Constraining phases of quark matter with studies of r-mode damping in neutron stars

Details Constraining phases of quark matter with studies of r-mode damping in neutron stars Constraining phases of quark matter with studies of r-mode damping in neutron stars

2010-05-23

arxiv.org/abs/1005.4161v1

Phys.Rev.C82:055806,2010

Physics

Nuclear Physics

Nuclear Theory

8 pages, 2 figures

Scientific paper

10.1103/PhysRevC.82.055806

The r-mode instability in rotating compact stars is used to constrain the phase of matter at high density. The color-flavor-locked phase with kaon condensation (CFL-K0) and without (CFL) is considered in the temperature range 10^8K < T <10^{11} K. While the bulk viscosity in either phase is only effective at damping the r-mode at temperatures T > 10^{11} K, the shear viscosity in the CFL-K0 phase is the only effective damping agent all the way down to temperatures T > 10^8 K characteristic of cooling neutron stars. However, it cannot keep the star from becoming unstable to gravitational wave emission for rotation frequencies f ~ 56-11 Hz at T ~ 10^8-10^9 K. Stars composed almost entirely of CFL or CFL-K0 matter are ruled out by observation of rapidly rotating neutron stars, indicating that dissipation at the quark-hadron interface or nuclear crust interface must play a key role in damping the instability.

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