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Let us assume that two neutron stars with masses tex2html_wrap_inline742 and tex2html_wrap_inline744 are merging. The following state of the after-merging object is determined by the ratio of the resulting total mass and the Oppenheimer-Volkoff limit. Two different scenarios may be distinguished as follows (Lipunova & Lipunov, 1998):



Here and below we interpret the Oppenheimer-Volkoff limit not as the standard value derived for the cold equation of state of baryonic matter for a non-rotating neutron star, but as a modified one. In the general case the Oppenheimer-Volkoff limit is a function of the angular spin velocity of the object, its entropy, and the specific equation of state: tex2html_wrap_inline750 .

Each neutron star can have a mass lying between the limits:


tex2html_wrap_inline754 -- derived by Landau (1938).

tex2html_wrap_inline756 -- commonly suggested now.

Lipunov V.M.
Fri Nov 28 17:12:56 MSK 1997