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Tidal heating as a direct probe of strangeness inside neutron stars
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It has been discussed whether viscous processes in neutron star matter during a binary inspiral can damp out the tidal energy induced by the companion and heat up the star. Earlier investigations concluded that this tidal heating is negligible for normal neutron star matter. In this work, we suggest a novel effect of tidal heating involving strange matter in the neutron star interior, that can significantly heat up the star, and is potentially observable by current and future gravitational wave detectors. We propose that this could serve as a direct probe of strangeness in neutron stars.
Forward citations
Cited by 3 Pith papers
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Oscillations of Dissipative Neutron Stars: The Impact of Hyperonic Reaction Rates
Finite hyperonic reaction rates, encoded as a complex sound speed, damp neutron-star f-modes and remove hyperonic g-modes before their restoring force vanishes, producing a tidal lag.
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Radial Oscillations of Viscous Stars
Viscosity damps neutron-star radial modes on ms timescales, shifts frequencies by up to ~1% at ζ∼10^30 g/cm/s, produces overdamped modes above ∼10^31, and cannot stabilize unstable stars in Eckart or BDNK theory.
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