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2012MNRAS.421.2206D - Mon. Not. R. Astron. Soc., 421, 2206-2222 (2012/April-2)
The evolution of low-mass, close binary systems with a neutron star component: a detailed grid.
DE VITO M.A. and BENVENUTO O.G.
Abstract (from CDS):
In this paper, we explore the evolutionary response of these close binary systems when we vary the amount of material accreted by the neutron star. We consider a parameter β which represents the fraction of material lost by the normal star that can be accreted by the neutron star. β is considered as constant throughout the evolution. We have computed the evolution of a set of models considering initial donor star masses Mi/M☉between 0.5 and 3.50, initial orbital periods Pi/d between 0.175 and 12, initial masses of neutron stars (MNS)i/M☉ of 0.80, 1.00, 1.20 and 1.40 and several values of β. We assumed solar abundances. These systems evolve to ultracompact or to open binary systems, many of which form low-mass helium white dwarfs. We present a grid of calculations and analyse how these results are affected upon changes in the value of β. We find a weak dependence of the final donor star mass on β. In most cases, this is also true for the final orbital period. The most sensitive quantity is the final mass of the accreting neutron star.
As we do not know the initial mass and rotation rate of the neutron star of any system, we find that performing evolutionary studies is not helpful for determining β.
Abstract Copyright: 2012 The Authors Monthly Notices of the Royal Astronomical Society2012 RAS
Journal keyword(s): binaries: close - stars: evolution - white dwarfs
CDS comments: Table 2, PSR J1614+2230 is a probable misprint for PSR J1614-2230.
Simbad objects: 8
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