38 research outputs found
The Impact of Rotation on Cluster Dynamics
The evolution of rotating, isolated clusters of stars up to core-collapse is
investigated with n-body numerical codes. The simulations start off from
axisymmetric generalisations of King profiles, with added global angular
momentum. In this contribution I report on results obtained for two sets of
single-mass cluster simulations. These confirm the more rapid evolution of even
mildly-rotating clusters. A model is presented with rotational energy
comparable to omega-Centauri's; it reaches core-collapse in less than half the
time required for non-rotating model clusters.Comment: Talk given at the Strasbourg meeting Massive Star Clusters in
November 1999; 7 pages, 3 figures xv-8bit giffed and tarred (= 100Kbytes);
newpasp style file include
Evolution of star clusters in arbitrary tidal fields
We present a novel and flexible tensor approach to computing the effect of a
time-dependent tidal field acting on a stellar system. The tidal forces are
recovered from the tensor by polynomial interpolation in time. The method has
been implemented in a direct-summation stellar dynamics integrator (NBODY6) and
test-proved through a set of reference calculations: heating, dissolution time
and structural evolution of model star clusters are all recovered accurately.
The tensor method is applicable to arbitrary configurations, including the
important situation where the background potential is a strong function of
time. This opens up new perspectives in stellar population studies reaching to
the formation epoch of the host galaxy or galaxy cluster, as well as for
star-burst events taking place during the merger of large galaxies. A pilot
application to a star cluster in the merging galaxies NGC 4038/39 (the
Antennae) is presented.Comment: 12 pages, 8 figures. Accepted for publication in MNRA
Hubble-Lema\^itre fragmentation and the path to equilibrium of merger-driven cluster formation
This paper discusses a new method to generate self-coherent initial
conditions for young substructured stellar cluster. The expansion of a uniform
system allows stellar sub-structures (clumps) to grow from fragmentation modes
by adiabatic cooling. We treat the system mass elements as stars, chosen
according to a Salpeter mass function, and the time-evolution is performed with
a collisional N-body integrator. This procedure allows to create a
fully-coherent relation between the clumps' spatial distribution and the
underlying velocity field. The cooling is driven by the gravitational field, as
in a cosmological Hubble-Lema\^itre flow. The fragmented configuration has a
`fractal'-like geometry but with a self-grown velocity field and mass profile.
We compare the characteristics of the stellar population in clumps with that
obtained from hydrodynamical simulations and find a remarkable correspondence
between the two in terms of the stellar content and the degree of spatial
mass-segregation. In the fragmented configuration, the IMF power index is ~0.3
lower in clumps in comparison to the field stellar population, in agreement
with observations in the Milky Way. We follow in time the dynamical evolution
of fully fragmented and sub-virial configurations, and find a soft collapse,
leading rapidly to equilibrium (timescale of 1 Myr for a ~ 10^4 Msun system).
The low-concentration equilibrium implies that the dynamical evolution
including massive stars is less likely to induce direct collisions and the
formation of exotic objects. Low-mass stars already ejected from merging clumps
are depleted in the end-result stellar clusters, which harbour a top-heavy
stellar mass function.Comment: 22 pages, accepted for publication in MNRA
The effects of bar-spiral coupling on stellar kinematics in the Galaxy
We investigate models of the Milky Way disc taking into account
simultaneously the bar and a two-armed quasi-static spiral pattern. Away from
major resonance overlaps, the mean stellar radial motions in the plane are
essentially a linear superposition of the isolated effects of the bar and
spirals. Thus, provided the bar is strong enough, even in the presence of
spiral arms, these mean radial motions are predominantly affected by the
Galactic bar for large scale velocity fluctuations. This is evident when
comparing the peculiar line-of-sight velocity power spectrum of our coupled
models with bar-only models. However, we show how forthcoming spectroscopic
surveys could disentangle bar-only non-axisymmetric models of the Galaxy from
models in which spiral arms have a significant amplitude. We also point out
that overlaps of low-order resonances are sufficient to enhance stellar
churning within the disc, even when the spirals amplitude is kept constant.
