1,012 research outputs found
Fingering Convection in Red Giants Revisited
Fingering (thermohaline) convection has been invoked for several years as a
possible extra-mixing which could occur in Red Giant stars due to the
modification of the chemical composition induced by nuclear reactions in the
hydrogen burning zone. Recent studies show however that this mixing is not
sufficient to account for the needed surface abundances. A new prescription for
fingering convection, based on 3D numerical simulations has recently been
proposed (BGS). The resulting mixing coefficient is larger than the ones
previously given in the literature. We compute models using this new
coefficient and compare them to previous studies. We use the LPCODE stellar
evolution code with the GNA generalized version of the mixing length theory to
compute Red Giant models and we introduce fingering convection using the BGS
prescription. The results show that, although the fingering zone now reaches
the outer dynamical convective zone, the efficiency of the mixing is not enough
to account for the observations. The fingering mixing coefficient should be
increased by two orders of magnitude for the needed surface abundances to be
reached. We confirm that fingering convection cannot be the mixing process
needed to account for surface abundances in RGB stars.Comment: Accepted for publication in Astronomy and Astrophysic
Traitement de la schistosomiase à S. mansoni : quelle alternative au praziquantel ?
Les schistosomiases sont des maladies parasitaires causées par des helminthes du genre Schistosoma (S.) qui touchent 200 millions de personnes dans le monde, mais restent rares chez le voyageur. Contrairement à S. heamatobium, agent de la bilharziose urinaire, S. mansoni, présent en Afrique subsaharienne, en Egypte ainsi qu'aux Antilles, au Surinam et dans le nordest du Brésil, est responsable des formes hépato-intestinales de la maladie. Les larves, vivant en eaux douces contaminées par des selles infectées, peuvent pénétrer la peau des baigneurs sans que l'individu ne s'en rende compte. Les parasites adultes s'établissent dans le système veineux digestif où ils se reproduisent et excrètent des oeufs qui migreront dans la lumière intestinale. Cette revue systématique évalue les effets des médicaments antibilharziens, utilisés seuls ou en association, pour traiter l'infection à S. mansoni
The roles of poly(ADP-ribose)-metabolizing enzymes in alkylation-induced cell death
Abstract.: Poly(ADP-ribose) (PAR) has been identified as a DNA damage-inducible cell death signal upstream of apoptosis-inducing factor (AIF). PAR causes the translocation of AIF from mitochondria to the nucleus and triggers cell death. In living cells, PAR molecules are subject to dynamic changes pending on internal and external stress factors. Using RNA interference (RNAi), we determined the roles of poly(ADP-ribose) polymerases-1 and -2 (PARP-1, PARP-2) and poly(ADP-ribose) glycohydrolase (PARG), the key enzymes configuring PAR molecules, in cell death induced by an alkylating agent. We found that PARP-1, but not PARP-2 and PARG, contributed to alkylation-induced cell death. Likewise, AIF translocation was only affected by PARP-1. PARP-1 seems to play a major role configuring PAR as a death signal involving AIF translocation regardless of the death pathway involve
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Thermohaline mixing and the photospheric composition of low-mass giant stars
We compute full evolutionary sequences of red giant branch stars close to the
luminosity bump by including state of the art composition transport
prescriptions for the thermohaline mixing regimes. In particular we adopt a
self-consistent double-diffusive convection theory, that allows to handle the
instabilities that arise when thermal and composition gradients compete against
each other, and a very recent empirically motivated and parameter free
asymptotic scaling law for thermohaline composition transport. In agreement
with previous works, we find that during the red giant stage, a thermohaline
instability sets in shortly after the hydrogen burning shell (HBS) encounters
the chemical discontinuity left behind by the first dredge-up. We also find
that the thermohaline unstable region, initially appearing at the exterior wing
of the HBS, is unable to reach the outer convective envelope, with the
consequence that no mixing of elements that produces a non-canonical
modification of the stellar surface abundances occurs. Also in agreement with
previous works, we find that by artificially increasing the mixing efficiency
of thermohaline regions it is possible to connect both unstable regions, thus
affecting the photospheric composition. However, we find that in order to
reproduce the observed abundances of red giant branch stars close to the
luminosity bump, thermohaline mixing efficiency has to be artificially
increased by about 4 orders of magnitude from that predicted by recent 3D
numerical simulations of thermohaline convection close to astrophysical
environments. From this we conclude the chemical abundance anomalies of red
giant stars cannot be explained on the basis of thermohaline mixing alone.Comment: 7 pages, 6 figures, accepted for publication in A&
Revisiting the theoretical DBV (V777 Her) instability strip: the MLT theory of convection
We reexamine the theoretical instability domain of pulsating DB white dwarfs
(DBV or V777 Her variables). We performed an extensive -mode nonadiabatic
pulsation analysis of DB evolutionary models considering a wide range of
stellar masses, for which the complete evolutionary stages of their progenitors
from the ZAMS, through the thermally pulsing AGB and born-again phases, the
domain of the PG1159 stars, the hot phase of DO white dwarfs, and then the DB
white dwarf stage have been considered. We explicitly account for the evolution
of the chemical abundance distribution due to time-dependent chemical diffusion
processes. We examine the impact of the different prescriptions of the MLT
theory of convection and the effects of small amounts of H in the almost
He-pure atmospheres of DB stars on the precise location of the theoretical blue
edge of the DBV instability strip.Comment: Proceedings, 16th European White Dwarf Workshop, Barcelona, 200
New fully evolutionary models for asteroseismology of ultra-massive white dwarf stars
Ultra-massive hydrogen-rich (DA spectral type) white dwarf (WD) stars
() coming from single-star evolution are expected to
harbor cores made of O and Ne, resulting from semi-degenerate
carbon burning when the progenitor star evolves through the super asymptotic
giant branch (S-AGB) phase. These stars are expected to be crystallized by the
time they reach the ZZ Ceti instability strip ( K).
Theoretical models predict that crystallization leads to a separation of
O and Ne in the core of ultra-massive WDs, which impacts their
pulsational properties. This property offers a unique opportunity to study the
processes of crystallization. Here, we present the first results of a detailed
asteroseismic analysis of the best-studied ultra-massive ZZ Ceti star
BPM~37093. As a second step, we plan to repeat this analysis using
ultra-massive DA WD models with C/O cores in order to study the possibility of
elucidating the core chemical composition of BPM~37093 and shed some light on
its possible evolutionary origin. We also plan to extend this kind of analyses
to other stars observed from the ground and also from space missions like
Kepler and TESS.Comment: 4 pages, 2 tables, 2 figures, poster contribution at the conference
"Stars and their variability observed from space - Celebrating the 5th
anniversary of BRITE-Constellation", Vienna, Austria, August 19 - 23, 2019.
Eds: C. Neiner, W. Weiss, D. Baade, E. Griffin, C. Lovekin, A. Moffa
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