Maximum Kick from Nonspinning Black-Hole Binary Inspiral

González, José Antonio García-Cruces; Sperhake, Ulrich; Brügmann, Bernd; Hannam, M. D.; Husa, S.

doi:10.1103/physrevlett.98.091101

Cited by 515 publications

(701 citation statements)

References 39 publications

Supporting

Mentioning

659

Contrasting

Order By: Relevance

“…According to numerical relativity results, when two spinning black holes collide, gravitational radiation could be emitted asymmetrically. This would lead to a recoil velocity in the resulting black hole that might be as high as 4000 km s −1 (Gonzalez et al 2007;Campanelli et al 2007b,a;Healy et al 2009;Herrmann et al 2007), depending on the mass ratio of the initial black holes and the directions of their spins, but this velocity might be significantly suppressed by the relativistic alignment of the spins (Kesden et al 2010). It is not easy, of course to include numerical relativity in an N-body code, but semi-analytical formulae, coming from fitting between numerical relativity results and post-Newtonian theory (Lousto & Zlochower 2008;Baker et al 2008;Lousto et al 2010) to determine the direction and magnitude of the recoil velocity.…”

Section: Discussionmentioning

confidence: 99%

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

Konstantinidis

Kokkotas

2010

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Discussionmentioning

confidence: 99%

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

Konstantinidis

Kokkotas

2010

A&A

View full text Add to dashboard Cite

show abstract

“…More recently, progress in numerical relativity (NR) [6][7][8] has allowed relativists to simulate the mergers of highly spinning, comparable-mass black holes. For non-spinning binaries, ensuing studies identified a maximum recoil of 175 km/s [9]. Simulations of spinning black holes, however, resulted in one of the greatest surprises of numerical relativity; for equal-mass binaries with opposite spins in the orbital plane gravitational recoils can * berti@phy.olemiss.edu † mhk10@nyu.edu ‡ sperhake@tapir.caltech.edu approach 4,000 km/s [10,11], greater than the escape velocity of even the most massive galaxies.…”

Section: Introductionmentioning

confidence: 99%

“…For non-spinning binaries, ensuing studies identified a maximum recoil of 175 km/s [9]. Simulations of spinning black holes, however, resulted in one of the greatest surprises of numerical relativity; for equal-mass binaries with opposite spins in the orbital plane gravitational recoils can * berti@phy.olemiss.edu † mhk10@nyu.edu ‡ sperhake@tapir.caltech.edu approach 4,000 km/s [10,11], greater than the escape velocity of even the most massive galaxies. This theoretical result seems at first difficult to reconcile with observations indicating that almost all large galaxies host SBHs.…”

Section: Introductionmentioning

confidence: 99%

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

2012

Self Cite

View full text Add to dashboard Cite

Recent numerical relativity simulations have shown that the final black hole produced in a binary merger can recoil with a velocity as large as 5, 000 km/s. Because of enhanced gravitational-wave emission in the so-called "hang-up" configurations, this maximum recoil occurs when the black-hole spins are partially aligned with the orbital angular momentum. We revisit our previous statistical analysis of post-Newtonian evolutions of black-hole binaries in the light of these new findings. We demonstrate that despite these new configurations with enhanced recoil velocities, spin alignment during the post-Newtonian stage of the inspiral will still significantly suppress (or enhance) kick magnitudes when the initial spin of the more massive black hole is more (or less) closely aligned with the orbital angular momentum than that of the smaller hole. We present a preliminary study of how this post-Newtonian spin alignment affects the ejection probabilities of supermassive black holes from their host galaxies with astrophysically motivated mass ratio and initial spin distributions. We find that spin alignment suppresses (enhances) ejection probabilities by ∼ 40% (20%) for an observationally motivated mass-dependent galactic escape velocity, and by an even greater amount for a constant escape velocity of 1,000 km/s. Kick suppression is thus at least a factor two more efficient than enhancement.

show abstract

“…For instance, Baker et al (2008) modeled the coalescence of nonspinning BHs with different mass ratios. Also, González et al (2007) and Campanelli et al (2007) studied the cases with general spin orientations. These simulations show that for mergers with BHs of low spins or the spins aligned, the maximum speeds of the kick are below 200 km s −1 .…”

Section: Discussionmentioning

confidence: 99%

Long gamma ray bursts from binary black holes

Janiuk

Charzyński

Bejger

2013

A&A

View full text Add to dashboard Cite

Aims. We consider a scenario for the longest duration gamma ray bursts, resulting from the collapse of a massive rotating star in a close binary system with a companion black hole (BH). Methods. The primary BH born during the core collapse is first being spun up and increases its mass during the fallback of the stellar envelope just after its birth. As the companion BH enters the outer envelope, it provides an additional angular momentum to the gas. After the infall and spiral-in toward the primary, the two BHs merge inside the circumbinary disk. Results. The second episode of mass accretion and high final spin of the postmerger BH prolongs the gamma ray burst central engine activity. The observed events should have two distinct peaks in the electromagnetic signal, separated by the gravitational wave emission. The gravitational recoil of the burst engine is also possible.

show abstract

Maximum Kick from Nonspinning Black-Hole Binary Inspiral

Cited by 515 publications

References 39 publications

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

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

Effects of post-Newtonian spin alignment on the distribution of black-hole recoils

Long gamma ray bursts from binary black holes

Contact Info

Product

Resources

About