Shear mixing in stellar radiative zones I. Effect of thermal diffusion and chemical stratification

Turbulent transport of chemical elements in radiative zones of stars is considered in current stellar evolution codes thanks to phenomenologically derived diffusion coefficients. Recent local numerical simulations (Prat & Ligni\`eres 2013, A&A, 551, L3) suggest that the coefficient for radial turbulent diffusion due to radial differential rotation satisfies $D_{\rm t}\simeq0.058\kappa/Ri$, in qualitative agreement with Zahn's model. However, this model does not apply when differential rotation is strong with respect to stable thermal stratification or when chemical stratification has a significant dynamical effect, a situation encountered at the outer boundary of nuclear-burning convective cores. We extend our numerical study to consider the effects of chemical stratification and of strong shear, and compare the results with prescriptions used in stellar evolution codes. We performed local, direct numerical simulations of stably stratified, homogeneous, sheared turbulence in the Boussinesq approximation. The regime of high thermal diffusivities, typical of stellar radiative zones, is reached thanks to the so-called small-P\'eclet-number approximation, which is an asymptotic development of the Boussinesq equations in this regime. The dependence of the diffusion coefficient on chemical stratification was explored in this approximation. Maeder's extension of Zahn's model in the strong-shear regime is not supported by our results, which are better described by a model found in the geophysical literature. As regards the effect of chemical stratification, our quantitative estimate of the diffusion coefficient as a function of the mean gradient of mean molecular weight leads to the formula $D_{\rm t}\simeq 0.45\kappa(0.12-Ri_\mu)/Ri$, which is compatible in the weak-shear regime with the model of Maeder & Meynet (1996, A&A, 313, 140).Comment: 10 pages, 9 figures, accepted in A&

Toward a consistent use of overshooting parametrizations in 1D stellar evolution codes

Several parametrizations for overshooting in 1D stellar evolution calculations coexist in the literature. These parametrizations are used somewhat arbitrarily in stellar evolution codes, based on what works best for a given problem, or even for historical reasons related to the development of each code. We bring attention to the fact that these different parametrizations correspond to different physical regimes of overshooting, depending whether the effects of radiation are dominant, marginal, or negligible. Our analysis is based on previously published theoretical results, as well as multidimensional hydrodynamical simulations of stellar convection where the interaction between the convective region and a stably-stratified region is observed. Although the underlying hydrodynamical processes are the same, the outcome of the overshooting process is profoundly affected by radiative effects. Using a simple picture of the scales involved in the overshooting process, we show how three regimes are obtained, depending on the importance of radiative effects. These three regimes correspond to the different behaviors observed in hydrodynamical simulations so far, and to the three types of parametrizations used in 1D codes. We suggest that the existing parametrizations for overshooting should coexist in 1D stellar evolution codes, and should be applied consistently at convective boundaries depending on the local physical conditions.Comment: 5 pages, 2 figures, to appear in A&A as a regular paper. Last version: language editing + typos in Eq. (6) & (9) correcte

Seismic diagnosis from gravity modes strongly affected by rotation

Most of the information we have about the internal rotation of stars comes from modes that are weakly affected by rotation, for example by using rotational splittings. In contrast, we present here a method, based on the asymptotic theory of Prat et al. (2016), which allows us to analyse the signature of rotation where its effect is the most important, that is in low-frequency gravity modes that are strongly affected by rotation. For such modes, we predict two spectral patterns that could be confronted to observed spectra and those computed using fully two-dimensional oscillation codes.Comment: 3 pages, 1 figure, to appear in the proceedings of the Joint TASC2 & KASC9 Workshop SPACEINN & HELAS8 Conference "Seismology of the Sun and the Distant Stars 2016

On the relevance of bubbles and potential flows for stellar convection

Recently Pasetto et al. have proposed a new method to derive a convection theory appropriate for the implementation in stellar evolution codes. Their approach is based on the simple physical picture of spherical bubbles moving within a potential flow in dynamically unstable regions, and a detailed computation of the bubble dynamics. Based on this approach the authors derive a new theory of convection which is claimed to be parameter free, non-local and time-dependent. This is a very strong claim, as such a theory is the holy grail of stellar physics. Unfortunately we have identified several distinct problems in the derivation which ultimately render their theory inapplicable to any physical regime. In addition we show that the framework of spherical bubbles in potential flows is unable to capture the essence of stellar convection, even when equations are derived correctly.Comment: 14 pages, 3 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society. (Comments and criticism are welcomed

