Rapidly rotating neutron star progenitorsстатья

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[1] Rapidly rotating neutron star progenitors / K. A. Postnov, A. G. Kuranov, D. A. Kolesnikov et al. // Monthly Notices of the Royal Astronomical Society. — 2016. — Vol. 463. — P. 1642–1650. Rotating proto-neutron stars can be important sources of gravitational waves to be searched for by present-day and future interferometric detectors. It was demonstrated by Imshennik that in extreme cases the rapid rotation of a collapsing stellar core may lead to fission and formation of a binary proto-neutron star which subsequently merges due to gravitational wave emission. In the present paper, we show that such dynamically unstable collapsing stellar cores may be the product of a former merger process of two stellar cores in a common envelope. We applied population synthesis calculations to assess the expected fraction of such rapidly rotating stellar cores which may lead to fission and formation of a pair of proto-neutron stars. We have used the BSE population synthesis code supplemented with a new treatment of stellar core rotation during the evolution via effective core-envelope coupling, characterized by the coupling time, τ_c. The validity of this approach is checked by direct MESA calculations of the evolution of a rotating 15 M_ star. From comparison of the calculated spin distribution of young neutron stars with the observed one, reported by Popov and Turolla, we infer the value τ_c ≅5 ×105 years. We show that merging of stellar cores in common envelopes can lead to collapses with dynamically unstable proto-neutron stars, with their formation rate being ∼0.1-1
collapses, depending on the common envelope efficiency. [ DOI ]

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