217 research outputs found
Atomic Diffusion and Mixing in Old Stars I. VLT/FLAMES-UVES Observations of Stars in NGC 6397
We present a homogeneous photometric and spectroscopic analysis of 18 stars
along the evolutionary sequence of the metal-poor globular cluster NGC 6397
([Fe/H] = -2), from the main-sequence turnoff point to red giants below the
bump. The spectroscopic stellar parameters, in particular stellar-parameter
differences between groups of stars, are in good agreement with broad-band and
Stroemgren photometry calibrated on the infrared-flux method. The spectroscopic
abundance analysis reveals, for the first time, systematic trends of iron
abundance with evolutionary stage. Iron is found to be 31% less abundant in the
turnoff-point stars than in the red giants. An abundance difference in lithium
is seen between the turnoff-point and warm subgiant stars. The impact of
potential systematic errors on these abundance trends (stellar parameters, the
hydrostatic and LTE approximations) is quantitatively evaluated and found not
to alter our conclusions significantly. Trends for various elements (Li, Mg,
Ca, Ti and Fe) are compared with stellar-structure models including the effects
of atomic diffusion and radiative acceleration. Such models are found to
describe the observed element-specific trends well, if extra (turbulent) mixing
just below the convection zone is introduced. It is concluded that atomic
diffusion and turbulent mixing are largely responsible for the sub-primordial
stellar lithium abundances of warm halo stars. Other consequences of atomic
diffusion in old metal-poor stars are also discussed.Comment: 20 pages (emulateapj), 11 figures, accepted for publication in Ap
The solar photospheric abundance of carbon.Analysis of atomic carbon lines with the CO5BOLD solar model
The use of hydrodynamical simulations, the selection of atomic data, and the
computation of deviations from local thermodynamical equilibrium for the
analysis of the solar spectra have implied a downward revision of the solar
metallicity. We are in the process of using the latest simulations computed
with the CO5BOLD code to reassess the solar chemical composition. We determine
the solar photospheric carbon abundance by using a radiation-hydrodynamical
CO5BOLD model, and compute the departures from local thermodynamical
equilibrium by using the Kiel code. We measure equivalent widths of atomic CI
lines on high resolution, high signal-to-noise ratio solar atlases. Deviations
from local thermodynamic equilibrium are computed in 1D with the Kiel code. Our
recommended value for the solar carbon abundance, relies on 98 independent
measurements of observed lines and is A(C)=8.50+-0.06, the quoted error is the
sum of statistical and systematic error. Combined with our recent results for
the solar oxygen and nitrogen abundances this implies a solar metallicity of
Z=0.0154 and Z/X=0.0211. Our analysis implies a solar carbon abundance which is
about 0.1 dex higher than what was found in previous analysis based on
different 3D hydrodynamical computations. The difference is partly driven by
our equivalent width measurements (we measure, on average, larger equivalent
widths with respect to the other work based on a 3D model), in part it is
likely due to the different properties of the hydrodynamical simulations and
the spectrum synthesis code. The solar metallicity we obtain from the CO5BOLD
analyses is in slightly better agreement with the constraints of
helioseismology than the previous 3D abundance results. (Abridged)Comment: Astronomy and Astrophysics, accepte
Spectroscopic abundance analysis of dwarfs in young open cluster IC 4665
We report a detailed spectroscopic abundance analysis for a sample of 18 F-K
dwarfs of the young open cluster IC 4665. Stellar parameters and element
abundances of Li, O, Mg, Si, Ca, Ti, Cr, Fe and Ni have been derived using the
spectroscopic synthesis tool SME (Spectroscopy Made Easy). Within the
measurement uncertainties the iron abundance is uniform with a standard
deviation of 0.04 dex. No correlation is found between the iron abundance and
the mass of the stellar convective zone, and between the Li abundance and the
Fe abundance. In other words, our results do not reveal any signature of
accretion and therefore do not support the scenario that stars with planets
(SWPs) acquire their on the average higher metallicity compared to field stars
via accretion of metal-rich planetary material. Instead the higher metallicity
of SWPs may simply reflect the fact that planet formation is more efficient in
high metallicity environs. However, since that many details of the planet
system formation processes remain poorly understood, further studies are needed
for a final settlement of the problem of the high metallicity of SWPs.
