141 research outputs found
Thermohaline instabilities inside stars: a synthetic study including external turbulence and radiative levitation
We have derived a new expression for the thermohaline mixing coefficient in
stars, including the effects of radiative levitation and external turbulence,
by solving Boussinesq equations in a quasi-incompressible fluid with a linear
approximation. It is well known that radiative levitation of individual
elements can lead to their accumulation in specific stellar layers. In some
cases, it can induce important effects on the stellar structure. Here we
confirm that this accumulation is moderated by thermohaline convection due to
the resulting inverse -gradient. The new coefficient that we have derived
shows that the effect of radiative accelerations on the thermohaline
instability itself is small. This effect must however be checked in all
computations. We also confirm that the presence of large horizontal turbulence
can reduce or even suppress the thermohaline convection. These results are
important as they concern all the cases of heavy element accumulation in stars.
The computations of radiative diffusion have to be revisited including
thermohaline convection and its consequences. It may be one of the basic
reasons for the fact that the observed abundances are always smaller than those
predicted by pure atomic diffusion. In any case, these processes have to
compete with rotation-induced mixing, but this competition is more complex than
previously thought due to their mutual interaction.Comment: 15 pages, 3 figures, to be published in Ap.
Comparisons for Esta-Task3: Cles and Cesam
We present the results of comparing three different implementations of the
microscopic diffusion process in the stellar evolution codes CESAM and CLES.
For each of these implementations we computed models of 1.0, 1.2 and 1.3
M. We analyse the differences in their internal structure at three
selected evolutionary stages, as well as the variations of helium abundance and
depth of the stellar convective envelope. The origin of these differences and
their effects on the seismic properties of the models are also considered.Comment: 10 pages, 8 figures, Joint HELAS and CoRoT/ESTA Workshop on
Solar/Stellar Models and Seismic Analysis Tools, Novembre, Porto 2007 To be
published in EAS Publications Serie
Asteroseismic Signatures of Helium gradients in Main-Sequence A Stars ; Application to the roAp Star HD60435
Asteroseismology is found to be a excellent tool for detecting
diffusion-induced helium gradients inside main-sequence A stars. Models have
been computed for 1.6 and 2.0 M stars with pure helium diffusion, at
different ages, so that the helium gradient lies at different depths inside the
star. The adiabatic oscillation frequencies have been analysed and compared
with those of a model without diffusion. Clear signatures of the
diffusion-induced helium gradient are found in the so-called ``second
differences" : these frequency differences present modulations due to the
partial reflexion of the sound waves on the layer where the helium gradient
takes place. A tentative application to the roAp star HD60435, which presents
enough detected oscillation frequencies for the test to be possible, is very
encouraging. The results suggest the presence of a helium gradient inside the
star, which is consistent with the idea that the triggering of the oscillations
is due to the hydrogen -mechanism.Comment: to be published in A&A ; 17 pages ; 8 figure
On the lithium content of the globular cluster M92
I use literature data and a new temperature calibration to determine the Li
abundances in the globular cluster M 92. Based on the same data, Boesgaard et
al. have claimed that there is a dispersion in Li abundances in excess of
observational errors. This result has been brought as evidence for Li depletion
in metal-poor dwarfs. In the present note I argue that there is no strong
evidence for intrinsic dispersion in Li abundances, although a dispersion as
large as 0.18 dex is possible. The mean Li abundance, A(Li)=2.36, is in good
agreement with recent results for field stars and TO stars in the metal-poor
globular cluster NGC 6397. The simplest interpretation is that this constant
value represents the primordial Li abundance.Comment: A&A accepte
Asteroseismic signatures of helium gradients in late F-type stars
Element diffusion is expected to occur in all kinds of stars : according to
the relative effect of gravitation and radiative acceleration, they can fall or
be pushed up in the atmospheres. Helium sinks in all cases, thereby creating a
gradient at the bottom of the convective zones. This can have important
consequences for the sound velocity, as has been proved in the sun with
helioseismology.
We investigate signatures of helium diffusion in late F-type stars by
asteroseismology.
Stellar models were computed with different physical inputs (with or without
element diffusion) and iterated in order to fit close-by evolutionary tracks
for each mass. The theoretical oscillation frequencies were computed and
compared for pairs of models along the tracks. Various asteroseismic tests
(large separations, small separations, second differences) were used and
studied for the comparisons.
