Astronomy and Astrophysics – Astrophysics
Scientific paper
Jan 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...267..433y&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 267, no. 2, p. 433-438.
Astronomy and Astrophysics
Astrophysics
44
Binary Stars, Neutron Stars, Stellar Evolution, Stellar Systems, Supernovae, B Stars, Stellar Mass, Stellar Models
Scientific paper
We investigate conditions for a double neutron star system to form through two supernova explosions in the evolution of massive binary systems. We calculate, in particular, the orbital change in the helium (or C + O) star-neutron star system and its center-of-mass velocity due to the explosion of the helium (or C + O) star. For the binary pulsars PSR 1534 + 12 and PSR 1913 + 16, the presupernova evolution models of helium stars provide important constraints on the parameters of the binary system. If the progenitor helium star is more massive than about 5 solar masses, its radius would not exceed the Roche lobe so that its explosion should be highly asymmetric, imparting a large kick velocity to the newly born neutron star. If the helium star is less massive than about 5 solar masses, it undergoes spiral-in of the companion neutron star to become a C + O star. The explosion of the C + O star might be a type Ic supernova or a peculiar type Ia supernova such as SN 1991 bg. The resultant double neutron star system would probably be smaller than those observed. However, such an evolutionary route would enhance the current estimate of the frequency of neutron star merging that could give rise to a gamma-ray burst and emission of gravitational radiation.
Nomoto Ken
Shigeyama Toshikazu
Yamaoka Hitoshi
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