1,388 research outputs found
An extensive grid of DARWIN models for M-type AGB stars I. Mass-loss rates and other properties of dust-driven winds
The purpose of this work is to present an extensive grid of dynamical
atmosphere and wind models for M-type AGB stars, covering a wide range of
relevant stellar parameters. We used the DARWIN code, which includes
frequency-dependent radiation-hydrodynamics and a time-dependent description of
dust condensation and evaporation, to simulate the dynamical atmosphere. The
wind-driving mechanism is photon scattering on submicron-sized MgSiO
grains. The grid consists of models, with luminosities from
to and
effective temperatures from 2200K to 3400K. For the first time different
current stellar masses are explored with M-type DARWIN models, ranging from
0.75M to 3M. The modelling results are radial atmospheric
structures, dynamical properties such as mass-loss rates and wind velocities,
and dust properties (e.g. grain sizes, dust-to-gas ratios, and degree of
condensed Si). We find that the mass-loss rates of the models correlate
strongly with luminosity. They also correlate with the ratio :
increasing by an order of magnitude increases the mass-loss rates by
about three orders of magnitude, which may naturally create a superwind regime
in evolution models. There is, however, no discernible trend of mass-loss rate
with effective temperature, in contrast to what is found for C-type AGB stars.
We also find that the mass-loss rates level off at luminosities higher than
, and consequently at pulsation periods longer
than days. The final grain radii range from 0.25 micron to 0.6
micron. The amount of condensed Si is typically between 10% and 40%, with
gas-to-dust mass ratios between 500 and 4000.Comment: Accepted to A&A, 17 pages, 15 figure
The Core Mass Growth and Stellar Lifetime of Thermally Pulsing Asymptotic Giant Branch Stars
We establish new constraints on the intermediate-mass range of the
initial-final mass relation by studying white dwarfs in four young star
clusters, and apply the results to study the evolution of stars on the
thermally pulsing asymptotic giant branch (TP-AGB). We show that the stellar
core mass on the AGB grows rapidly from 10% to 30% for stars with = 1.6 to 2.0 . At larger masses, the core-mass growth
decreases steadily to 10% at = 3.4 . These
observations are in excellent agreement with predictions from the latest TP-AGB
evolutionary models in Marigo et al. (2013). We also compare to models with
varying efficiencies of the third dredge-up and mass loss, and demonstrate that
the process governing the growth of the core is largely the stellar wind, while
the third dredge-up plays a secondary, but non-negligible role. Based on the
new white dwarf measurements, we perform an exploratory calibration of the most
popular mass-loss prescriptions in the literature. Finally, we estimate the
lifetime and the integrated luminosity of stars on the TP-AGB to peak at
3 Myr and = 1.2 10 yr for 2 ( 2 Myr for luminosities brighter than
the RGB tip at 3.4), decreasing to = 0.4 Myr and
= 6.1 10 yr for stars with
3.5 . The implications of these results are discussed with
respect to general population synthesis studies that require correct modeling
of the TP-AGB phase of stellar evolution.Comment: 14 pages, 7 figures, 4 tables. Accepted for publication in Ap
Pre-MS depletion, accretion and primordial 7Li
We reconsider the role of pre-main sequence (pre-MS) Li depletion on the
basis of new observational and theoretical evidence: i) new observations of
Halpha emissions in young clusters show that mass accretion could be continuing
till the first stages of the MS, ii) theoretical implications from
helioseismology suggest large overshooting values below the bottom of the
convective envelopes. We argue here that a significant pre-MS 7Li destruction,
caused by efficient overshoot mixing, could be followed by a matter accretion
after 7Li depletion has ceased on MS thus restoring Li almost to the pristine
value. As a test case we show that a halo dwarf of 0.85 Msun with an extended
overshooting envelope starting with an initial abundance of A(Li) = 2.74 would
burn Li completely, but an accretion rate of the type 1e-8xe^{-t/3e6} Msun
yr would restore Li to end with an A(Li) = 2.31. A self-regulating
process is required to produce similar final values in a range of different
stellar masses to explain the PopII Spite plateau. However, this framework
