Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.281..145u&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 281, Issue 1, pp. 145-152.
Astronomy and Astrophysics
Astronomy
5
Hydrodynamics, Stars: Evolution, Stars: Interiors, Stars: Neutron
Scientific paper
The equilibrium number densities of species in particles in the neutron star core depend on the local density. Hydrodynamic motions, if they exist in the core, can deviate the chemical composition of matter from equilibrium, since the relaxation of a moving fluid element towards the new equilibrium requires a finite time. Thus, the moving core plasma is not entirely in chemical equilibrium, and the departure from equilibrium can substantially increase the rate of neutrino energy loss. In the frame of the simplest model, we examine the influence of a hydrodynamic flow on the neutrino emissivity and show that the latter may be enhanced by many orders of magnitude even for a relatively slow motion. The neutrino energy loss rate is calculated for a wide range of the velocity of flow. The effect of an enhanced neutrino emission on cooling is considered for different neutron star models. Cooling turns out to be extremely sensitive to the velocity of flow. Owing to this, a study of the thermal evolution of neutron stars may be a powerful diagnostic of their internal hydrodynamics. Thus, available observational data on the surface temperature are consistent with the theoretical models only if there are no motions in the core with velocity V>=10^-9 cm s^-1.
Shalybkov Dmitry A.
Urpin Vadim A.
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