Binary mass function: Difference between revisions

Revision as of 19:32, 2 November 2016

Revision as of 22:31, 3 November 2016

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=== X-ray binaries ===

If the accretor in an [[X-ray binary]] has a minimum mass that significantly exceeds the [[Tolman–Oppenheimer–Volkoff limit]] (the maximum possible mass for a [[neutron star]]), it is expected to be a black hole. This is the case in [[Cygnus X-1]], for example, where the radial velocity of the companion star has been measured.<ref>{{citation | last=Mauder | first=H. | date=1973 | title=On the Mass Limit of the X-ray Source in Cygnus X-1 | bibcode=1973A&A....28..473M | journal=[[Astronomy and Astrophysics]] | volume=28 | pages=473–475}}</ref><ref>[http://imagineeagle.gsfcphys.nasautk.govedu/featuresguidry/ybaastro421/cyg-X1-masslectures/mass-solution3lecture490_ch15.htmlpdf] NASA – Imagine the Universe! Partial Solution for Mass[[University of Cyg X-1Tennessee]]{{dead link|date=November– 2016Observational |bot=InternetArchiveBotEvidence |fix-attempted=yesfor }}</ref>Black

Holes</ref>

=== Exoplanets ===