Bound for entropy and viscosity ratio for strange quark matter

Details Bound for entropy and viscosity ratio for strange quark matter Bound for entropy and viscosity ratio for strange quark matter

2007-05-31

arxiv.org/abs/0705.4645v3

Phys.Lett.B666:145-149,2008

Astronomy and Astrophysics

Astrophysics

10 pages, 2 figures, 1 table; Accepted for publication in Phys. Lett. B

Scientific paper

10.1016/j.physletb.2008.07.008

High energy density ($\eps$) and temperature (T) links general relativity and hydrodynamics leading to a lower bound for the ratio of shear viscosity ($\eta$) 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 $\eta/s$ 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.

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