could explain why open cluster stars have lower Li abundances than the
pre-solar nebula, the absence of Li in the most metal poor dwarfs and a number
of other features which lack of a satisfactory explanation.Comment: To be published in Memorie della Societ\`a Astronomica Italiana
Supplementi Vol. 22, Proceedings of Lithium in the cosmos, Iocco F.,
Bonifacio P., Vangioni E., ed
The possibility of determining open-cluster parameters from BVRI photometry
In the last decades we witnessed an increase in studies of open clusters of
the Galaxy, especially because of the good determination for a wide range of
values of parameters such as age, distance, reddening, and proper motion. The
reliable determination of the parameters strongly depends on the photometry
available and especially on the U filter, which is used to obtain the color
excess E(B-V) through the color-color diagram (U-B) by (B-V) by fitting a zero
age main-sequence. Owing to the difficulty of performing photometry in the U
band, many authors have tried to obtain E(B-V) without the filter. But because
of the near linearity of the color-color diagrams that use the other bands,
combined with the fact that most fitting procedures are highly subjective (many
done "by eye") the reliability of those results has always been questioned. Our
group has recently developed, a tool that performs isochrone fitting in
open-cluster photometric data with a global optimization algorithm, which
removes the need to visually perform the fits and thus removes most of the
related subjectivity. Here we apply our method to a set of synthetic clusters
and two observed open clusters (Trumpler 1 and Melotte 105) using only
photometry for the BVRI bands. Our results show that, considering the cluster
structural variance caused only by photometric and Poisson sampling errors, our
method is able to recover the synthetic cluster parameters with errors of less
than 10% for a wide range of ages, distances, and reddening, which clearly
demonstrates its potential. The results obtained for Trumpler 1 and Melotte 105
also agree well with previous literature values.Comment: 5 pages, 5 figures, accepted for publication in
Astronomy&Astrophysic
Catching the fish - Constraining stellar parameters for TX Psc using spectro-interferometric observations
Stellar parameter determination is a challenging task when dealing with
galactic giant stars. The combination of different investigation techniques has
proven to be a promising approach. We analyse archive spectra obtained with the
Short-Wavelength-Spectrometer (SWS) onboard of ISO, and new interferometric
observations from the Very Large Telescope MID-infrared Interferometric
instrument (VLTI/MIDI) of a very well studied carbon-rich giant: TX Psc. The
aim of this work is to determine stellar parameters using spectroscopy and
interferometry. The observations are used to constrain the model atmosphere,
and eventually the stellar evolutionary model in the region where the tracks
map the beginning of the carbon star sequence. Two different approaches are
used to determine stellar parameters: (i) the 'classic' interferometric
approach where the effective temperature is fixed by using the angular diameter
in the N-band (from interferometry) and the apparent bolometric magnitude; (ii)
parameters are obtained by fitting a grid of state-of-the-art hydrostatic
models to spectroscopic and interferometric observations. We find a good
agreement between the parameters of the two methods. The effective temperature
and luminosity clearly place TX Psc in the carbon-rich AGB star domain in the
H-R-diagram. Current evolutionary tracks suggest that TX Psc became a C-star
just recently, which means that the star is still in a 'quiet' phase compared
to the subsequent strong-wind regime. This is in agreement with the C/O ratio
being only slightly larger than 1.Comment: 11 pages, 9 figures, 5 table
Evolution and Yields of Extremely Metal Poor Intermediate Mass Stars
Intermediate mass stellar evolution tracks from the main sequence to the tip
of the AGB for five initial masses (2 to 6Msun) and metallicity Z=0.0001 have
been computed. The detailed 1D structure and evolution models include
exponential overshooting, mass loss and a detailed nucleosynthesis network with
updated nuclear reaction rates. The network includes a two-particle heavy
neutron sink for approximating neutron density in the He-shell flash. It is
