23,824 research outputs found
Searching for chemical inhomogeneities in Open Clusters: Analysis of the CN and CH Molecular Band Strengths in NGC 2158, NGC 2420, NGC 2682, NGC 7789 and Berkeley 29
Context: The total mass of a cluster, being the main parameter determining
its ability to host more than one stellar generation, may constitute a
threshold below which the cluster is able to form only a single stellar
population. AIms: Our goal is to investigate the existence of star-to-star
variations of CN and CH band strengths, related to the N and C abundances,
respectively, among the stars in five open cluster (NGC 2158, NGC 2420, NGC
2682, NGC 7789 and Berkeley 29) similar to those observed in globular clusters
and linked with the existence of multiple populations therein. Since these
systems are less massive than globulars, our results may allow us to constrain
the lower mass necessary to form more than one stellar population. Methods: We
measured the strength of the CN and CH bands, which correlate with the C and N
abundances, using four molecular indices in low-resolution SDSS/SEGUE spectra.
Results: We found that for four of the open clusters (NGC 2158, NGC 2420, NGC
2682 and Berkeley 29) all the stars studied in each of them have similar CN and
CH band strengths within the uncertainties since neither anomalous spreads nor
bimodalities have been detected in their CN and CH distributions. In contrast,
for NGC 7789 we found an anomalous spread in the strength of the CN molecular
band at 3839 \AA which is larger than the uncertainties. However, the small
number of stars studied in this cluster implies that further analysis is needed
to confirm the existence of chemical inhomogeneities in this cluster.Comment: 11 pages, 9 figures, Accepted for publication in A&A, Tables 7, 8 and
9 will be publish onlin
A Turbulent Model for the Interstellar Medium. II. Magnetic Fields and Rotation
We present results from two-dimensional numerical simulations of a supersonic
turbulent flow in the plane of the galactic disk, incorporating shear,
thresholded and discrete star formation (SF), self-gravity, rotation and
magnetic fields. A test of the model in the linear regime supports the results
of the linear theory of Elmegreen (1991). In the fully nonlinear turbulent
regime, while some results of the linear theory persist, new effects also
emerge. Some exclusively nonlinear effects are: a) Even though there is no
dynamo in 2D, the simulations are able to maintain or increase their net
magnetic energy in the presence of a seed uniform azimuthal component. b) A
well-defined power-law magnetic spectrum and an inverse magnetic cascade are
observed in the simulations, indicating full MHD turbulence. Thus, magnetic
field energy is generated in regions of SF and cascades up to the largest
scales. c) The field has a slight but noticeable tendency to be aligned with
density features. d) The magnetic field prevents HII regions from expanding
freely, as in the recent results of Slavin \& Cox (1993). e) A tendency to
exhibit {\it less} filamentary structures at stronger values of the uniform
component of the magnetic field is present in several magnetic runs. f) For
fiducial values of the parameters, the flow in general appears to be in rough
equipartition between magnetic and kinetic energy. There is no clear domination
of either the magnetic or the inertial forces. g) A median value of the
magnetic field strength within clouds is G, while for the
intercloud medium a value of G is found. Maximum contrasts of up to
a factor of are observed.Comment: Plain TeX file, 25 pages. Gzipped, tarred set of Tex file plus 17
figures and 3 tables (Postscript) available at
ftp://kepler.astroscu.unam.mx/incoming/enro/papers/mhdgturb.tar.g
Highly Compressible MHD Turbulence and Gravitational Collapse
We investigate the properties of highly compressible turbulence and its
ability to produce self-gravitating structures. The compressibility is
parameterized by an effective polytropic exponent gama-eff. In the limit of
small gama-eff, the density jump at shocks is shown to be of the order of
e^{M^2}, and the production of vorticity by the nonlinear terms appears to be
negligible. In the presence of self-gravity, we suggest that turbulence can
produce bound structures for gama-eff < 2(1-1/n), where 'n' is the typical
dimensionality of the turbulent compressions. We show, by means of numerical
simulations, that, for sufficiently small gama-eff, small-scale turbulent
density fluctuations eventually collapse even though the medium is globally
stable. This result is preserved in the presence of a magnetic field for
supercritical mass-to-flux ratios.Comment: 4 pages, 3 postscript figures. Latex, uses aipproc.sty Contribution
to the Conference Proc. of the 7th Annual Astrophysics Conference in
Maryland, STAR FORMATION, NEAR AND FAR, eds. Stephen S. Holt and Lee G. Mund
Perturbation theory in a pure exchange non-equilibrium economy
We develop a formalism to study linearized perturbations around the equilibria of a pure exchange economy. With the use of mean field theory techniques, we derive equations for the flow of products in an economy driven by heterogeneous preferences and probabilistic interaction between agents. We are able to show that if the economic agents have static preferences, which are also homogeneous in any of the steady states, the final wealth distribution is independent of the dynamics of the non-equilibrium theory. In particular, it is completely determined in terms of the initial conditions, and it is independent of the probability, and the network of interaction between agents. We show that the main effect of the network is to determine the relaxation time via the usual eigenvalue gap as in random walks on graphs.non-equilibrium economics; perturbation theory
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