Observational lower mass limit for black hole formation derived from massive X-ray binaries

Details Observational lower mass limit for black hole formation derived from massive X-ray binaries Observational lower mass limit for black hole formation derived from massive X-ray binaries

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.309..598v&link_type=abstract

Nature (ISSN 0028-0836), vol. 309, July 14, 1984, p. 598-600. Research supported by the Nederlandse Organisatie voor Zuiver-Wete

Astronomy and Astrophysics

Astrophysics

63

Binary Stars, Black Holes (Astronomy), Stellar Evolution, Stellar Mass, X Ray Binaries, X Ray Sources, X Ray Stars, Astrophysics, Minima, Star Formation Rate, Stellar Envelopes, Supernovae, Wolf-Rayet Stars

Scientific paper

The high radial velocity amplitude and 1.70-day orbital period of the B3 V optical counterpart of the X-ray source LMC X-3 set a lower limit of 6 - 10 M_sun; for the mass of the X-ray source, strongly suggesting that it is a black hole. Considerations about the evolutionary history of the system lead to an upper limit to the mass of the progenitor of the compact star in this system: ≤80±10 M_sun;. From the orbital parameters of pulsating massive X-ray binaries one finds that stars with masses up to ≥40 M_sun; terminate life as neutron stars. Thus, if LMC X-3 is a black hole, the lower mass limit for terminating life as a black hole is in the range between 40 and 80 M_sun;. Together with the initial mass function of massive stars this yields a black hole formation rate in the galaxy about two orders of magnitude smaller than the neutron-star formation rate.

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