The initial mass limit for neutron star and black hole formation

Details The initial mass limit for neutron star and black hole formation The initial mass limit for neutron star and black hole formation

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...143l...7s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 143, no. 2, Feb. 1985, p. L7-L10. Research supported by the Swiss National Sci

Astronomy and Astrophysics

Astronomy

37

Black Holes (Astronomy), Neutron Stars, Pulsars, Star Clusters, Stellar Evolution, Stellar Mass, Metallicity, Nuclear Fusion, Wolf-Rayet Stars

Scientific paper

The membership of pulsars to young (<107 y) clusters and associations is analysed. As expected, the rate of pulsars associated to stellar groups is a strongly decreasing function of the pulsar ages. From pulsars in the youngest associations we find that stars with an initial mass on the zero age main sequence up to 50 Msub terminate their evolution as neutron stars. This suggests that black holes, if any exist, are formed from stars initially more massive than 50 Msun. The ratio δY/δZ of the relative helium to metal enrichment is rather sensitive to the lower mass limit MBH for black hole formation. Although important uncertainties remain, the best empirical data on δY/δZ are consistent with a value of 50 Msun for MBH. Among the consequences of black holes being formed only from large initial stellar masses (at least in Pop. I) we note: 1) It is not likely that the missing mass is locked in the form of black holes since their expected number is very low. 2) The direct progenitors of black holes are Wolf-Rayet stars of late WN or early WC subtype.

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