Nevertheless, for churning to be truly non-local, stronger or (more likely)
transient amplitudes would be needed: otherwise the disc is actually mostly
unaffected by churning in the present models. Finally, regarding vertical
breathing modes, the combined effect of the bar and spirals on vertical motions
is a clear non-linear superposition of the isolated effects of both components,
significantly superseding the linear superposition of modes produced by each
perturber separately, thereby providing an additional effect to consider when
analysing the observed breathing mode of the Galactic disc in the extended
Solar neighbourhood.Comment: 13 pages, 12 figures. MNRAS. Accepted for publication. v2 is the
published versio
Search for and investigation of new stellar clusters using the data from huge stellar catalogues
We present new automatic methods of search for star clusters using the data
available in new huge stellar catalogues. Using 2MASS catalogue we have
discovered over ten new open clusters in the region of Galaxy anticenter and
determined their physical parameters.Comment: Proceedings of the 79th Annual Scientific Meeting of the
Astronomische Gesellschaft, Cologne(Germany), September 200
Satellite decay in flattened dark matter haloes
We carry out a set of self-consistent N-body calculations to compare the
decay rates of satellite dwarf galaxies orbiting a disc galaxy embedded in a
dark matter halo (DMH). We consider both spherical and oblate axisymmetric DMHs
of aspect ratio q_h=0.6. The satellites are given different initial orbital
inclinations, orbital periods and mass. The live flattened DMHs with embedded
discs and bulges are set-up using a new fast algorithm, MaGalie (Boily, Kroupa
and Pe\~{n}arrubia 2001).
We find that the range of survival times of satellites within a flattened DMH
becomes of the order of 100% larger than the same satellites within a spherical
DMH. In the oblate DMH, satellites on polar orbits have the longest survival
time, whereas satellites on coplanar prograde orbits are destroyed most
rapidly. The orbital plane of a satellite tilts as a result of anisotropic
dynamical friction, causing the satellite's orbit to align with the plane of
symmetry of the DMH. Polar orbits are not subjected to alignment. Therefore the
decay of a satellites in an axisymmetric DMH may provide a natural explanation
for the observed lack of satellites within (0-30) degrees of their host
galaxy's disc (Holmberg 1969; Zaritsky and Gonz\'alez 1999).
The computations furthermore indicate that the evolution of the orbital
eccentricity is highly dependent of its initial value e(t=0) and the DMH's
shape. We also discuss some implications of flattened DMHs for satellite debris
streams.Comment: 13 pages, 9 figures. Accepted by MNRA
Disk galaxies are self-similar: the universality of the HI-to-Halo mass ratio for isolated disks
Observed scaling relations in galaxies between baryons and dark matter global
properties are key to shed light on the process of galaxy formation and on the
nature of dark matter. Here, we study the scaling relation between the neutral
hydrogen (HI) and dark matter mass in isolated rotationally-supported disk
galaxies at low redshift. We first show that state-of-the-art galaxy formation
simulations predict that the HI-to-dark halo mass ratio decreases with stellar
mass for the most massive disk galaxies. We then infer dark matter halo masses
from high-quality rotation curve data for isolated disk galaxies in the local
Universe, and report on the actual universality of the HI-to-dark halo mass
ratio for these observed galaxies. This scaling relation holds for disks
spanning a range of 4 orders of magnitude in stellar mass and 3 orders of
magnitude in surface brightness. Accounting for the diversity of rotation curve
shapes in our observational fits decreases the scatter of the HI-to-dark halo
mass ratio while keeping it constant. This finding extends the previously
reported discrepancy for the stellar-to-halo mass relation of massive disk
galaxies within galaxy formation simulations to the realm of neutral atomic
gas. Our result reveals that isolated galaxies with regularly rotating extended
HI disks are surprisingly self-similar up to high masses, which hints at
mass-independent self-regulation mechanisms that have yet to be fully
understood.Comment: 14 pages, 4 figures. Accepted for publication in ApJ
The mass-to-light ratio of rich star clusters
We point out a strong time-evolution of the mass-to-light conversion factor
eta commonly used to estimate masses of unresolved star clusters from observed
cluster spectro-photometric measures. We present a series of gas-dynamical
models coupled with the Cambridge stellar evolution tracks to compute
line-of-sight velocity dispersions and half-light radii weighted by the
luminosity. We explore a range of initial conditions, varying in turn the
cluster mass and/or density, and the stellar population's IMF. We find that
eta, and hence the estimated cluster mass, may increase by factors as large as
3 over time-scales of 50 million years. We apply these results to an hypothetic
cluster mass distribution function (d.f.) and show that the d.f. shape may be
strongly affected at the low-mass end by this effect. Fitting truncated
isothermal (Michie-King) models to the projected light profile leads to
over-estimates of the concentration parameter c of delta c ~ 0.3 compared to
the same functional fit applied to the projected mass density.Comment: 6 pages, 2 figures, to appear in the proceedings of the "Young
massive star clusters", Granada, Spain, September 200