1,043 research outputs found
Cosmological Neutrino Background Revisited
We solve the Boltzmann equation for cosmological neutrinos around the epoch
of the electron-positron annihilation in order to verify the freeze-out
approximation and to compute accurately the cosmological neutrino distribution
function. We find the radiation energy density to be about 0.3% higher than the
one predicted by the freeze-out approximation. As a result, the spectrum of the
Cosmic Microwave Background anisotropies changes by 0.3-05%, depending on the
angular scale, and the amplitude of the mass fluctuations on scales below about
100 h^{-1} Mpc decreases by about 0.2-0.3%.Comment: An error is corrected, figure revised; submitted to Ap
Thermal Evolution of a Pulsating Neutron Star
We have derived a set of equations to describe the thermal evolution of a
neutron star which undergoes small-amplitude radial pulsations. We have taken
into account, in the frame of the General Theory of Relativity, the pulsation
damping due to the bulk and shear viscosity and the accompanying heating of the
star. The neutrino emission of a pulsating non-superfluid star and its heating
due to the bulk viscosity are calculated assuming that both processes are
determined by the non-equilibrium modified Urca process. Analytical and
numerical solutions to the set of equations of the stellar evolution are
obtained for linear and strongly non-linear deviations from beta-equilibrium.
It is shown that a pulsating star may be heated to very high temperatures,
while the pulsations damp very slowly with time (a power law damping for
100-1000 years), as long as the damping is determined by the bulk viscosity.
The contribution of the shear viscosity to the damping becomes important in a
rather cool star with a low pulsation energy.Comment: 10 pages, 3 figures, an important reference to the paper by Finzi &
Wolf (1968) is added; analytical consideration of the problem (Section 5) is
essentially extende
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