27,017 research outputs found
Stellar evolution with rotation X: Wolf-Rayet star populations at solar metallicity
We examine the properties of Wolf--Rayet (WR) stars predicted by models of
rotating stars taking account of the new mass loss rates for O--type stars and
WR stars (Vink et al. \cite{Vink00}, \cite{Vink01}; Nugis & Lamers
\cite{NuLa00}) and of the wind anisotropies induced by rotation. We find that
the rotation velocities of WR stars are modest, i.e. about 50 km s,
not very dependant on the initial and masses. For the most massive stars,
the evolution of is very strongly influenced by the values of the mass loss
rates; below 12 M the evolution of rotation during the MS phase
and later phases is dominated by the internal coupling. Massive stars with
extreme rotation may skip the LBV phase.
Models having a typical for the O--type stars have WR lifetimes on the
average two times longer than for non--rotating models. The increase of the WR
lifetimes is mainly due to that of the H--rich eWNL phase. Rotation allows a
transition WN/WC phase to be present for initial masses lower than 60
M. The durations of the other WR subphases are less affected by
rotation. The mass threshold for forming WR stars is lowered from 37 to 22
M for typical rotation. The comparisons of the predicted number ratios
WR/O, WN/WC and of the number of transition WN/WC stars show very good
agreement with models with rotation, while this is not the case for models with
the present--day mass loss rates and no rotation. As to the chemical abundances
in WR stars, rotation brings only very small changes for WN stars, since they
have equilibrium CNO values. However, WC stars with rotation have on average
lower C/He and O/He ratios. The luminosity distribution of WC stars is also
influenced by rotation.Comment: 17 pages, 20 figures, accepted for publication in A&
Stellar evolution with rotation XI: Wolf-Rayet star populations at different metallicities
Grids of models of massive stars ( 20 ) with rotation are
computed for metallicities ranging from that of the Small Magellanic Cloud
(SMC) to that of the Galactic Centre. The hydrostatic effects of rotation, the
rotational mixing and the enhancements of the mass loss rates by rotation are
included. The evolution of the surface rotational velocities of the most
massive O--stars mainly depends on the mass loss rates and thus on the initial
value. The minimum initial mass for a star for entering the Wolf--Rayet
(WR) phase is lowered by rotation. For all metallicities, rotating stars enter
the WR phase at an earlier stage of evolution and the WR lifetimes are
increased, mainly as a result of the increased duration of the eWNL phase.
Models of WR stars predict in general rather low rotation velocities (
km s) with a few possible exceptions, particularly at metallicities
lower than solar where WR star models have in general faster rotation and more
chance to reach the break--up limit.The properties of the WR populations as
predicted by the rotating models are in general in much better agreement with
the observations in nearby galaxies. The observed variation with metallicity of
the fractions of type Ib/Ic supernovae with respect to type II supernovae as
found by Prantzos & Boissier (\cite{Pr03}) is very well reproduced by the
rotating models, while non--rotating models predict much too low ratios.Comment: 20 pages, 16 figure, Astronomy and Astrophysics, in pres
Copulas in finance and insurance
Copulas provide a potential useful modeling tool to represent the dependence structure
among variables and to generate joint distributions by combining given marginal
distributions. Simulations play a relevant role in finance and insurance. They are used to
replicate efficient frontiers or extremal values, to price options, to estimate joint risks, and so
on. Using copulas, it is easy to construct and simulate from multivariate distributions based
on almost any choice of marginals and any type of dependence structure. In this paper we
outline recent contributions of statistical modeling using copulas in finance and insurance.
We review issues related to the notion of copulas, copula families, copula-based dynamic and
static dependence structure, copulas and latent factor models and simulation of copulas.
Finally, we outline hot topics in copulas with a special focus on model selection and
goodness-of-fit testing
The chemical enrichment of the ICM from hydrodynamical simulations
The study of the metal enrichment of the intra-cluster and inter-galactic
media (ICM and IGM) represents a direct means to reconstruct the past history
of star formation, the role of feedback processes and the gas-dynamical
processes which determine the evolution of the cosmic baryons. In this paper we
review the approaches that have been followed so far to model the enrichment of
the ICM in a cosmological context. While our presentation will be focused on
the role played by hydrodynamical simulations, we will also discuss other
approaches based on semi-analytical models of galaxy formation, also critically
discussing pros and cons of the different methods. We will first review the
concept of the model of chemical evolution to be implemented in any
chemo-dynamical description. We will emphasise how the predictions of this
model critically depend on the choice of the stellar initial mass function, on
the stellar life-times and on the stellar yields. We will then overview the
comparisons presented so far between X-ray observations of the ICM enrichment
and model predictions. We will show how the most recent chemo-dynamical models
are able to capture the basic features of the observed metal content of the ICM
and its evolution. We will conclude by highlighting the open questions in this
study and the direction of improvements for cosmological chemo-dynamical models
of the next generation.Comment: 25 pages, 11 figures, accepted for publication in Space Science
Reviews, special issue "Clusters of galaxies: beyond the thermal view",
Editor J.S. Kaastra, Chapter 18; work done by an international team at the
International Space Science Institute (ISSI), Bern, organised by J.S.
Kaastra, A.M. Bykov, S. Schindler & J.A.M. Bleeke
Fluctuations and correlations in an individual-based model of biological coevolution
We extend our study of a simple model of biological coevolution to its
statistical properties. Staring with a complete description in terms of a
master equation, we provide its relation to the deterministic evolution
equations used in previous investigations. The stationary states of the
mutationless model are generally well approximated by Gaussian distributions,
so that the fluctuations and correlations of the populations can be computed
analytically. Several specific cases are studied by Monte Carlo simulations,
and there is excellent agreement between the data and the theoretical
predictions.Comment: 25 pages, 2 figure
Muon Catalyzed Fusion in 3 K Solid Deuterium
Muon catalyzed fusion in deuterium has traditionally been studied in gaseous
and liquid targets. The TRIUMF solid-hydrogen-layer target system has been used
to study the fusion reaction rates in the solid phase of D_2 at a target
temperature of 3 K. Products of two distinct branches of the reaction were
observed; neutrons by a liquid organic scintillator, and protons by a silicon
detector located inside the target system. The effective molecular formation
rate from the upper hyperfine state of and the hyperfine transition
rate have been measured: , and .
The molecular formation rate is consistent with other recent measurements, but
not with the theory for isolated molecules. The discrepancy may be due to
incomplete thermalization, an effect which was investigated by Monte Carlo
calculations. Information on branching ratio parameters for the s and p wave
d+d nuclear interaction has been extracted.Comment: 19 pages, 11 figures, submitted to PRA Feb 20, 199
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