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Case B: tex2html_wrap_inline768

Why it is possible that the Oppenheimer-Volkoff limit exceeds tex2html_wrap_inline770 ?

- fast rotation (which is naturally expected after the merging) increases the Oppenheimer-Volkoff limit to the value tex2html_wrap_inline772 (Friedman & Ipser, 1987) for hard equations of state.

- high temperature of the formed object.

- relativistic behavior of nuclear forces.

Thus we can present these three sub-scenarios as follows:




1. The lifetime of HSP (``hot'' spinar) is completely determined by the cooling time which is of the order of tex2html_wrap_inline780  s according to different calculations. The subsequent collapse is accompanied by the GWB, neutrino emission, and possible weak photon emission can be expected:


It seems very attractive to identify this cooling time with the mean characteristic gamma-ray burst duration tex2html_wrap_inline784  s!

2. The lifetime of CSP (``cool'' spinar, the centrifugal forces make the main contribution to the equilibrium) is completely defined by the characteristic time of the angular momentum loss tex2html_wrap_inline786 and evolutionary track looks like


3. Finally, for the high Oppenheimer-Volkoff limit for the cool non-rotating object, when


we obtain the formation of a very powerful pulsar (maybe without pulsation) with the maximum spin rotation


The characteristic time tex2html_wrap_inline786 of its evolution is governed by the momentum loss rate.

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