30,229 research outputs found
On-line determination of stellar atmospheric parameters Teff, log g, [Fe/H] from ELODIE echelle spectra. II - The library of F5 to K7 stars
A library of 211 echelle spectra taken with ELODIE at the Observatoire de
Haute-Provence is presented. It provides a set of spectroscopic standards
covering the full range of gravities and metallicities in the effective
temperature interval [4000 K, 6300 K]. The spectra are straightened, wavelength
calibrated, cleaned of cosmic ray hits, bad pixels and telluric lines. They
cover the spectral range [440 nm, 680 nm] with an instrumental resolution of
42000. For each star, basic data were compiled from the Hipparcos catalogue and
the Hipparcos Input Catalogue. Radial velocities with a precision better than
100 m/s are given. Atmospheric parameters (Teff, log g, [Fe/H]) from the
literature are discussed. Because of scattered determinations in the
bibliography, even for the most well-known stars, these parameters were
adjusted by an iterative process which takes account of common or different
spectral features between the standards, using our homogeneous set of spectra.
Revised values of (Teff, log g, [Fe/H]) are proposed. They are still consistent
with the literature, and also lead to the self-consistency of the library, in
the sense that similar spectra have similar atmospheric parameters. This
adjustment was performed by using step by step a method based on the least
square comparison of carefully prepared spectra, which was originally developed
for the on-line estimation of the atmospheric parameters of faint field stars
(companion paper in the main journal). The spectra and corresponding data will
only be available in electronic form at the CDS (ftp cdsarc.u-strasbg.fr or
http://cdsweb.u-strasbg.fr/Abstract.html).Comment: 7 pages, 7 figures, accepted for publication in A&A Supplement Serie
Magmatic intrusions control Io's crustal thickness
Io, the most volcanically active body in the solar system, loses heat through
eruptions of hot lava. Heat is supplied by tidal heating and is thought to be
transferred through the mantle by magmatic segregation, a mode of transport
that sets it apart from convecting terrestrial planets. We present a model that
couples magmatic transport of tidal heat to the volcanic system in the crust,
in order to determine the controls on crustal thickness, magmatic intrusions,
and eruption rates. We demonstrate that magmatic intrusions are a key component
of Io's crustal heat balance; around 80% of the magma delivered to the base of
the crust must be emplaced and frozen as plutons to match rough estimates of
crustal thickness. As magma ascends from a partially molten mantle into the
crust, a decompacting boundary layer forms, which can explain inferred
observations of a high-melt-fraction region.Comment: Accepted to JGR:Planets. 24 pages inc appendices and references. 7
figure
Integral Constraints On cosmological Perturbations and their Energy
We show the relation between Traschen's integral equations and the energy,
and ``position of the centre of mass'', of the matter perturbations in a
Robertson-Walker spacetime. When the perturbations are ``localised'' we get a
set of integral constraints that includes hers. We illustrate them on a simple
example.Comment: 19 pages, Tex file, submitted to Classical and Quantum Gravit
The growth of galaxies in cosmological simulations of structure formation
We use hydrodynamic simulations to examine how the baryonic components of
galaxies are assembled, focusing on the relative importance of mergers and
smooth accretion in the formation of ~L_* systems. In our primary simulation,
which models a (50\hmpc)^3 comoving volume of a Lambda-dominated cold dark
matter universe, the space density of objects at our (64-particle) baryon mass
resolution threshold, M_c=5.4e10 M_sun, corresponds to that of observed
galaxies with L~L_*/4. Galaxies above this threshold gain most of their mass by
accretion rather than by mergers. At the redshift of peak mass growth, z~2,
accretion dominates over merging by about 4:1. The mean accretion rate per
galaxy declines from ~40 M_sun/yr at z=2 to ~10 M_sun/yr at z=0, while the
merging rate peaks later (z~1) and declines more slowly, so by z=0 the ratio is
about 2:1. We cannot distinguish truly smooth accretion from merging with
objects below our mass resolution threshold, but extrapolating our measured
mass spectrum of merging objects, dP/dM ~ M^a with a ~ -1, implies that
sub-resolution mergers would add relatively little mass. The global star
formation history in these simulations tracks the mass accretion rate rather
than the merger rate. At low redshift, destruction of galaxies by mergers is
approximately balanced by the growth of new systems, so the comoving space
density of resolved galaxies stays nearly constant despite significant mass
evolution at the galaxy-by-galaxy level. The predicted merger rate at z<~1
agrees with recent estimates from close pairs in the CFRS and CNOC2 redshift
surveys.Comment: Submitted to ApJ, 35 pp including 15 fig
Temporal evolution of mesoscopic structure of some non-Euclidean systems using a Monte Carlo model
A Monte Carlo based computer model is presented to comprehend the contrasting
observations of Mazumder et al. [Phys. Rev. Lett. 93, 255704 (2004) and Phys.