The standard deviation of [Fe/H] deduced from our observations, taken as an
upper limit on the metallicity dispersion amongst the IC 4665 member stars, has
been used to constrain proto-planetary disk evolution, terrestrial and giant
planets formation and evolution processes. Our results do not support the
possibility that the migration of gas giants and the circularization of
terrestrial planets' orbits are regulated by their interaction with a residual
population of planetesimals and dust particles.Comment: 18 pages, 6 figures, accepted for publication in Ap
Nitrogen Enrichment in Atmospheres of A- and F- Type Supergiants
Using new accurate fundamental parameters of 30 Galactic A and F supergiants,
namely their effective temperatures Teff and surface gravities log g, we
implemented a non-LTE analysis of the nitrogen abundance in their atmospheres.
It is shown that the non-LTE corrections to the N abundances increase with
Teff. The nitrogen overabundance as a general feature of this type of stars is
confirmed. A majority of the stars has a nitrogen excess [N/Fe] between 0.2 and
0.9 dex with the maximum position of the star's distribution on [N/Fe] between
0.4 and 0.7 dex. The N excesses are discussed in light of predictions for
B-type main sequence (MS) stars with rotationally induced mixing and for their
next evolutionary phase, i.e. A- and F-type supergiants that have experienced
the first dredge-up. Rotationally induced mixing in the MS progenitors of the
supergiants may be a significant cause of the nitrogen excesses. When comparing
our results with predictions of the theory developed for stars with the mixing,
we find that the bulk of the supergiants (28 of 30) show the N enrichment that
can be expected (i) either after the MS phase for stars with the initial
rotational velocities v0 = 200-400 km s-1, (ii) or after the first dredge-up
for stars with v0 = 50-400 km s-1. The latter possibility is preferred on
account of the longer lifetime for stars on red-blue loops following the first
dredge-up. Two supergiants without a discernible N enrichment, namely HR 825
and HR 7876, may be post-MS objects with the relatively low initial rotational
velocity of about 100 km s-1. The suggested range for v0 is approximately
consistent with inferences from the observed projected rotational velocities of
B-type MS stars, progenitors of A and F supergiants.Comment: 14 pages, 13 figure
A primordial star in the heart of the Lion
Context: The discovery and chemical analysis of extremely metal-poor stars
permit a better understanding of the star formation of the first generation of
stars and of the Universe emerging from the Big Bang. aims: We report the study
of a primordial star situated in the centre of the constellation Leo (SDSS
J102915+172027). method: The star, selected from the low resolution-spectrum of
the Sloan Digital Sky Survey, was observed at intermediate (with X-Shooter at
VLT) and at high spectral resolution (with UVES at VLT). The stellar parameters
were derived from the photometry. The standard spectroscopic analysis based on
1D ATLAS models was completed by applying 3D and non-LTE corrections. results:
An iron abundance of [Fe/H]=--4.89 makes SDSS J102915+172927 one of the lowest
[Fe/H] stars known. However, the absence of measurable C and N enhancements
indicates that it has the lowest metallicity, Z<= 7.40x10^{-7} (metal-mass
fraction), ever detected. No oxygen measurement was possible. conclusions: The
discovery of SDSS J102915+172927 highlights that low-mass star formation
occurred at metallicities lower than previously assumed. Even lower metallicity
stars may yet be discovered, with a chemical composition closer to the
composition of the primordial gas and of the first supernovae.Comment: To be published in A&
Formation of Zr I and II lines under non-LTE conditions of stellar atmospheres
The non-local thermodynaic equilibrium (non-LTE) line formation for the two
ions of zirconium is considered through a range of spectral types when the Zr
abundance varies from the solar value down to [Zr/H] = -3. The model atom was
built using 148 energy levels of Zr I, 772 levels of Zr II, and the ground
state of Zr III. It was shown that the main non-LTE mechnism for the minority
species Zr I is ultraviolet overionization. Non-LTE leads to systematically
depleted total absorption in the Zr I lines and positive abundance corrections,
reaching to 0.33 dex for the solar metallicity models. The excited levels of Zr
II are overpopulated relative to their thermodynamic equilibrium populations in
the line formation layers due to radiative pumping from the low-excitation
levels. As a result, the line source function exceeds the Planck function
leading to weakening the Zr II lines and positive non-LTE abundance
corrections. Such corrections grow towards lower metallicity and lower surface
gravity and reach to 0.34 dex for Teff = 5500 K, log g = 2.0, [M/H] = -2. As a
test and first application of the Zr I-Zr II model atom, Zr abundance was
determined for the Sun on the basis of 1D LTE model atmosphere. Lines of Zr I
and Zr II give consistent within the error bars non-LTE abundances, while the
difference in LTE abundances amounts to 0.28 dex. The solar abundance of
zirconium obtained with the MAFAGS solar model atmosphere is log eps(Zr) =
2.63+-0.07.Comment: published in Astron. Letters, 36, 664 (2010); Erratum was submitte
Manganese Abundances in the Globular Cluster Omega Centauri
We present manganese abundances in 10 red-giant members of the globular
cluster Omega Centauri; 8 stars are from the most metal-poor population (RGB MP
and RGB MInt1) while two targets are members of the more metal rich groups (RGB
MInt2 and MInt3). This is the first time Mn abundances have been studied in
this peculiar stellar system. The LTE values of [Mn/Fe] in Omega Cen overlap
those of Milky Way stars in the metal poor Omega Cen populations ([Fe/H] ~ -1.5
to -1.8), however unlike what is observed in Milky Way halo and disk stars,
[Mn/Fe] declines in the two more metal-rich RGB MInt2 and MInt3 targets.
