Binary mass function: Difference between revisions

Revision as of 22:34, 3 November 2016

Revision as of 22:38, 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>[{{cite web |url=http://eagle.phys.utk.edu/guidry/astro421/lectures/lecture490_ch15.pdf] |title=Observational Evidence for Black Holes |publisher=[[University of Tennessee]] –|access-date=November Observational3, Evidence2016 for Black}}</ref>

Holes. Retrieved 3 November 2016.</ref>

=== Exoplanets ===