111 research outputs found
Scandium: A key element for understanding Am stars
{\rm Context.} Atomic diffusion is believed to cause the abundance anomalies
observed in AmFm stars. However, the detailed process has still not been
well-established. For instance, two possible scenarios for the diffusion theory
are presently envisaged. They differ mainly by the depth from which the
abundance anomalies emanate. The first scenario predicts that the abundances
are modified in the superficial regions of the star, just below the hydrogen
convection zone. The second scenario predicts that a much deeper extension of
the mixing zone exists due to the convection caused by Fe accumulation in
regions below the hydrogen convection zone. {\rm Aims.} We calculate much more
accurate radiative accelerations of Sc than previously, to better understand
the observed abundance anomalies of this element. We believe that it is a key
element to use as a diagnostic tool for understanding AmFm stars.
{\rmMethods.} The method employed to obtain these radiative accelerations is
based on an interpolation from the parameters of the so-called SVP parametric
method.
{\rm Results.} The radiative accelerations, shown here in a typical Am
stellar model, are discussed in light of the observed anomalies of Ca and Sc.
Our results suggest that the deeper mixing scenario is not entirely
satisfactory: the mixing zone should be deeper than what is predicted by recent
models to account for observed Sc underabundances. Our results seem more
compatible with the scenario where the abundances anomalies are created in the
superficial regions. However, only detailed evolutionary modelling with mass
loss and diffusion of all important species, including Ca and Sc, with accurate
radiative accelerations, will be able to give more insight into where the
source of these anomalies occur in AmFm stars.Comment: 6 pages, 3 figures, accepted for publication in A&
Modelling of the scandium abundance evolution in AmFm stars
Scandium is a key element of the Am star phenomenon since its surface
under-abundance is one of the criteria that characterise such stars. Thanks to
the availability of a sufficiently complete set of theoretical atomic data for
this element, reliable radiative accelerations for Sc can now be computed,
which allows its behaviour under the action of atomic diffusion to be modelled.
We explore the required conditions, in terms of mixing processes or mass loss,
for our models to reproduce the observed surface abundances of Sc in Am stars.
The models are computed with the Toulouse-Geneva evolution code, which uses the
parametric single-valued parameter method for the calculation of radiative
accelerations. Fingering mixing is included, using a prescription that comes
from 3D hydrodynamical simulations. Other parameter-dependent turbulent mixing
processes are also considered. A global mass loss is also implemented. When no
mass loss is considered, the observed abundances of Sc are rather in favour of
the models whose superficial layers are fully mixed down to the iron
accumulation zone, although other mixing prescriptions are also able to
reproduce the observations for the most massive model presented here (). The models including mass loss with rates in the range of
/yr are compatible with some of the observations,
while other observations suggest that the mass-loss rate could be lower. The
constraints brought by the modelling of Sc are consistent with those derived
using other chemical elements.Comment: 9 pages, 7 figure
Dynamics of Electron Transport in Cytochrome P450 Systems Studied at Sub-Zero Temperature
Experimentation in fluid mixed solvents (1 : 1 v/v phosphate
buffer ethylene glycol) at sub-zero temperatures has permitted us
to record the two univalent reductions of the bacterial cytochrome
P450 by the natural electron donor putidaredoxin, without recycling
or alternative pathway reactions. Dynamic evidence shows the formation of putidaredoxincytochrome complexes prior to electron
transfer. The complex formation is rate limiting in the first reduction
and in our experimental conditions. The kinetics of binding
between the two oxidized proteins has also been recorded in the
same medium under various conditions of concentration, temperature
and ionic strength. At very low ionic strength, the rate is
limited by electrostatic repulsion between the two negatively charge
proteins; above I = 0.03 this effect appears negligible and the affinity
seems to be governed by hydrophobic interaction free energy
Dynamics of Electron Transport in Cytochrome P450 Systems Studied at Sub-Zero Temperature
Experimentation in fluid mixed solvents (1 : 1 v/v phosphate
buffer ethylene glycol) at sub-zero temperatures has permitted us
to record the two univalent reductions of the bacterial cytochrome
P450 by the natural electron donor putidaredoxin, without recycling
or alternative pathway reactions. Dynamic evidence shows the formation of putidaredoxincytochrome complexes prior to electron
transfer. The complex formation is rate limiting in the first reduction
and in our experimental conditions. The kinetics of binding
between the two oxidized proteins has also been recorded in the
same medium under various conditions of concentration, temperature
and ionic strength. At very low ionic strength, the rate is
limited by electrostatic repulsion between the two negatively charge
proteins; above I = 0.03 this effect appears negligible and the affinity
