mass of about 0.6 times that of the Sun. The system consists of a central pair, WD J1953−1019 BC, and a distant companion, WD J1953−1019 A. WD J1953−1019 B and C correspond to the sources Gaia DR2 4190499986125543168 and 4190499986125543296 respectively. The white dwarfs of the central pair, WD J1953−1019 B and C, are separated 303.25±0.01 AU from each other while the distant companion, WD J1953−1019 A, orbits the barycenter, or center of mass, of the central binary at a distance of 6398.97±0.09 AU. The cooling age found by M. Perpinyà-Vallès and collaborators for the three white dwarfs is consistent, with an estimated value between 40 and 290 million years. The three stars would each come from a star that had a mass between 1.6 and 2.6 times that of the Sun. A collision of the central pair due to Lidov-Kozai oscillations is unlikely as the system is dynamically stable. However, if this collision occurred, it could produce a type Ia supernova below the Chandrasekhar mass. (en)
appmag 5 passband	g (en)
dec	A: (en) B: (en) C: (en)
RA	A: (en)

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