266 research outputs found
Captures of stars by a massive black hole: Investigations in numerical stellar dynamics
Among the astrophysical systems targeted by LISA, stars on relativistic
orbits around massive black holes (MBHs) are particularly promising sources.
Unfortunately, the prediction for the number and characteristics of such
sources suffers from many uncertainties. Stellar dynamical Monte Carlo
simulations of the evolution of galactic nucleus models allow more realistic
estimates of these quantities. The computations presented here strongly suggest
that the closest such extreme mass-ratio binary to be detected by LISA could be
a low-mass MS star (MSS) orbiting the MBH at the center of our Milky Way. Only
compact stars contribute to the expected detections from other galaxies because
MSSs are disrupted by tidal forces too early.Comment: 4 pages, 2 figures, to appear in the proceedings of "The Astrophysics
of Gravitational Wave Sources", a workshop held at the University of
Maryland, April 24-26, 200
A new Monte Carlo code for star cluster simulations: II. Central black hole and stellar collisions
We have recently written a new code to simulate the long term evolution of
spherical clusters of stars. It is based on the pioneering Monte Carlo scheme
proposed by Henon in the 70's. Our code has been devised in the specific goal
to treat dense galactic nuclei. After having described how we treat relaxation
in a first paper, we go on and include further physical ingredients that are
mostly pertinent to galactic nuclei, namely the presence of a central (growing)
black hole (BH) and collisions between MS stars. Stars that venture too close
to the BH are destroyed by the tidal field. This process is a channel to feed
the BH and a way to produce accretion flares. Collisions between stars have
often been proposed as another mechanism to drive stellar matter into the
central BH. To get the best handle on the role of this process in galactic
nuclei, we include it with unpreceded realism through the use of a set of more
than 10000 collision simulations carried out with a SPH (Smoothed Particle
Hydrodynamics) code. Stellar evolution has also been introduced in a simple
way, similar to what has been done in previous dynamical simulations of
galactic nuclei. To ensure that this physics is correctly simulated, we
realized a variety of tests whose results are reported here. This unique code,
featuring most important physical processes, allows million particle
simulations, spanning a Hubble time, in a few CPU days on standard personal
computers and provides a wealth of data only rivalized by N-body simulations.Comment: 32 pages, 19 figures. Slightly shortened and clarified following
referee's suggestions. Accepted for publication in A&A. Version with high
quality figures available at
http://obswww.unige.ch/~freitag/papers/article_MC2.ps.g
Gravitational waves from eccentric intermediate-mass black hole binaries
If binary intermediate-mass black holes (IMBHs; with masses between 100 and
10^4 \Msun) form in dense stellar clusters, their inspiral will be detectable
with the planned Laser Interferometer Space Antenna (LISA) out to several Gpc.
Here we present a study of the dynamical evolution of such binaries using a
combination of direct -body techniques (when the binaries are well
separated) and three-body relativistic scattering experiments (when the
binaries are tight enough that interactions with stars occur one at a time). We
find that for reasonable IMBH masses there is only a mild effect on the
structure of the surrounding cluster even though the binary binding energy can
exceed the binding energy of the cluster. We demonstrate that, contrary to
standard assumptions, the eccentricity in the LISA band can be in {\em some}
cases as large as and that it induces a measurable phase
difference from circular binaries in the last year before merger. We also show
that, even though energy input from the binary decreases the density of the
core and slows down interactions, the total time to coalescence is short enough
(typically less than a hundred million years) that such mergers will be unique
snapshots of clustered star formation.Comment: Accepted for publication by ApJ Lett
Runaway collisions in young star clusters. II. Numerical results
We present a new study of the collisional runaway scenario to form an
intermediate-mass black hole (IMBH, MBH > 100 Msun) at the centre of a young,
compact stellar cluster. The first phase is the formation of a very dense
central core of massive stars (Mstar =~ 30-120 Msun) through mass segregation
and gravothermal collapse. Previous work established the conditions for this to
happen before the massive stars evolve off the main sequence (MS). In this and
a companion paper, we investigate the next stage by implementing direct
collisions between stars. Using a Monte Carlo stellar dynamics code, we follow
the core collapse and subsequent collisional phase in more than 100 models with
varying cluster mass, size, and initial concentration. Collisions are treated
either as ideal, ``sticky-sphere'' mergers or using realistic prescriptions
derived from 3-D hydrodynamics computations. In all cases for which the core
collapse happens in less than the MS lifetime of massive stars (~3 Myr), we
obtain the growth of a single very massive star (VMS, Mstar =~ 400-4000 Msun)
through a runaway sequence of mergers. Mass loss from collisions, even for
velocity dispersions as high as sigma1D ~ 1000 km/s, does not prevent the
runaway. The region of cluster parameter space leading to runaway is even more
extended than predicted in previous work because, in clusters with sigma1D >
300 km/s, collisions accelerate (and, in extreme cases, drive) core collapse.
Although the VMS grows rapidly to > 1000 Msun in models exhibiting runaway, we
cannot predict accurately its final mass. This is because the termination of
the runaway process must eventually be determined by a complex interplay
between stellar dynamics, hydrodynamics, and the stellar evolution of the VMS.
[abridged]Comment: 23 pages, 24 figures. For publication in MNRAS. Paper revised to
follow requests and suggestions of referee. Companion paper to Freitag, Rasio
& Baumgardt 200
A comprehensive set of simulations of high-velocity collisions between main-sequence stars
We report on a very large set of simulations of collisions between two main-sequence (MS) stars. These computations were carried out with the smoothed particle hydrodynamics method. Realistic stellar structure models for evolved MS stars were used. In order to sample an extended domain of initial parameters space (masses of the stars, relative velocity and impact parameter), more than 14 000 simulations were carried out. We considered stellar masses ranging between 0.1 and 75 Mâ and relative velocities up to a few thousand km sâ1. To limit the computational burden, a resolution of 1000-32 000 particles per star was used. The primary goal of this study was to build a complete data base from which the result of any collision can be interpolated. This allows us to incorporate the effects of stellar collisions with an unprecedented level of realism into dynamical simulations of galactic nuclei and other dense stellar clusters. We make the data describing the initial condition and outcome (mass and energy loss, angle of deflection) of all our simulations available on the Internet. We find that the outcome of collisions depends sensitively on the stellar structure and that, in most cases, using polytropic models is inappropriate. Published fitting formulae for the collision outcomes, established from a limited set of collisions, prove of limited use because they do not allow robust extrapolation to other stellar structures or relative velocitie
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