Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998astl...24..206i&link_type=abstract
Astronomy Letters, Volume 24, Issue 2, March 1998, pp.206-221; Pis'ma v Astronomicheskii Zhurnal, Vol. 24, p. 251
Astronomy and Astrophysics
Astronomy
14
Scientific paper
The evolution of a close binary system of neutron stars is studied in the point-mass approximation with allowance for gravitational radiation and mass exchange between the components of the system. The calculation of mass transfer from the low-mass component of the system based on the known approximations for the radii of the Roche lobe and the low-mass component provides the reliable determination of the characteristics of the system by the end of its evolution, which are virtually independent of the initial ratio of the component masses. The evolution of the system is accompanied by the mass loss from the low-mass component and ends in the explosion of this component at the time when its mass reaches the lower limit for neutron stars (close to 0.1 M_solar). After the explosion, the second component of the system leaves the supernova remnant with the speed and rotation period which are determined almost entirely by the total mass of the system M_t. The assumption about the explosion of the low-mass component and subsequent escape of the high-mass component (pulsar or black hole) from the system have been made in the recently proposed scenario of the explosion of collapsing supernovae with allowance for rotational effects (Imshennik 1992; Imshennik and Nadezhin 1992; Imshennik and Popov 1996). We formulate and substantiate an analytic model for the evolution of the system under consideration, in which virtually all mass exchange between the components occurs under the assumption of quasi-stationary circular orbits with significant energy and angular momentum losses related to gravitational radiation. Such character of the evolution persists until the time the mass of the low-mass component reaches the value of order ~ 0.15 M_solar. The remaining mass (~0.05 M_solar) is lost by this component in the dynamical regime and the given analytic model takes on, strictly speaking, the character of a crude estimate. On the basis of this model, the main features of gravitational radiation are calculated, as well as the system's parameters essential for observing collapsing supernovae, i.e., SNII (IIP, IIL) and, possibly, SNI(Ib, Ic).
Imshennik Vladimir S.
Popov V. D.
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