seems to be governed by hydrophobic interaction free energy
Modelling element distributions in the atmospheres of magnetic Ap stars
In recent papers convincing evidence has been presented for chemical
stratification in Ap star atmospheres, and surface abundance maps have been
shown to correlate with the magnetic field direction. Radiatively driven
diffusion in magnetic fields is among the processes responsible for these
inhomogeneities. Here we explore the hypothesis that equilibrium
stratifications can, in a number of cases, explain the observed abundance maps
and vertical distributions of the various elements. The investigation of
equilibrium stratifications in stellar atmospheres with temperatures from 8500K
to 12000K and fields up to 10 kG reveals considerable variations in the
vertical distribution of the 5 elements studied (Mg, Si, Ca, Ti, Fe), often
with zones of large over- or under-abundances and with indications of other
competing processes (such as mass loss). Horizontal magnetic fields can be very
efficient in helping the accumulation of elements in higher layers. A
comparison between our calculations and the vertical abundance profiles and
surface maps derived by magnetic Doppler imaging reveals that equilibrium
stratifications are in a number of cases consistent with the main trends
inferred from observed spectra. However, it is not clear whether such
equilibrium solutions will ever be reached during the evolution of an Ap star.Comment: 7 pages, 6 figures, the paper will be published in Astronomy &
Astrophysics, on November 200
Radiative diffusion in stellar atmospheres: diffusion velocities
The present paper addresses some of the problems in the buildup of element
stratification in stellar magnetic atmospheres due to microscopic diffusion, in
particular the redistribution of momentum among the various ionisation stages
of a given element and the calculation of diffusion velocities in the presence
of inclined magnetic fields.
We have considerably modified and extended our CARAT code to provide
radiative accelerations, not only from bound-bound but also from bound-free
transitions. In addition, our code now computes ionisation and recombination
rates, both radiative and collisional. These rates are used in calculating the
redistribution of momentum among the various ionisation stages of the chemical
elements. A careful comparison shows that the two different theoretical
approaches to redistribution that are presently available lead to widely
discrepant results for some chemical elements, especially in the magnetic case.
In the absence of a fully satisfactory theory of redistribution, we propose to
use the geometrical mean of the radiative accelerations from both methods.
Diffusion velocities have been calculated for 28 chemical elements in a T_eff
= 12000K, log g = 4.00 stellar magnetic atmosphere with solar abundances.
Velocities and resulting element fluxes in magnetic fields are discussed; rates
of abundance changes are analysed for systematic trends with field strength and
field direction. Special consideration is given to the Si case and our results
are confronted in detail with well-known results derived more than two decades
ago.Comment: To be published in Astronomy & Astrophysics (accepted 02/03/2006
AmFm and lithium gap stars: Stellar evolution models with mass loss
A thorough study of the effects of mass loss on internal and surface
abundances of A and F stars is carried out in order to constrain mass loss
rates for these stars, as well as further elucidate some of the processes which
compete with atomic diffusion. Self-consistent stellar evolution models of 1.3
to 2.5 M_sun stars including atomic diffusion and radiative accelerations for
all species within the OPAL opacity database were computed with mass loss and
compared to observations as well as previous calculations with turbulent
mixing. Models with unseparated mass loss rates between 5 x 10^-14 and 10^-13
M_sun/yr reproduce observations for many cluster AmFm stars as well as Sirius A
and o Leonis. These models also explain cool Fm stars, but not the Hyades
lithium gap. Like turbulent mixing, these mass loss rates reduce surface
abundance anomalies; however, their effects are very different with respect to
internal abundances. For most of the main sequence lifetime of an A or F star,
surface abundances in the presence of such mass loss depend on separation which
takes place between log(Delta M/M_star)= -6 and -5. The current observational
constraints do not allow us to conclude that mass loss is to be preferred over
turbulent mixing (induced by rotation or otherwise) in order to explain the
AmFm phenomenon. Internal concentration variations which could be detectable
through asteroseismic tests should provide further information. If atomic
diffusion coupled with mass loss are to explain the Hyades Li gap, the wind
would need to be separated.Comment: 27 pages, 25 figures, accepted for publication in A&
Late stages of the evolution of A-type stars on the main sequence: comparison between observed chemical abundances and diffusion models for 8 Am stars of the Praesepe cluster
Aims. We aim to provide observational constraints on diffusion models that
predict peculiar chemical abundances in the atmospheres of Am stars. We also
intend to check if chemical peculiarities and slow rotation can be explained by
the presence of a weak magnetic field.
