Entropy & viscosity bound of strange stars

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dc.creatorLaha, Sibasish
dc.creatorGangopadhyay, Taparati
dc.creatorBagchi, Manjari
dc.creatorDey, Mira
dc.creatorDey, Jishnu
dc.creatorSinha, Monika
dc.creatorRay, Subharthi
dc.date2007-02-08
dc.date.accessioned2026-07-07T08:05:54Z
dc.date.available2026-07-07T08:05:54Z
dc.descriptionAt 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 (η/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.
dc.description7 pages, 2 figures; Improved version available in arXiv:0705.4645 [astro-ph]
dc.identifierhttps://arxiv.org/abs/hep-ph/0702086
dc.identifierhttp://arxiv.org/abs/hep-ph/0702086
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/130426
dc.subjectHigh Energy Physics - Phenomenology
dc.subjectAstrophysics
dc.titleEntropy & viscosity bound of strange stars
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