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Tsuruta, S., and A.G.W. Cameron, 1965: Cooling of neutron stars. Nature, 207, 364-366.
The discovory of discrete sources of X-rays in the sky has led to much speculation as to the mechanisms responsible for the X-ray emission. Among these suggeations has b3en the thermal emission of X-rays from the hot surfaces of neutron star remnants of supernova explosions. Calculations of the cooling of such a neutron star following its formation have seemed to indicate that the temperature would still be several million degrees at an age of several thousand years. Such cooling calculations have been based on estimates of photon emission from the surface and of neutrino-antineutrino pair emission by the plasma process from the interior. There have recently been new suggestions regarding other possible mechanisms of neutrino emission from the interior, and this has led to the impression that neutron stars might cool too rapidly to be observable as celestial X-ray objects. We believe this view to be too pessimistic, and we give here a brief summary of some of our cooling calculations for neutron stars.
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