Methods. We have obtained high resolution, high signal-to-noise ratio spectra
of eight previously-classified Am stars, two normal A-type stars and one Blue
Straggler, considered to be members of the Praesepe cluster. For all of these
stars we have determined fundamental parameters and photospheric abundances for
a large number of chemical elements, with a higher precision than was ever
obtained before for this cluster. For seven of these stars we also obtained
spectra in circular polarization and applied the LSD technique to constrain the
longitudinal magnetic field.
Results. No magnetic field was detected in any of the analysed stars. HD
73666, a Blue Straggler previously considered as an Ap (Si) star, turns out to
have the abundances of a normal A-type star. Am classification is not confirmed
for HD 72942. For HD 73709 we have also calculated synthetic Delta-a photometry
that is in good agreement with the observations. There is a generally good
agreement between abundance predictions of diffusion models and values that we
have obtained for the remaining Am stars. However, the observed Na and S
abundances deviate from the predictions by 0.6 dex and >0.25 dex respectively.
Li appears to be overabundant in three stars of our sample.Comment: Accepted for publication on A&
Vertical abundance stratification in the blue horizontal branch star HD135485
It is commonly believed that the observed overabundances of many chemical
species relative to the expected cluster metallicity in blue horizontal branch
(BHB) stars appear as a result of atomic diffusion in the photosphere. The slow
rotation of BHB stars (with T_eff > 11,500K), typically v sin{i} < 10 km/s, is
consistent with this idea. In this work we search for observational evidence of
vertical chemical stratification in the atmosphere of HD135485. If this
evidence exists, it will demonstrate the importance of atomic diffusion
processes in the atmospheres of BHB stars. We undertake an extensive abundance
stratification analysis of the atmosphere of HD135485, based on recently
acquired high resolution and S/N CFHT ESPaDOnS spectra and a McDonald-CE
spectrum. Our numerical simulations show that nitrogen and sulfur reveal
signatures of vertical abundance stratification in the stellar atmosphere. It
appears that the abundances of these elements increase toward the upper
atmosphere. This fact cannot be explained by the influence of microturbulent
velocity, because oxygen, carbon, neon, argon, titanium and chromium do not
show similar behavior and their abundances remain constant throughout the
atmosphere. It seems that the iron abundance may increase marginally toward the
lower atmosphere. This is the first demonstration of vertical abundance
stratification of metals in a BHB star.Comment: 8 pages, 5 figures, accepted to A&
Precise Modeling of the Exoplanet Host Star and CoRoT Main Target HD 52265
This paper presents a detailed and precise study of the characteristics of
the Exoplanet Host Star and CoRoT main target HD 52265, as derived from
asteroseismic studies. The results are compared with previous estimates, with a
comprehensive summary and discussion. The basic method is similar to that
previously used by the Toulouse group for solar-type stars. Models are computed
with various initial chemical compositions and the computed p-mode frequencies
are compared with the observed ones. All models include atomic diffusion and
the importance of radiative accelerations is discussed. Several tests are used,
including the usual frequency combinations and the fits of the \'echelle
diagrams. The possible surface effects are introduced and discussed. Automatic
codes are also used to find the best model for this star (SEEK, AMP) and their
results are compared with that obtained with the detailed method. We find
precise results for the mass, radius and age of this star, as well as its
effective temperature and luminosity. We also give an estimate of the initial
helium abundance. These results are important for the characterization of the
star-planet system.Comment: 9 pages, 6 figures, 7 tables, to be published in Astronomy and
Astrophysic
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