1,204 research outputs found
The mean surface density of companions in a stellar-dynamical context
Applying the mean surface density of companions, Sigma(r), to the dynamical
evolution of star clusters is an interesting approach to quantifying structural
changes in a cluster. It has the advantage that the entire density structure,
ranging from the closest binary separations, over the core-halo structure
through to the density distribution in moving groups that originate from
clusters, can be analysed coherently as one function of the stellar separations
r.
This contribution assesses the evolution of Sigma(r) for clusters with
different initial densities and binary populations. The changes in the binary,
cluster and halo branches as the clusters evolve are documented using direct
N-body calculations, and are correlated with the cluster core and half-mass
radius. The location of breaks in the slope of Sigma(r) and the possible
occurrence of a binary gap can be used to infer dynamical cluster properties.Comment: 12 pages including 7 figures, accepted for publication in A&
The mass-metallicity relation of tidal dwarf galaxies
Dwarf galaxies generally follow a mass-metallicity (MZ) relation, where more
massive objects retain a larger fraction of heavy elements. Young tidal dwarf
galaxies (TDGs), born in the tidal tails produced by interacting gas-rich
galaxies, have been thought to not follow the MZ relation, because they inherit
the metallicity of the more massive parent galaxies. We present chemical
evolution models to investigate if TDGs that formed at very high redshifts,
where the metallicity of their parent galaxy was very low, can produce the
observed MZ relation. Assuming that galaxy interactions were more frequent in
the denser high-redshift universe, TDGs could constitute an important
contribution to the dwarf galaxy population. The survey of chemical evolution
models of TDGs presented here captures for the first time an initial mass
function (IMF) of stars that is dependent on both the star formation rate and
the gas metallicity via the integrated galactic IMF (IGIMF) theory. As TDGs
form in the tidal debris of interacting galaxies, the pre-enrichment of the
gas, an underlying pre-existing stellar population, infall, and mass dependent
outflows are considered. The models of young TDGs that are created in strongly
pre-enriched tidal arms with a pre-existing stellar population can explain the
measured abundance ratios of observed TDGs. The same chemical evolution models
for TDGs, that form out of gas with initially very low metallicity, naturally
build up the observed MZ relation. The modelled chemical composition of ancient
TDGs is therefore consistent with the observed MZ relation of satellite
galaxies.Comment: 7 pages, 3 figures, MNRAS accepte
On the origin of the distribution of binary-star periods
Pre-main sequence and main-sequence binary systems are observed to have
periods, P, ranging from one day to 10^(10) days and eccentricities, e, ranging
from 0 to 1. We pose the problem if stellar-dynamical interactions in very
young and compact star clusters may broaden an initially narrow period
distribution to the observed width. N-body computations of extremely compact
clusters containing 100 and 1000 stars initially in equilibrium and in cold
collapse are preformed. In all cases the assumed initial period distribution is
uniform in the narrow range 4.5 < log10(P) < 5.5 (P in days) which straddles
the maximum in the observed period distribution of late-type Galactic-field
dwarf systems. None of the models lead to the necessary broadening of the
period distribution, despite our adopted extreme conditions that favour
binary--binary interactions. Stellar-dynamical interactions in embedded
clusters thus cannot, under any circumstances, widen the period distribution
sufficiently. The wide range of orbital periods of very young and old binary
systems is therefore a result of cloud fragmentation and immediate subsequent
magneto-hydrodynamical processes operating within the multiple proto-stellar
system.Comment: 11 pages, 4 figures, ApJ, in pres
Limits on the primordial stellar multiplicity
Most stars - especially young stars - are observed to be in multiple systems.
Dynamical evolution is unable to pair stars efficiently, which leads to the
conclusion that star-forming cores must usually fragment into \geq 2 stars.
