On the initial progenitor masses of stellar mass black holes and neutron stars

Details On the initial progenitor masses of stellar mass black holes and neutron stars On the initial progenitor masses of stellar mass black holes and neutron stars

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...331l..29e&link_type=abstract

Astronomy and Astrophysics, v.331, p.L29-L32 (1998)

Astronomy and Astrophysics

Astrophysics

65

Black Holes, Neutron Stars, Stellar Evolution, Black Hole Mass Limit, X-Ray Binaries, Soft X-Ray Transients

Scientific paper

We examine the information on the progenitor masses of stellar black holes that can be derived from the seven known black hole X-ray binaries with low- mass donor stars (Soft X-ray Transients- SXRs) in combination with stellar evolution considerations and observed properties of High Mass X-ray Binaries (HMXBs). It appears that several independent lines of evidence indicate that a considerable fraction of the stars more massive than 20 - 25 M_sun leave black holes as remnants while, on the other hand, t e neutron star in at least one HMXB had a progenitor more massive than 50 M_sun. We argue that the only plausible explanation of these apparently contradicting facts is that in a certain mass range, probably between 20 and 50 M_sun, the outcome of core collapse can either be a neutron star or the black hole, depending on additional stellar parameters, for example rotation and magnetic fields. The high masses of the black holes in three soft X-ray Transients (6 - 13 M_sun) and Cygnus X-1 (16 M_sun) exclude the alternative explanation that in a limited mass range (e.g.20 - 40 M_sun) stars leave black holes, and, due to very heavy stellar wind mass loss, stars more massive than about 40 M_sun leave neutron stars, just as stars between 8 and 20 M_sun. Correspondence and requests for materials to ene@physic.ut.ee

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