The results show that element diffusion leads to changes in the frequencies
for masses larger than 1.2 Msun. In particular the helium gradient below the
convective zone should be detectable through the second differences.Comment: 8 pages, 11 figures, 2 tables Accepted for publication in Astronomy
and Astrophysics. The official date of acceptance is 03/05/200
Abundance anomalies in pre-main-sequence stars: Stellar evolution models with mass loss
The effects of atomic diffusion on internal and surface abundances of A and F
pre-main-sequence stars with mass loss are studied in order to determine at
what age the effects materialize, as well as to further understand the
processes at play in HAeBe and young ApBp stars. Self-consistent stellar
evolution models of 1.5 to 2.8Msun with atomic diffusion (including radiative
accelerations) for all species within the OPAL opacity database were computed
and compared to observations of HAeBe stars. Atomic diffusion in the presence
of weak mass loss can explain the observed abundance anomalies of
pre-main-sequence stars, as well as the presence of binary systems with metal
rich primaries and chemically normal secondaries such as V380 Ori and HD72106.
This is in contrast to turbulence models which do not allow for abundance
anomalies to develop on the pre-main-sequence. The age at which anomalies can
appear depends on stellar mass. For A and F stars, the effects of atomic
diffusion can modify both the internal and surface abundances before the onset
of the MS. The appearance of important surface abundance anomalies on the
pre-main-sequence does not require mass loss, though the mass loss rate affects
their amplitude. Observational tests are suggested to decipher the effects of
mass loss from those of turbulent mixing. If abundance anomalies are confirmed
in pre-main-sequence stars they would severely limit the role of turbulence in
these stars.Comment: 9 pages, 6 figures, accepeted for publicatio
BD+48 740 - Li overabundant giant star with a planet. A case of recent engulfment?
We report the discovery of a unique object, BD+48 740, a lithium overabundant
giant with A(Li)=2.33 +/- 0.04 (where A(Li) = log(n_Li/n_H) + 12), that
exhibits radial velocity (RV) variations consistent with a 1.6 M_J companion in
a highly eccentric, e = 0.67 +/- 0.17 and extended, a=1.89 AU (P=771 d), orbit.
The high eccentricity of the planet is uncommon among planetary systems
orbiting evolved stars and so is the high lithium abundance in a giant star.
The ingestion by the star of a putative second planet in the system originally
in a closer orbit, could possibly allow for a single explanation to these two
exceptional facts. If the planet candidate is confirmed by future RV
observations, it might represent the first example of the remnant of a multiple
planetary system possibly affected by stellar evolution.Comment: 14 pages, 2 figures, accepted to ApJ Letter
Be abundances in cool main-sequence stars with exoplanets
We present new UVES spectra of a sample of 15 cool unevolved stars with and
without detected planetary companions. Together with previous determinations,
we study Be depletion and possible differences in Be abundances between both
groups of stars. We obtain a final sample of 89 and 40 stars with and without
planets, respectively, which covers a wide range of effective temperatures,
from 4700 K to 6400 K, and includes several cool dwarf stars for the first
time. We determine Be abundances for these stars and find that for most of them
(the coolest ones) the BeII resonance lines are often undetectable, implying
significant Be depletion. While for hot stars Be abundances are aproximately
constant, with a slight fall as Teff decreases and the Li-Be gap around 6300 K,
we find a steep drop of Be content as Teff decreases for Teff < 5500 K,
confirming the results of previous papers. Therefore, for these stars there is
an unknown mechanism destroying Be that is not reflected in current models of
Be depletion. Moreover, this strong Be depletion in cool objects takes place
for all the stars regardless of the presence of planets, thus, the effect of
extra Li depletion in solar-type stars with planets when compared with stars
without detected planets does not seem to be present for Be, although the
number of stars at those temperatures is still small to reach a final
conclusion.Comment: Accepted for publication in Ap
Low abundances of heavy elements in the solar outer layers: comparisons of solar models with helioseismic inversions
Recent solar photospheric abundance analyses have led to a significant
reduction of the metal abundances compared to the previous determinations. The
solar models computed with standard opacities and diffusion processes using
these new abundances give poor agreement with helioseismic inversions for the
sound-speed profile, the surface helium abundance, and the convective zone
depth.
We attempt to obtain a good agreement between helioseismic inversions and
solar models which present the "old" mixture in the interior and new chemical
composition in the convective zone. To reach this result, we assume an
undermetallic accretion at the beginning of the main sequence.
We compute solar models with the Toulouse-Geneva Evolution Code, in which we
simulate an undermetallic accretion in the early stages of the main sequence,
in order to obtain new mixture in the outer convective zone. We compare the
sound-speed profile, the convective zone depth, and the surface helium
abundance with those deduced from helioseismology.
The model with accretion but without any mixing process inside is in better
agreement with helioseismology than the solar model with the new abundances
throughout. There is, however, a spike under the convective zone which reaches
3.4%. Furthermore, the convective zone depth and the surface helium abundance
are too low. Introducing undershooting below the convective zone allows us to
recover the good convective zone radius and the addition of rotation-induced
mixing and tachocline allows us to reconcile the surface helium abundance. But
in any case the agreement of the sound-speed profile with helioseismic
inference is worse than obtained with the old abundances.Comment: 5 pages, 2 figure
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