Gravitational waves from r-modes

Sá, Paulo M.; Tomé, Brigitte

doi:10.1007/s10509-007-9371-5

Cited by 3 publications

(2 citation statements)

References 17 publications

(28 reference statements)

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“…If α max is indeed ≪ 1 (see also [125, 27, 26, 28, 252, 24]), GW emission from r -modes in collapsed remnants is likely undetectable. From Equation (10), we can see that the GW signal is proportional to the mode amplitude, so a decrease in the maximum amplitude by an order of magnitude corresponds to an order of magnitude decrease in the GW strain.…”

Section: Gravitational Wave Emission Mechanismsmentioning

confidence: 99%

Gravitational Waves from Gravitational Collapse

Fryer

New

2011

Living Rev. Relativ.

171

111

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Gravitational-wave emission from stellar collapse has been studied for nearly four decades. Current state-of-the-art numerical investigations of collapse include those that use progenitors with more realistic angular momentum profiles, properly treat microphysics issues, account for general relativity, and examine non-axisymmetric effects in three dimensions. Such simulations predict that gravitational waves from various phenomena associated with gravitational collapse could be detectable with ground-based and space-based interferometric observatories. This review covers the entire range of stellar collapse sources of gravitational waves: from the accretion-induced collapse of a white dwarf through the collapse down to neutron stars or black holes of massive stars to the collapse of supermassive stars.Electronic Supplementary MaterialSupplementary material is available for this article at 10.12942/lrr-2011-1.

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Section: Gravitational Wave Emission Mechanismsmentioning

confidence: 99%

Gravitational Waves from Gravitational Collapse

Fryer

New

2011

Living Rev. Relativ.

171

111

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“…These gravitational waves may be detected given the expected improved sensitivities of ground-based interferometers eg. VIRGO, advanced LIGO [6]. In addition, r-modes are probes of the equation of state of cold and dense matter through viscous damping effects and advance our understanding of nuclear and quark interactions by providing an astrophysical and phenomenological link to Quantum Chromodynamics (QCD) over a certain range of temperatures (10 7 K T 10 11 K) and at super-saturation densities [n B ∼ (2-5)n sat ].…”

Section: Introductionmentioning

confidence: 99%

Constraining phases of quark matter with studies ofr-mode damping in compact stars

Rupak

Jaikumar

2010

Phys. Rev. C

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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 8 K 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 ν ≈ 56 − 11Hz 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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r-mode instability in quark stars with a crystalline crust

Rupak

Jaikumar

2013

Phys. Rev. C

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The r-mode instability, believed to limit the rotation speed of compact stars, can provide empirical confirmation for the existence of stable deconfined phases of quark matter that are predicted by weak coupling calculations in Quantum Chromodynamics. We construct a model for strange quark stars as heavy as 2M that are made of superconducting quark matter in the bulk and a thin crystalline quark matter crust. This crystalline quark crust is sufficiently robust to withstand r-mode heating and viscous rubbing for realistic mode amplitudes O(10 −2 ), unlike a crust made of neutron-rich nuclei. The dissipation provided by viscous rubbing at the core-crust boundary is both necessary and sufficient to obtain stable rotation speeds that are consistent with the majority of rapidly spinning pulsars in low mass X-ray binaries. Our analysis implies that while bare strange stars are ruled out by the existence of rapidly spinning pulsars, a strange star with a quark matter crust is a distinct possibility.

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Gravitational waves from r-modes

Cited by 3 publications

References 17 publications

Gravitational Waves from Gravitational Collapse

Gravitational Waves from Gravitational Collapse

Constraining phases of quark matter with studies ofr-mode damping in compact stars

r-mode instability in quark stars with a crystalline crust

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