Gravitational wave asteroseismology with fast rotating neutron stars

Gaertig, Erich; Kokkotas, Kostas D.

doi:10.1103/physrevd.83.064031

Cited by 57 publications

(143 citation statements)

References 77 publications

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“…Potentially destabilizing mechanisms that may trigger instability for β > β sec , and that have been well studied in the literature, are viscosity and gravitational radiation reaction (Chandrasekhar 1970;Friedman & Schutz 1978;Lai 2001;Gaertig & Kokkotas 2011). A rough estimate for the growth time due to destabilization from gravitational radiation is…”

Section: Instability and Gw Productionmentioning

confidence: 99%

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Piro

Thrane

2012

ApJ

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Massive stars generally end their lives as neutron stars (NSs) or black holes (BHs), with NS formation typically occurring at the low-mass end and collapse to a BH more likely at the high-mass end. In an intermediate regime, with a mass range that depends on the uncertain details of rotation and mass loss during the star's life, an NS is initially formed, which then experiences fallback accretion and collapse to a BH. The electromagnetic consequence of such an event is not clear. Depending on the progenitor's structure, possibilities range from a long gamma-ray burst to a Type II supernova (which may or may not be jet powered) to a collapse with a weak electromagnetic signature. Gravitational waves (GWs) provide the exciting opportunity to peer through the envelope of a dying massive star and directly probe what is occurring inside. We explore whether fallback onto young NSs can be detected by ground-based interferometers. When the incoming material has sufficient angular momentum to form a disk, the accretion spins up the NS sufficiently to produce non-axisymmetric instabilities and gravitational radiation at frequencies of ∼700-2400 Hz for ∼30-3000 s until collapse to a BH occurs. Using a realistic excess cross-power search algorithm, we show that such events are detectable by Advanced LIGO out to ≈17 Mpc. From the rate of nearby core-collapse supernovae in the past five years, we estimate that there will be ∼1-2 events each year that are worth checking for fallback GWs. The observation of these unique GW signatures coincident with electromagnetic detections would identify the transient events that are associated with this channel of BH formation, while providing information about the protoneutron star progenitor.

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Section: Instability and Gw Productionmentioning

confidence: 99%

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Piro

Thrane

2012

ApJ

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“…In [100,101] the damping timescale due to gravitational wave emission of the l = m = 2 f −mode in rapidly rotating stars was studied, assuming uniform rotation and the Cowling approximation. In particular, [101] used tabulated EoSs and estimated that the Cowling approximation overestimates the mode frequencies by up to 30%, while it underestimates damping timescales by up to a factor of three.…”

Section: Hybrid Waveformsmentioning

confidence: 99%

Prospects for high frequency burst searches following binary neutron star coalescence with advanced gravitational wave detectors

et al. 2014

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The equation of state plays a critical role in the physics of the merger of two neutron stars. Recent numerical simulations with microphysical equation of state suggest the outcome of such events depends on the mass of the neutron stars. For less massive systems, simulations favor the formation of a hypermassive, quasi-stable neutron star, whose oscillations produce a short, high frequency burst of gravitational radiation. Its dominant frequency content is tightly correlated with the radius of the neutron star, and its measurement can be used to constrain the supranuclear equation of state. In contrast, the merger of higher mass systems results in prompt gravitational collapse to a black hole. We have developed an algorithm which combines waveform reconstruction from a morphologyindependent search for gravitational wave transients with Bayesian model selection, to discriminate between post-merger scenarios and accurately measure the dominant oscillation frequency. We demonstrate the efficacy of the method using a catalogue of simulated binary merger signals in data from LIGO and Virgo, and we discuss the prospects for this analysis in advanced ground-based gravitational wave detectors. From the waveforms considered in this work and assuming an optimally oriented source, we find that the post-merger neutron star signal may be detectable by this technique to ∼ 10-25 Mpc. We also find that we successfully discriminate between the post-merger scenarios with ∼ 95% accuracy and determine the dominant oscillation frequency of surviving post-merger neutron stars to within ∼ 10 Hz, averaged over all detected signals. This leads to an uncertainty in the estimated radius of a non-rotating 1.6 M⊙ reference neutron star of ∼ 100 m.

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“…The growth timescale for this secular instability is likely to be of order seconds or longer [120,121].…”

Section: Evolution Of the Rotation Rate And Prospects For Rotationmentioning

confidence: 99%

Correlated gravitational wave and neutrino signals from general-relativistic rapidly rotating iron core collapse

et al. 2012

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We present results from a new set of 3D general-relativistic hydrodynamic simulations of rotating iron core collapse. We assume octant symmetry and focus on axisymmetric collapse, bounce, the early postbounce evolution, and the associated gravitational wave (GW) and neutrino signals. We employ a finite-temperature nuclear equation of state, parameterized electron capture in the collapse phase, and a multi-species neutrino leakage scheme after bounce. The latter captures the important effects of deleptonization, neutrino cooling and heating and enables approximate predictions for the neutrino luminosities in the early evolution after core bounce. We consider 12-M and 40-M presupernova models and systematically study the effects of (i) rotation, (ii) progenitor structure, and (iii) postbounce neutrino leakage on dynamics, GW, and, neutrino signals. We demonstrate, that the GW signal of rapidly rotating core collapse is practically independent of progenitor mass and precollapse structure. Moreover, we show that the effects of neutrino leakage on the GW signal are strong only in nonrotating or slowly rotating models in which GW emission is not dominated by inner core dynamics. In rapidly rotating cores, core bounce of the centrifugally-deformed inner core excites the fundamental quadrupole pulsation mode of the nascent protoneutron star. The ensuing global oscillations (f ∼ 700 − 800 Hz) lead to pronounced oscillations in the GW signal and correlated strong variations in the rising luminosities of antineutrino and heavy-lepton neutrinos. We find these features in cores that collapse to protoneutron stars with spin periods 2.5 ms and rotational energies sufficient to drive hyper-energetic core-collapse supernova explosions. Hence, GW or neutrino observations of a core collapse event could deliver strong evidence for or against rapid core rotation. Joint GW + neutrino observations would allow to make statements with high confidence. Our estimates suggest that the GW signal should be detectable throughout the Milky Way by advanced laser-interferometer GW observatories, but a water-Cherenkov neutrino detector would have to be of near-megaton size to observe the variations in the early neutrino luminosities from a core collapse event at 1 kpc.

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Gravitational wave asteroseismology with fast rotating neutron stars

Cited by 57 publications

References 77 publications

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Gravitational Waves From Fallback Accretion Onto Neutron Stars

Prospects for high frequency burst searches following binary neutron star coalescence with advanced gravitational wave detectors

Correlated gravitational wave and neutrino signals from general-relativistic rapidly rotating iron core collapse

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