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dc.contributor.authorMiller-Jones, James
dc.contributor.authorJonker, P.
dc.contributor.authorNelemans, G.
dc.contributor.authorPortegies Zwart, S.
dc.contributor.authorDhawan, V.
dc.contributor.authorBrisken, W.
dc.contributor.authorGallo, E.
dc.contributor.authorRupen, M.
dc.identifier.citationMiller-Jones, J. and Jonker, P. and Nelemans, G. and Portegies Zwart, S. and Dhawan, V. and Brisken, W. and Gallo, E. et al. 2009. The formation of the black hole in the X-ray binary system V404 Cyg. Monthly Notices of the Royal Astronomical Society. 394 (3): pp. 1440-1448.

Using new and archival radio data, we have measured the proper motion of the black hole X-ray binary V404 Cyg to be 9.2 ± 0.3 mas yr-1. Combined with the systemic radial velocity from the literature, we derive the full three-dimensional heliocentric space velocity of the system, which we use to calculate a peculiar velocity in the range 47–102 km s-1, with a best-fitting value of 64 km s-1. We consider possible explanations for the observed peculiar velocity and find that the black hole cannot have formed via direct collapse. A natal supernova is required, in which either significant mass (~11 M?) was lost, giving rise to a symmetric Blaauw kick of up to ~65 km s-1, or, more probably, asymmetries in the supernova led to an additional kick out of the orbital plane of the binary system. In the case of a purely symmetric kick, the black hole must have been formed with a mass ~9 M?, since when it has accreted 0.5–1.5 M? from its companion.

dc.publisherWiley-Blackwell Publishing Ltd.
dc.subjectstars: kinematics
dc.subjectstars: supernovae: general
dc.subjectstars: individual: V404 Cyg
dc.subjectradio continuum: stars
dc.subjectX-rays: binaries
dc.titleThe formation of the black hole in the X-ray binary system V404 Cyg
dc.typeJournal Article
dcterms.source.titleMonthly Notices of the Royal Astronomical Society
curtin.accessStatusFulltext not available

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