shown how the neutron-capture nucleosynthesis is important in models of very
low metallicity for the formation of light neutron-heavy species, like sodium
or the heavy neon and magnesium isotopes. The models have high resolution, as
required for modeling the third dredge-up. All sequences have been followed
from the pre-main sequence to the end of the AGB when all envelope mass is
lost. Detailed structural and chemical model properties as well as yields are
presented. This set of stellar models is based on standard assumptions and
updated input physics. It can be confronted with observations of
extremely-metal poor stars and may be used to assess the role of AGB stars in
the origin of abundance anomalies of some Globular Cluster members of
correspondingly low metallicity.Comment: 40 pages, 11 figures, to appear in ApJS, including 5 electronic
table
Carbon Nitrogen, and Oxygen Galactic Gradients: A Solution to the Carbon Enrichment Problem
Eleven models of Galactic chemical evolution, differing in the carbon,
nitrogen,and oxygen yields adopted, have been computed to reproduce the
Galactic O/H values obtained from H II regions. All the models fit the oxygen
gradient, but only two models fit also the carbon gradient, those based on
carbon yields that increase with metallicity due to stellar winds in massive
stars (MS) and decrease with metallicity due to stellar winds in low and
intermediate mass stars (LIMS). The successful models also fit the C/O versus
O/H evolution history of the solar vicinity obtained from stellar observations.
We also compare the present day N/H gradient and the N/O versus O/H and the
C/Fe, N/Fe, O/Fe versus Fe/H evolution histories of the solar vicinity
predicted by our two best models with those derived from H II regions and from
stellar observations. While our two best models fit the C/H and O/H gradients
as well as the C/O versus O/H history, only Model 1 fits well the N/H gradient
and the N/O values for metal poor stars but fails to fit the N/H values for
metal rich stars. Therefore we conclude that our two best models solve the C
enrichment problem, but that further work needs to be done on the N enrichment
problem. By adding the C and O production since the Sun was formed predicted by
Models 1 and 2 to the observed solar values we find an excellent agreement with
the O/H and C/H values of the solar vicinity derived from H II regions O and C
recombination lines. One of the most important results of this paper is that
the fraction of carbon due to MS and LIMS in the interstellar medium is
strongly dependent on time and on the galactocentric distance; at present about
half of the carbon in the interstellar medium of the solar vicinity has been
produced by MS and half by LIMS.Comment: 34 pages, 6 tables, 7 figures. Accepted for publication in Ap
Mutations in splicing factor PRPF3, causing retinal degeneration, form detrimental aggregates in photoreceptor cells.
PRPF3 is an element of the splicing machinery ubiquitously expressed, yet mutations in this gene are associated with a tissue-specific phenotype: autosomal dominant retinitis pigmentosa (RP). Here, we studied the subcellular localization of endogenous- and mutant-transfected PRPF3. We found that (i) subcellular distribution of the endogenous wild-type protein co-localizes with small nuclear ribonucleoproteins, partially with a nucleolar marker and accumulates in speckles labeled by SC35; (ii) in human retinas, PRPF3 does not show a distinctive abundance in photoreceptors, the cells affected in RP and (iii) the RP causing mutant PRPF3, differently from the wild-type protein, forms abnormally big aggregates in transfected photoreceptor cells. Aggregation of T494M mutant PRPF3 inside the nucleus triggers apoptosis only in photoreceptor cells. On the basis of the observation that mutant PRPF3 accumulates in the nucleolus and that transcriptional, translational and proteasome inhibition can induce this phenomenon in non-photoreceptor cells, we hypothesize that mutation affects splicing factor recycling. Noteworthy, accumulation of the mutant protein in big aggregates also affects distribution of some other splicing factors. Our data suggest that the mutant protein has a cell-specific dominant effect in rod photoreceptors while appears not to be harmful to epithelial and fibroblast cells
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