Rev. B 72, 224208 (2005)], based on neutron-scattering measurements, on
temporal evolution of effective fractal dimension and characteristic length for
hydration of cement with light and heavy water. In this context, a theoretical
model is also proposed to elucidate the same.Comment: 31 Pages, 13 Figure
On the Evolutionary History of Stars and their Fossil Mass and Light
The total extragalactic background radiation can be an important test of the
global star formation history (SFH). Using direct observational estimates of
the SFH, along with standard assumptions about the initial mass function (IMF),
we calculate the total extragalactic background radiation and the observed
stellar density today. We show that plausible SFHs allow a significant range in
each quantity, but that their ratio is very tightly constrained. Current
estimates of the stellar mass and extragalactic background are difficult to
reconcile, as long as the IMF is fixed to the Salpeter slope above 1 Msun. The
joint confidence interval of these two quantities only agrees with that
determined from the allowed range of SFH fits at the 3-sigma level, and for our
best-fit values the discrepancy is about a factor of two. Alternative energy
sources that contribute to the background, such as active galactic nuclei
(AGN), Population III stars, or decaying particles, appear unlikely to resolve
the discrepancy. However, changes to the IMF allow plausible solutions to the
background problem. The simplest is an average IMF with an increased
contribution from stars around 1.5--4 Msun. A ``paunchy'' IMF of this sort
could emerge as a global average if low mass star formation is suppressed in
galaxies experiencing rapid starbursts. Such an IMF is consistent with
observations of star-forming regions, and would help to reconcile the fossil
record of star formation with the directly observed SFH.Comment: 21 pages, 7 figures, 3 tables; submitted to Monthly Notice
Gravitational energy
Observers at rest in a stationary spacetime flat at infinity can measure
small amounts of rest-mass+internal energies+kinetic energies+pressure energy
in a small volume of fluid attached to a local inertial frame. The sum of these
small amounts is the total "matter energy" for those observers. The total
mass-energy minus the matter energy is the binding gravitational energy.
Misner, Thorne and Wheeler evaluated the gravitational energy of a
spherically symmetric static spacetime. Here we show how to calculate
gravitational energy in any static and stationary spacetime for isolated
sources with a set of observers at rest.
The result of MTW is recovered and we find that electromagnetic and
gravitational 3-covariant energy densities in conformastatic spacetimes are of
opposite signs. Various examples suggest that gravitational energy is negative
in spacetimes with special symmetries or when the energy-momentum tensor
satisfies usual energy conditions.Comment: 12 pages. Accepted for publication in Class. Quantum Gra
Thermodynamics of a black hole in a cavity
We present a unified thermodynamical description of the configurations
consisting on self-gravitating radiation with or without a black hole. We
compute the thermal fluctuations and evaluate where will they induce a
transition from metastable configurations towards stable ones. We show that the
probability of finding such a transition is exponentially small. This indicates
that, in a sequence of quasi equilibrium configurations, the system will remain
in the metastable states till it approaches very closely the critical point
beyond which no metastable configuration exists. Near that point, we relate the
divergence of the local temperature fluctuations to the approach of the
instability of the whole system, thereby generalizing the usual fluctuations
analysis in the cases where long range forces are present. When angular
momentum is added to the cavity, the above picture is slightly modified.
Nevertheless, at high angular momentum, the black hole loses most of its mass
before it reaches the critical point at which it evaporates completely.Comment: 27 pages, latex file, contains 3 figures available on request at
[email protected]
- …