Bound for entropy and viscosity ratio for strange quark matter

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dc.creatorBagchi, Manjari
dc.creatorDey, Jishnu
dc.creatorDey, Mira
dc.creatorGangopadhyay, Taparati
dc.creatorLaha, Sibasish
dc.creatorRay, Subharthi
dc.creatorSinha, Monika
dc.date2007-05-31
dc.date2008-07-03
dc.date.accessioned2026-07-07T11:56:53Z
dc.date.available2026-07-07T11:56:53Z
dc.descriptionHigh energy density ($\eps$) and temperature (T) links general relativity and hydrodynamics leading to a lower bound for the ratio of shear viscosity ($η$) and entropy density ($s$). We get the interesting result that the bound is saturated in the simple model for quark matter that we use for strange stars at the surface for $T \sim 80 MeV$. At this $T$ we have the possibility of cosmic separation of phases. At the surface of the star where the pressure is zero - the density $\eps$ has a fixed value for all stars of various masses with correspondingly varying central energy density $\eps_c$. Inside the star where this density is higher, the ratio of $η/s$ is larger and are like the known results found for perturbative QCD. This serves as a check of our calculation. The deconfined quarks at the surface of the strange star at $T = 80 MeV$ seem to constitute the most perfect interacting fluid permitted by nature.
dc.description10 pages, 2 figures, 1 table; Accepted for publication in Phys. Lett. B
dc.identifierhttps://arxiv.org/abs/0705.4645
dc.identifierhttp://arxiv.org/abs/0705.4645
dc.identifierPhys.Lett.B666:145-149,2008
dc.identifierdoi:10.1016/j.physletb.2008.07.008
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205692
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.titleBound for entropy and viscosity ratio for strange quark matter
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