Entropy & viscosity bound of strange stars

Details Entropy & viscosity bound of strange stars Entropy & viscosity bound of strange stars

2007-02-08

arxiv.org/abs/hep-ph/0702086v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

7 pages, 2 figures; Improved version available in arXiv:0705.4645 [astro-ph]

Scientific paper

At finite temperature (T) there is a link with general relativity and hydrodynamics that leads to a lower bound for the ratio of shear viscosity and entropy density (\eta/s). We find that the bound is saturated in the simple model for quark matter that we use for strange stars at T = 80 MeV, at the surface of a strange star. At this T we have the possibility of cosmic separation of phases. We find that, although strongly correlated, the quark matter at the surface of strange stars constitute the most perfect interacting fluid permitted by nature. At the centre of the star, however, the density is higher and conditions are more like the results found for perturbative QCD.

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