Gravitational waves from pulsations of neutron stars described by realistic equations of state

Bernuzzi, Sebastiano; Nagar, Alessandro

doi:10.1103/physrevd.78.024024

Cited by 19 publications

(40 citation statements)

References 62 publications

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“…For what concerns the proper radial frequencies of F0, we estimate ν F = 3045 Hz and ν H = 7232 Hz, with a resolution of h 2 = 0.2 and a total simulated time of 7 ms. They agree within few percent with perturbative results computed in [135]. As expected in this case the evolutions with the cold table and with the corresponding hybrid EoS do not differ significantly, while we observe some small differences due to the different atmosphere treatment.…”

Section: A Stable Starssupporting

confidence: 88%

“…For instance the pulsations amplitude is less than 0.5% over 10 ms. Two frequencies dominates the pulsations: ν F = 1421 Hz and ν H = 3959 Hz. They agree within the errors estimated from the output time sampling (2%) with the fundamental radial linear mode and its first overtone as computed by perturbative methods [134,135]. The figure highlights a secular drift in the case that MC2 reconstruction is adopted.…”

Section: A Stable Starssupporting

confidence: 82%

“…The metric waveform is composed at early times of six GW cycles emitted during the three orbit inspiral. After the merger the emission is dominated by the bar-deformed HMNS, and the signal has a typical frequency around 3 kHz which increases as the HMNS becomes more compact [135,161]. Finally, after t ret > 2132 (10.5 ms) the GW signal is composed of the quasi-normal-mode ringing of the BH.…”

Section: Gravitational Wavesmentioning

confidence: 99%

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Numerical relativity simulations of binary neutron stars

Thierfelder¹,

Bernuzzi²,

Brügmann³

2011

Phys. Rev. D

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139

231

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We present a new numerical relativity code designed for simulations of compact binaries involving matter. The code is an upgrade of the BAM code to include general relativistic hydrodynamics and implements state-of-the-art high-resolution-shock-capturing schemes on a hierarchy of mesh refined Cartesian grids with moving boxes. We test and validate the code in a series of standard experiments involving single neutron star spacetimes. We present test evolutions of quasi-equilibrium equal-mass irrotational binary neutron star configurations in quasi-circular orbits which describe the late inspiral to merger phases. Neutron star matter is modeled as a zero-temperature fluid; thermal effects can be included by means of a simple ideal-gas prescription. We analyze the impact that the use of different values of damping parameter in the Gamma-driver shift condition has on the dynamics of the system. The use of different reconstruction schemes and their impact in the post-merger dynamics is investigated. We compute and characterize the gravitational radiation emitted by the system. Self-convergence of the waves is tested, and we consistently estimate error-bars on the numerically generated waveforms in the inspiral phase

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Section: A Stable Starssupporting

confidence: 88%

Section: A Stable Starssupporting

confidence: 82%

Section: Gravitational Wavesmentioning

confidence: 99%

See 1 more Smart Citation

Numerical relativity simulations of binary neutron stars

Thierfelder¹,

Bernuzzi²,

Brügmann³

2011

Phys. Rev. D

Self Cite

139

231

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“…Table I lists, by order of decreasing radius (or increasing compactness) the main characteristics of Tolman-Oppenheimer-Volkoff neutron star models built from these EOS having mass 1:4M . These NS properties were computed starting from the tabulated EOS, using Hermite polynomials interpolation [45], for all EOS but (MS1, MS2, MPA1, AP3), that we read instead from Table I of Ref. [9].…”

Section: A a Sample Of Equations Of Statementioning

confidence: 99%

Measurability of the tidal polarizability of neutron stars in late-inspiral gravitational-wave signals

2012

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The gravitational wave signal from a binary neutron star inspiral contains information on the nuclear equation of state. This information is contained in a combination of the tidal polarizability parameters of the two neutron stars and is clearest in the late inspiral, just before merger. We use the recently defined tidal extension of the effective one-body formalism to construct a controlled analytical description of the frequency-domain phasing of neutron star inspirals up to merger. Exploiting this analytical description we find that the tidal polarizability parameters of neutron stars can be measured by the advanced LIGO-Virgo detector network from gravitational wave signals having a reasonable signal-to-noise ratio of ¼ 16. This measurability result seems to hold for all the nuclear equations of state leading to a maximum mass larger than 1:97M . We also propose a promising new way of extracting information on the nuclear equation of state from a coherent analysis of an ensemble of gravitational wave observations of separate binary merger events.

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“…[These errors were later corrected in an erratum, which, however, did not correct Eq. (27), nor Fig. 2.]…”

Section: Motivation and Introductionmentioning

confidence: 97%

Relativistic tidal properties of neutron stars

2009

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We study the various linear responses of neutron stars to external relativistic tidal fields. We focus on three different tidal responses, associated to three different tidal coefficients: (i) a gravito-electric-type coefficient G\mu_\ell=[length]^{2\ell+1} measuring the \ell^{th}-order mass multipolar moment GM_{a_1... a_\ell} induced in a star by an external \ell^{th}-order gravito-electric tidal field G_{a_1... a_\ell}; (ii) a gravito-magnetic-type coefficient G\sigma_\ell=[length]^{2\ell+1} measuring the \ell^{th} spin multipole moment G S_{a_1... a_\ell} induced in a star by an external \ell^{th}-order gravito-magnetic tidal field H_{a_1... a_\ell}; and (iii) a dimensionless ``shape'' Love number h_\ell measuring the distortion of the shape of the surface of a star by an external \ell^{th}-order gravito-electric tidal field. All the dimensionless tidal coefficients G\mu_\ell/R^{2\ell+1}, G\sigma_\l/R^{2\ell+1} and h_\ell (where R is the radius of the star) are found to have a strong sensitivity to the value of the star's ``compactness'' c\equiv GM/(c_0^2 R) (where we indicate by c_0 the speed of light). In particular, G\mu_\l/R^{2\l+1}\sim k_\ell is found to strongly decrease, as c increases, down to a zero value as c is formally extended to the ``black-hole (BH) limit'' c^{BH}=1/2. The shape Love number h_\ell is also found to significantly decrease as c increases, though it does not vanish in the formal limit c\to c^{BH}. The formal vanishing of \mu_\ell and \sigma_\ell as c\to c^{BH} is a consequence of the no-hair properties of black holes; this suggests, but in no way proves, that the effective action describing the gravitational interactions of black holes may not need to be augmented by nonminimal worldline couplings.Comment: 21 pages, 10 figures. Matches the published versio

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Gravitational waves from pulsations of neutron stars described by realistic equations of state

Cited by 19 publications

References 62 publications

Numerical relativity simulations of binary neutron stars

Numerical relativity simulations of binary neutron stars

Measurability of the tidal polarizability of neutron stars in late-inspiral gravitational-wave signals

Relativistic tidal properties of neutron stars

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