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dc.contributor.authorHolberg, Jay B.
dc.contributor.authorOswalt, Terry D.
dc.contributor.authorSión, Edward M.
dc.date.accessioned2014-12-01T19:42:25Z
dc.date.available2014-12-01T19:42:25Z
dc.date.issued2002
dc.identifier.citationHolberg, J.B., Oswalt, T.D., Sión, E.M. (2002) A determination of the local density of white dwarf stars. The Astrophysical Journal, 571(1), 512.en_US
dc.identifier.urihttp://hdl.handle.net/11141/447
dc.description.abstractThe most recent version of the Catalog of Spectroscopically Identified White Dwarfs lists 2249 white dwarf stars. Among these stars are 109 white dwarfs that have either reliable trigonometric parallaxes or color-based distance moduli that place them at a distance within 20 pc of the Sun. Most of these nearby white dwarfs are isolated stars, but 28 (25% of the sample) are in binary systems, including such well-known systems as Sirius A/B and Procyon A/B. There are also three double degenerate systems in this sample of the local white dwarf population. The sample of local white dwarfs is largely complete out to 13 pc, and the local density of white dwarf stars is found to be 5.0 ± 0.7 × 10-3 pc-3, with a corresponding mass density of 3.4 ± 0.5 × 10-3 M⊙ pc-3.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is available in accordance with the publisher's policy. It may be subject to U.S. Copyright Law.en_US
dc.rights.urihttp://aas.org/publications/aas-copyright-policyen_US
dc.titleA determination of the local density of white dwarf starsen_US
dc.typeArticleen_US
dc.identifier.doi10.1086/339842


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