Relativistic Binaries in Globular Clusters

Benacquista, M.; Downing, J. M. B.

doi:10.12942/lrr-2013-4

Cited by 198 publications

(132 citation statements)

References 443 publications

(618 reference statements)

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“…The centrifugal breakup of NS spins for most EoS is ∼ 1500 Hz, far greater than the maximum spin of ∼ 700 Hz inferred from X-ray observations [457]. It has, therefore, been a puzzle as to why NS spin frequencies are stalled.…”

Section: Science Targetsmentioning

confidence: 95%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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Section: Science Targetsmentioning

confidence: 95%

Sources of Gravitational Waves: Theory and Observations

Buonanno

Sathyaprakash²

2015

General Relativity and Gravitation

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“…There is also evidence that dynamical capture and exchange interactions involving NSs are a frequent occurrence in globular clusters [20]; during this process exotic objects, such as double millisecond pulsars might form [21].…”

Section: Introductionmentioning

confidence: 99%

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the stars’ rotation

et al. 2017

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We present new (3+1) dimensional numerical relativity simulations of the binary neutron star (BNS) mergers that take into account the NS spins. We consider different spin configurations, aligned or antialigned to the orbital angular momentum, for equal and unequal mass BNS and for two equations of state. All the simulations employ quasiequilibrium circular initial data in the constant rotational velocity approach, i.e. they are consistent with Einstein equations and in hydrodynamical equilibrium. We study the NS rotation effect on the energetics, the gravitational waves (GWs) and on the possible electromagnetic (EM) emission associated to dynamical mass ejecta. For dimensionless spin magnitudes of χ ∼ 0.1 we find that both spin-orbit interactions and spin-induced-quadrupole deformations affect the late-inspiral-merger dynamics. The latter is, however, dominated by finite-size effects. Spin (tidal) effects contribute to GW phase differences up to ∼ 5 (20) radians accumulated during the last eight orbits to merger. Similarly, after merger the collapse time of the remnant and the GW spectrogram are affected by the NSs rotation. Spin effects in dynamical ejecta are clearly observed in unequal mass systems in which mass ejection originates from the tidal tail of the companion. Consequently kilonovae and other EM counterparts are affected by spins. We find that spin aligned to the orbital angular momentum leads to brighter EM counterparts than antialigned spin with luminosities up to a factor of two higher.

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“…Also the spins at merger could potentially be considerably higher than those observed in binary pulsars to date, which is discussed in Appendix A 2. On the other hand, dynamical capture in dense stellar regions, such as globular clusters, offers the possibility of forming quite exotic objects, such as double millisecond pulsars [8,9]. In fact, there is good evidence that dynamical capture and exchange interactions involving neutron stars are a frequent occurrence in globular clusters [10].…”

Section: Introductionmentioning

confidence: 99%

Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

Dietrich¹,

Moldenhauer²,

et al. 2015

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Information about the last stages of a binary neutron star inspiral and the final merger can be extracted from quasiequilibrium configurations and dynamical evolutions. In this article, we construct quasiequilibrium configurations for different spins, eccentricities, mass ratios, compactnesses, and equations of state. For this purpose we employ the SGRID code, which allows us to construct such data in previously inaccessible regions of the parameter space. In particular, we consider spinning neutron stars in isolation and in binary systems; we incorporate new methods to produce highly eccentric and eccentricity-reduced data; we present the possibility of computing data for significantly unequal-mass binaries with mass ratios q ≃ 2; and we create equal-mass binaries with individual compactness up to C ≃ 0.23. As a proof of principle, we explore the dynamical evolution of three new configurations. First, we simulate a q ¼ 2.06 mass ratio which is the highest mass ratio for a binary neutron star evolved in numerical relativity to date. We find that mass transfer from the companion star sets in a few revolutions before merger and a rest mass of ∼10 −2 M ⊙ is transferred between the two stars. This amount of mass accretion corresponds to ∼10 51 ergs of accretion energy. This configuration also ejects a large amount of material during merger (∼7.6 × 10 −2 M ⊙ ), imparting a substantial kick to the remnant neutron star. Second, we simulate the first merger of a precessing binary neutron star. We present the dominant modes of the gravitational waves for the precessing simulation, where a clear imprint of the precession is visible in the (2,1) mode. Finally, we quantify the effect of an eccentricity-reduction procedure on the gravitational waveform. The procedure improves the waveform quality and should be employed in future precision studies. However, one also needs to reduce other errors in the waveforms, notably truncation errors, in order for the improvement due to eccentricity reduction to be effective.

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Relativistic Binaries in Globular Clusters

Cited by 198 publications

References 443 publications

Sources of Gravitational Waves: Theory and Observations

Sources of Gravitational Waves: Theory and Observations

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of the stars’ rotation

Binary neutron stars with generic spin, eccentricity, mass ratio, and compactness: Quasi-equilibrium sequences and first evolutions

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