Non-LTE calculations were carried out in order to derive corrections to the LTE
Mn abundances. The non-LTE results for Omega Cen in comparison with the non-LTE
[Mn/Fe] versus [Fe/H] trend obtained for the Milky Way confirm and strengthen
the conclusion that the manganese behavior in Omega Cen is distinct. These
results suggest that low-metallicity supernovae (with metallicities < -2) of
either Type II or Type Ia dominated the enrichment of the more metal-rich stars
in Omega Cen. The dominance of low-metallicity stars in the chemical evolution
of Omega Cen has been noted previously in the s-process elements where
enrichment from metal-poor AGB stars is indicated. In addition, copper, which
also has metallicity dependent yields, exhibits lower values of [Cu/Fe] in the
RGB MInt2 and MInt3 Omega Cen populations.Comment: Accepted for publication in the Ap
Subgiants as probes of galactic chemical evolution
Chemical abundances for 23 candidate subgiant stars have been derived with
the aim at exploring their usefulness for studies of galactic chemical
evolution. High-resolution spectra from ESO CAT-CES and NOT-SOFIN covered 16
different spectral regions in the visible part of the spectrum. Some 200
different atomic and molecular spectral lines have been used for abundance
analysis of about 30 elemental species. The wings of strong, pressure-broadened
metal lines were used for determination of stellar surface gravities, which
have been compared with gravities derived from Hipparcos parallaxes and
isochronic masses. Stellar space velocities have been derived from Hipparcos
and Simbad data, and ages and masses were derived with recent isochrones. Only
12 of the stars turned out to be subgiants, i.e. on the "horizontal" part of
the evolutionary track between the dwarf- and the giant stages. The abundances
derived for the subgiants correspond closely to those of dwarf stars.
With the possible exceptions of lithium and carbon we find that subgiant
stars show no "chemical" traces of post-main-sequence evolution and that they
are therefore very useful targets for studies of galactic chemical evolution.Comment: A&A LaTeX, 21 pages, 17 b/w figures, Astronomy & Astrophysics in
pres
Energy Flow in the Hadronic Final State of Diffractive and Non-Diffractive Deep-Inelastic Scattering at HERA
An investigation of the hadronic final state in diffractive and
non--diffractive deep--inelastic electron--proton scattering at HERA is
presented, where diffractive data are selected experimentally by demanding a
large gap in pseudo --rapidity around the proton remnant direction. The
transverse energy flow in the hadronic final state is evaluated using a set of
estimators which quantify topological properties. Using available Monte Carlo
QCD calculations, it is demonstrated that the final state in diffractive DIS
exhibits the features expected if the interaction is interpreted as the
scattering of an electron off a current quark with associated effects of
perturbative QCD. A model in which deep--inelastic diffraction is taken to be
the exchange of a pomeron with partonic structure is found to reproduce the
measurements well. Models for deep--inelastic scattering, in which a
sizeable diffractive contribution is present because of non--perturbative
effects in the production of the hadronic final state, reproduce the general
tendencies of the data but in all give a worse description.Comment: 22 pages, latex, 6 Figures appended as uuencoded fil
A Search for Selectrons and Squarks at HERA
Data from electron-proton collisions at a center-of-mass energy of 300 GeV
are used for a search for selectrons and squarks within the framework of the
minimal supersymmetric model. The decays of selectrons and squarks into the
lightest supersymmetric particle lead to final states with an electron and
hadrons accompanied by large missing energy and transverse momentum. No signal
is found and new bounds on the existence of these particles are derived. At 95%
confidence level the excluded region extends to 65 GeV for selectron and squark
masses, and to 40 GeV for the mass of the lightest supersymmetric particle.Comment: 13 pages, latex, 6 Figure
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