Binary Mergers and Growth of Black Holes in Dense Star Clusters

Oct 1, 2005 - successive mergers of BHs lead to the growth and retention of .... Another possibility that favors the retention of large ..... the powe...

0 downloads 18 Views 647KB Size

Recommend Documents

Nov 13, 2016 - ABSTRACT. Recent N-body simulations predict that large numbers of stellar black holes (BHs) could remain bound ... synthesis models for the field, where results are very sensitive to many uncertain parameters in the initial binary ....

Apr 17, 2008 - times well under a Hubble time, and escape speeds that are several .... Studies of main sequence binaries in globular clusters, which have.

son & Hernquist 1993) and has been demonstrated recently by direct N-body simulations .... was quite angry when much later in 1969 Lynden-Bell was given credit for the idea after a ... star” in the Galactic Center Quintuplet cluster (Figer et al.

Feb 22, 2012 - Consequently, favourable configurations are initiated through the Kozai mechanism where ec- centricity growth is possible for long-lived triple ...

Jun 21, 2016 - are the sites of feedback processes, and likely drive the BH-host scaling relations. 3.1. Triggering of ... a few extreme outliers of very massive BHs in low-mass host galaxies have been reported recently .... the blazar OJ 287 with it

Feb 3, 2010 - 1Harvard-Smithsonian Center for Astrophysics, Cambridge, USA, 2University of Oxford, UK,. 3ESO, Garching ... FIGURE 1. MMT 6.5m optical spectrum of the NGC 404 nuclear cluster (black line) with the best fit ... material from the disk of

May 7, 2012 - 2 Interactive Research Center of Science, Tokyo Institute of. Technology .... in the cluster center. We discuss more details in section. 3.1. We additionally performed simulations of a single model with the same parameters as single-w6

Apr 17, 2012 - Irr. Taniguchi. [300] CTS. Spectral. Physical. C = 0.1 − 0.3. 0.7 – 1.0. Irr. Ury¯u. [311] WL/NHS. Multipatch Γ = 3, Physical. C = 0.13 − 0.22 1.0. Irr. 24 ...... [2] Abbott, B.P. et al. (LIGO Scientific Collaboration), “Sear

Feb 10, 2011 - Auriga association have much higher binary frequencies (see. Duchêne 1999, and references therein). This leads to the ques- tion of what ...

Oct 1, 2018 - Trajectories are shaded to indicate the passage of time; darker shades ..... (light band) represent the median, 50%, and 90% credible regions.

the MBH binary hard enough that they can merge through gravitational wave radiation. So far, theories and numerical simulations ... one month, on a single-host, 4-processor-board GRAPE-6 system with the peak speed of 4 Tflops. 3. Results.

Dec 24, 2004 - star clusters throughout the local universe. These systems are large and young enough that they contain statistically significant numbers .... detailed evolution and ultimate fate of stars hundreds or thousands of times more massive th

Dec 24, 2004 - relation r = 3m1/2, then for the object to reach m » 103 in 3 Myr (to form .... Thrall, A. P., Deneva, J. S., Fleming, S. W., & Grabowski, P. E. 2003,.

Jun 29, 2010 - Conversely, the fastest merging model shows that rotation is quickly lost ... 2136/NGC 2137, in the Large Magellanic Cloud. .... server. This research has made use of the WEBDA database operated at the Institute of. Astronomy of the Un

May 2, 2012 - ABSTRACT. A promising mechanism to form intermediate-mass black holes (IMBHs) is the runaway merger in dense star clusters, where main-sequence stars collide and form a very massive star (VMS), which then collapses to a black hole. In t

Mar 12, 2012 - initially developed to improve the accuracy of black hole bi- nary mergers. The choice of how to modify .... In this paper, we are interested in the behavior of BHNS bi- naries for high mass ratio q = MBH/MNS ..... ment of Ontario; Ont

Aug 14, 2018 - Askar, Arca Sedda & Giersz 2018; Arca Sedda, Askar, & Giersz. 2018). The retention of a large number of BHs can significantly influence not ...

Mar 12, 2012 - eration of ground-based detectors, Advanced LIGO [1] and. VIRGO [2]. Indeed, whether for ... tion is limited by the minimum spacing of the numerical grid ..... We pre- fer to choose the free data (gij,K) according to the prescrip-.

The present model is most similar to recent models in McKee & Offner (2010),. OM11, Myers (2010), and ..... present-day protostar mass functions depends on accretion start times as discussed in. Section 2.3. This subsection ... where all stars start

Abstract. A model of core-clump accretion with equally likely stopping describes star formation in the dense parts of clusters, where models of isolated collapsing ...

Oct 30, 2012 - Email: [email protected] Devecchi .... For each simulation, we evolved 2000 binaries, one at a time, ...... NS retention fraction Pfahl et al.

Feb 5, 2008 - They measured a very large sample of Magellanic Cloud clusters .... lanic Cloud clusters possess radial surface brightness pro- ...... It is enlight-.

Feb 5, 2008 - In this study we present the results from realistic N-body modelling of massive star clusters in the Magellanic Clouds. We have computed eight simulations with N ~ 105 particles; six of these were evolved for at least a Hubble time. The

Feb 5, 2008 - GRAPE-6 special purpose computer (Makino et al. 2003) at ..... NGC 330), as well as in the Galaxy (e.g., Orion Nebula. Cluster, Arches ...