Transport turbulent d'éléments chimiques dans les zones radiatives stellaires

Un des enjeux majeurs de la théorie de l'évolution stellaire est de comprendre l'influence des processus de transport liés aux mouvements macroscopiques engendrés par la rotation sur la structure interne et l'évolution des étoiles. En particulier, le transport turbulent des éléments chimiques dû à la rotation différentielle dans les zones radiatives des étoiles est actuellement pris en compte dans de nombreux codes d'évolution stellaire comme un processus diffusif dont le coefficient est déterminé à partir d'arguments phénoménologiques. Le but de cette thèse est de contraindre l'un de ces coefficients, le coefficient de diffusion radiale induit par la rotation différentielle radiale, à l'aide de simulations numériques directes décrivant les mouvements turbulents engendrés par un cisaillement forcé localement dans une zone radiative d'étoile. L'exploration du domaine des très fortes diffusivités thermiques - ou, de manière équivalente, des petits nombres de Péclet - typiques des intérieurs stellaires a été rendue possible par l'utilisation d'un développement asymptotique des équations de Boussinesq adapté. Le principal résultat ce cette thèse est que nos simulations numériques sont en accord avec la forme du coefficient de diffusion proposée par J.-P. Zahn dans le régime des nombres de Péclet turbulents inférieurs à un. Les résultats obtenus pour des nombres de Péclet supérieurs à un sont en accord avec le modèle de Lindborg & Brethouwer (2008) proposé dans un contexte géophysique. Les simulations réalisées en prenant en compte l'effet dynamique de la stratification chimique nous ont également permis de valider un des modèles utilisés dans les codes d'évolution stellaire et d'en éliminer un autre.One of the key issues of stellar evolution theory is the influence of transport processes related to macroscopic motions driven by rotation on the internal structure and evolution of stars. In particular, turbulent mixing of chemical elements due to differential rotation in stellar radiative zones is currently taken into account in many stellar evolution codes as a diffusive process whose coefficient is determined from phenomenological arguments. The purpose of this thesis is to constrain one of these coefficients, the radial diffusion coefficient driven by radial differential rotation through local direct numerical simulations describing turbulent motions induced by a locally forced shear in a stellar radiative zone. The exploration of the domain of very large thermal diffusivities - or equivalently of small Péclet numbers - typical of stellar interiors was made possible thanks to a suitable asymptotic expansion of the Boussinesq equations. The main result of this thesis is that our numerical simulations are in agreement with the form of the vertical turbulent diffusion coefficient proposed by J.-P. Zahn in the regime of turbulent Péclet numbers smaller than one. The results obtained for Péclet numbers greater than one are in agreement with the model of Lindborg & Brethouwer (2008) proposed in a geophysical context. The simulations taking into account the dynamical effect of chemical stratification also allowed us to validate one of the models used in stellar evolution codes and to eliminate another one

On the relevance of bubbles and potential flows for stellar convection

Recently Pasetto et al. have proposed a new method to derive a convection theory appropriate for the implementation in stellar evolution codes. Their approach is based on the simple physical picture of spherical bubbles moving within a potential flow in dynamically unstable regions, and a detailed computation of the bubble dynamics. Based on this approach, the authors derive a new theory of convection which is claimed to be parameter-free, non-local and time-dependent. This is a very strong claim, as such a theory is the holy grail of stellar physics. Unfortunately, we have identified several distinct problems in the derivation which ultimately render their theory inapplicable to any physical regime. In addition, we show that the framework of spherical bubbles in potential flows is unable to capture the essence of stellar convection, even when equations are derived correctly.Facultad de Ciencias Astronómicas y GeofísicasInstituto de Astrofísica de La Plat

Helicobacter pylori infection is not associated with an increased hemorrhagic risk in patients in the intensive care unit

INTRODUCTION: The potential role of Helicobacter pylori in acute stress ulcer in patients in an intensive care unit (ICU) is controversial. The aim of this study was to determine the frequency of H. pylori infection in ICU patients by antigen detection on rectal swabs, and to analyze the potential relationship between the presence of H. pylori and the risk of digestive gastrointestinal bleeding. METHODS: In this prospective, multicenter, epidemiological study, the inclusion criteria were as follows: patients admitted to the 12 participating ICU for at least two days, who were free of hemorrhagic shock and did not receive more than four units of red blood cells during the day before or the first 48 hours after admission to the ICU. Rectal swabs were obtained within the first 24 hours of admission to the ICU and were tested for H. pylori antigens with the ImmunoCard STAT! HpSA kit. The following events were analyzed according to H. pylori status: gastrointestinal bleeding, unexplained decline in hematocrit, and the number of red cell transfusions. RESULTS: The study involved 1,776 patients. Forty-nine patients (2.8%) had clinical evidence of upper digestive bleeding. Esophagogastroduodenoscopy was performed in 7.6% of patients. Five hundred patients (28.2%) required blood transfusion. H. pylori antigen was detected in 6.3% of patients (95% confidence interval 5.2 to 7.5). H. pylori antigen positivity was associated with female sex (p < 0.05) and with a higher Simplified Acute Physiology Score II (SAPS II; p < 0.05). H. pylori antigen status was not associated with the use of fiber-optic gastroscopy, the need for red cell transfusions, or the number of red cell units infused. CONCLUSION: This large study reported a small percentage of H. pylori infection detected with rectal swab sampling in ICU patients and showed that the patients infected with H. pylori had no additional risk of gastrointestinal bleeding. Thus H. pylori does not seem to have a major role in the pathogenesis of acute stress ulcer in ICU patients

Weak Lensing from Space I: Instrumentation and Survey Strategy

A wide field space-based imaging telescope is necessary to fully exploit the technique of observing dark matter via weak gravitational lensing. This first paper in a three part series outlines the survey strategies and relevant instrumental parameters for such a mission. As a concrete example of hardware design, we consider the proposed Supernova/Acceleration Probe (SNAP). Using SNAP engineering models, we quantify the major contributions to this telescope's Point Spread Function (PSF). These PSF contributions are relevant to any similar wide field space telescope. We further show that the PSF of SNAP or a similar telescope will be smaller than current ground-based PSFs, and more isotropic and stable over time than the PSF of the Hubble Space Telescope. We outline survey strategies for two different regimes - a ``wide'' 300 square degree survey and a ``deep'' 15 square degree survey that will accomplish various weak lensing goals including statistical studies and dark matter mapping.Comment: 25 pages, 8 figures, 1 table, replaced with Published Versio