Constraining phases of quark matter with studies of r-mode damping in neutron stars
arXiv:1005.4161 · doi:10.1103/PhysRevC.82.055806
Abstract
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.
arXiv comment8 pages, 2 figures
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Cited by in corpus (9)
- EMMI Rapid Reaction Task Force Meeting on 'Quark Matter in Compact Star'
- g-mode Oscillations in Hybrid Stars: A Tale of Two Sounds
- Non-radial Oscillation Modes of Compact Stars with a Crust
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- Contraction of cold neutron star due to in the presence a quark core
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