Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries

Blanchet, Luc

doi:10.12942/lrr-2002-3

Cited by 460 publications

(779 citation statements)

References 187 publications

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“…Because of the modular structure of the code, this improvement could be made by simply adding a function under the binary class. This function would calculate the appropriate post-Newtonian terms (up to 2.5 PN) for the acceleration and its first derivative, following the formalisms found in Blanchet (2002), Berentzen et al (2008), and Kupi et al (2006). Another extension that would make the binary class more complete in treating binary black holes is the inclusion of the relativistic effect of the asymmetric emission of gravitational radiation and recoil velocity, during the merging of two orbiting black holes.…”

Section: Discussionmentioning

confidence: 99%

MYRIAD: a newN-body code for simulations of star clusters

Konstantinidis

Kokkotas

2010

A&A

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Aims. We present a new C++ code for collisional N-body simulations of star clusters. Methods. The code uses the Hermite fourth-order scheme with block time steps, to advance the particles in time, while the forces and neighboring particles are computed using the GRAPE-6 board. Special treatment is used for close encounters, and binary or multiple subsystems that form either dynamically or exist in the initial configuration. The structure of the code is modular and allows the appropriate treatment of more physical phenomena, such as stellar and binary evolution, stellar collisions, and evolution of close black-hole binaries. Moreover, it can be easily modified so that the part of the code that uses GRAPE-6, could be replaced by another module that uses other accelerating-hardware such as the graphics processing units (GPUs).Results. Appropriate choice of the free parameters give a good accuracy and speed for simulations of star clusters up to and beyond core collapse. Simulations of Plummer models consisting of equal-mass stars reached core collapse at t 17 half-mass relaxation times, which compares very well with existing results, while the cumulative relative error in the energy remained below 10 −3 . Comparisons with published results of other codes for the time of core collapse for different initial conditions, show excellent agreement. Simulations of King models with an initial mass-function, similar to those found in the literature, reached core collapse at t 0.17 ± 0.05 half-mass relaxation times, which is slightly earlier than expected from previous work. Finally, the code accuracy becomes comparable to and even better than the accuracy of existing codes, when a number of close binary systems is dynamically created in a simulation. This is because of the high accuracy of the method that is used for close binary and multiple subsystems. Conclusions. The code can be used for evolving star clusters containing equal-mass stars or star clusters with an initial mass function (IMF) containing an intermediate mass black hole (IMBH) at the center and/or a fraction of primordial binaries, which are systems of particular astrophysical interest.

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Section: Discussionmentioning

confidence: 99%

MYRIAD: a newN-body code for simulations of star clusters

Konstantinidis

Kokkotas

2010

A&A

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“…This can easily be done, but the results should be considered only as an indication of what may happen in reality. Indeed, in order to correctly generalize the results, the perturbative approach should be improved in many ways: the geodesic equation which are used to describe the motion of m 0 should be replaced by the correct equations of motion of a two-body system, as seen in the coordinate system centered on one star; these equations are now known at the 3.5 PN level [17], and they would change the stress energy tensor we put on the right-hand side of our equations; the problem of chosing the reference frame in which to compute the radiated power as seen by a distant observer is a very delicate one, and in order to compare the results of the perturbative approach for equal masses with those of the post-newtonian approach one should change to a frame centered in the center of mass of the binary system; in computing the orbital evolution due to radiation reaction effects it is customary to use the adiabatic approximation which assumes that the timescale of the orbital evolution is larger than the orbital period; we think that the role of this assumption has to be investigated very carefully during the last few cycles before coalescence. All of these problems are important: we are looking for very small effects which arise just before coalescence, and they may introduce corrections of a few percents in the emitted power, which are of the same order as the effects of stellar structure we discuss in this paper.…”

Section: On the Validity Of The Perturbative Approachmentioning

confidence: 99%

Gravitational signals emitted by a point mass orbiting a neutron star: Effects of stellar structure

et al. 2002

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The effects that the structure of a neutron star would have on the gravitational emission of a binary system are studied in a perturbative regime, and in the frequency domain. Assuming that a neutron star is perturbed by a point mass moving on a close, circular orbit, we solve the equations of stellar perturbations in general relativity to evaluate the energy lost by the system in gravitational waves. We compare the energy output obtained for different stellar models with that found by assuming that the perturbed object is a black hole with the same mass, and we discuss the role played by the excitation of the stellar modes. Our results indicate that the stellar structure begins to affect the emitted power when the orbital velocity is v > ∼ 0.2 c (ν GW > ∼ 185 Hz for a binary system composed of two 1.4M ⊙ neutron stars). We show that the differences between different stellar models and a black hole are due mainly to the excitation of the quasinormal modes of the star. Finally, we discuss to what extent and up to which distance the perturbative approach can be used to describe the interaction of a star and a pointlike massive body.

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“…Gravitational waves from the inspiral stage are quasi-periodic "chirp" signals of increasing frequency and amplitude which are well described by analytical postNewtonian (PN) models [5][6][7][8] before the binary evolution reaches the inner-most stable circular orbit (ISCO). Near the ISCO, the strong gravitational interaction no longer allows for a stable orbit and the two black holes merge together to form a single black hole.…”

Section: Introductionmentioning

confidence: 99%

Search for gravitational waves from intermediate mass binary black holes

Abadie¹,

Abbott²,

Abbott³

et al. 2012

Phys. Rev. D

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We present the results of a weakly modeled burst search for gravitational waves from mergers of non-spinning intermediate mass black holes (IMBH) in the total mass range 100-450 M and with the component mass ratios between 1:1 and 4:1. The search was conducted on data collected by the LIGO and Virgo detectors between November of 2005 and October of 2007. No plausible signals were observed by the search which constrains the astrophysical rates of the IMBH mergers as a function of the component masses. In the most efficiently detected bin centered on 88 + 88 M , for non-spinning sources, the rate density upper limit is 0.13 per Mpc 3 per Myr at the 90% confidence level.

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Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries

Cited by 460 publications

References 187 publications

MYRIAD: a newN-body code for simulations of star clusters

MYRIAD: a newN-body code for simulations of star clusters

Gravitational signals emitted by a point mass orbiting a neutron star: Effects of stellar structure

Search for gravitational waves from intermediate mass binary black holes

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