However, the dynamical decay of systems with \geq 3 or 4 stars would result in
a large single-star population that is not seen in the young stellar
population. Additionally, ejections would produce a significant population of
hard binaries that are not observed. This leads to a strong constraint on star
formation theories that cores must typically produce only 2 or 3 stars. This
conclusion is in sharp disagreement with the results of currently available
numerical simulations that follow the fragmentation of molecular cores and
typically predict the formation of 5--10 seeds per core. In addition, open
cluster remnants may account for the majority of observed highly hierarchical
higher-order multiple systems in the field.Comment: A&A in press, 5 pages (no figures
The rotationally stabilized VPOS and predicted proper motions of the Milky Way satellite galaxies
The satellite galaxies of the Milky Way (MW) define a vast polar structure
(VPOS), a thin plane perpendicular to the MW disc. Proper motion (PM)
measurements are now available for all of the 11 brightest, `classical'
satellites and allow an updated analysis of the alignment of their orbital
poles with this spatial structure. The coherent orbital alignment of 7 to 9 out
of 11 satellites demonstrates that the VPOS is a rotationally stabilized
structure and not only a pressure-supported, flattened ellipsoid. This allows
us to empirically and model independently predict the PMs of almost all
satellite galaxies by assuming that the MW satellite galaxies orbit within the
VPOS. As a test of our method, the predictions are best met by satellites whose
PMs are already well constrained, as expected because more uncertain
measurements tend to deviate more from the true values. Improved and new PM
measurements will further test these predictions. A strong alignment of the
satellite galaxy orbital poles is not expected in dark matter based simulations
of galaxy formation. Coherent orbital directions of satellite galaxies are,
however, a natural consequence of tidal dwarf galaxies formed together in the
debris of a galaxy collision. The orbital poles of the MW satellite galaxies
therefore lend further support to tidal scenarios for the origin of the VPOS
and are a very significant challenge for the standard LCDM model of cosmology.
We also note that the dependence of the MW satellite speeds on Galactocentric
distance appear to map an effective potential with a constant velocity of
approximately 240 km/s to about 250 kpc. The individual satellite velocities
are only mildly radial.Comment: 17 pages, 8 figures, 4 tables, accepted for publication in MNRA
Evidence for the Strong Effect of Gas Removal on the Internal Dynamics of Young Stellar Clusters
We present detailed luminosity profiles of the young massive clusters M82-F,
NGC 1569-A, and NGC 1705-1 which show significant departures from equilibrium
(King and EFF) profiles. We compare these profiles with those from N-body
simulations of clusters which have undergone the rapid removal of a significant
fraction of their mass due to gas expulsion. We show that the observations and
simulations agree very well with each other suggesting that these young
clusters are undergoing violent relaxation and are also losing a significant
fraction of their stellar mass. That these clusters are not in equilibrium can
explain the discrepant mass-to-light ratios observed in many young clusters
with respect to simple stellar population models without resorting to
non-standard initial stellar mass functions as claimed for M82-F and NGC
1705-1. We also discuss the effect of rapid gas removal on the complete
disruption of a large fraction of young massive clusters (``infant
mortality''). Finally we note that even bound clusters may lose >50% of their
initial stellar mass due to rapid gas loss (``infant weight-loss'').Comment: 6 pages, 3 figures, MNRAS letters, accepte
A discontinuity in the low-mass initial mass function
The origin of brown dwarfs (BDs) is still an unsolved mystery. While the
standard model describes the formation of BDs and stars in a similar way recent
data on the multiplicity properties of stars and BDs show them to have
different binary distribution functions. Here we show that proper treatment of
these uncovers a discontinuity of the multiplicity-corrected mass distribution
in the very-low-mass star (VLMS) and BD mass regime. A continuous IMF can be
discarded with extremely high confidence. This suggests that VLMSs and BDs on
the one hand, and stars on the other, are two correlated but disjoint
populations with different dynamical histories. The analysis presented here
suggests that about one BD forms per five stars and that the BD-star binary
fraction is about 2%-3% among stellar systems.Comment: 14 pages, 11 figures, uses emulateapj.cls. Minor corrections and 1
reference added after being accepted by the Ap
The Origin of the Arches Stellar Cluster Mass Function
We investigate the time evolution of the mass distribution of pre-stellar
cores (PSCs) and their transition to the initial stellar mass function (IMF) in
the central parts of a molecular cloud (MC) under the assumption that the
coalescence of cores is important. Our aim is to explain the observed shallow
IMF in dense stellar clusters such as the Arches cluster. The initial
distributions of PSCs at various distances from the MC center are those of
gravitationally unstable cores resulting from the gravo-turbulent fragmentation
of the MC. As time evolves, there is a competition between the PSCs rates of
coalescence and collapse. Whenever the local rate of collapse is larger than
the rate of coalescence in a given mass bin, cores are collapsed into stars.
With appropriate parameters, we find that the coalescence-collapse model
reproduces very well all the observed characteristics of the Arches stellar
cluster IMF; Namely, the slopes at high and low mass ends and the peculiar bump
observed at ~5-6 M_sol. Our results suggest that today's IMF of the Arches
cluster is very similar to the primordial one and is prior to the dynamical
effects of mass segregation becoming importantComment: 5 pages, 2 figures, accepted to MNRAS Letter
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