Journal Article

Stationary states of irrotational binary neutron star systems and their evolution as a result of gravitational wave emission

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 296, issue 1, pages L1-L5
Published in print May 1998 | ISSN: 0035-8711
Published online May 1998 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1046/j.1365-8711.1998.01385.x
Stationary states of irrotational binary neutron star systems and their evolution as a result of gravitational wave emission

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We have succeeded in obtaining exact configurations of irrotational binary systems for compressible (polytropic) equations of state. Our models correspond to binary systems of equal-mass neutron stars in the viscosity free limit. By using the obtained sequences of stationary states, the evolution of binary systems of irrotational neutron stars resulting from gravitational wave emission has been examined. For inviscid binary systems, the spin angular velocity of each component in a detached phase is smaller than the orbital angular velocity at a contact phase. The irrotational approximation during the evolution of binary neutron stars resulting from gravitational wave emission can therefore be justified. Our computational results show that the binary will never reach a dynamically unstable state before a contact phase, even for rather stiff polytropes with index N≳0.7, as the separation of two components decreases as a result of gravitational wave emission. This conclusion is quantitatively different from that of Lai, Rasio & Shapiro, who employed approximate solutions for polytropic binary systems.

Keywords: hydrodynamics; instabilities; binaries: close; stars: neutron; stars: rotation.

Journal Article.  0 words. 

Subjects: Astronomy and Astrophysics

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