Light elements in stars with exoplanets

It is well known that stars orbited by giant planets have higher abundances of heavy elements when compared with average field dwarfs. A number of studies have also addressed the possibility that light element abundances are different in these stars. In this paper we will review the present status of these studies. The most significant trends will be discussed.Comment: 10 pages, 6 figures. Submitted to the proceedings of IAU symposium 268: Light elements in the universe

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

The Updated BaSTI Stellar Evolution Models and Isochrones: I. Solar Scaled Calculations

We present an updated release of the BaSTI (a Bag of Stellar Tracks and Isochrones) stellar model and isochrone library for a solar scaled heavy element distribution. The main input physics changed from the previous BaSTI release include the solar metal mixture, electron conduction opacities, a few nuclear reaction rates, bolometric corrections, and the treatment of the overshooting efficiency for shrinking convective cores. The new model calculations cover a mass range between 0.1 and 15 Msun, 22 initial chemical compositions between [Fe/H]=-3.20 and +0.45, with helium to metal enrichment ratio dY /dZ=1.31. The isochrones cover an age range between 20 Myr and 14.5 Gyr, take consistently into account the pre-main sequence phase, and have been translated to a large number of popular photometric systems. Asteroseismic properties of the theoretical models have also been calculated. We compare our isochrones with results from independent databases and with several sets of observations, to test the accuracy of the calculations. All stellar evolution tracks, asteroseismic properties and isochrones are made available through a dedicated Web site

Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi

Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies1. Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called Gaia–Enceladus1, leading to substantial pollution of the chemical and dynamical properties of the Milky Way. Here we identify the very bright, naked-eye star ν Indi as an indicator of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be 11.0±0.7 (stat) ±0.8 (sys) billion years. The star bears hallmarks consistent with having been kinematically heated by the Gaia–Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 billion years ago, at 68% and 95% confidence, respectively. Computations based on hierarchical cosmological models slightly reduce the above limits

Age dating of an early Milky Way merger via asteroseismology of the naked-eye star νν Indi

Over the course of its history, the Milky Way has ingested multiple smaller satellite galaxies. While these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to precisely date the age at which any one merger occurred. Recent results have revealed a population of stars that were accreted via the collision of a dwarf galaxy, called \textit{Gaia}-Enceladus, leading to a substantial pollution of the chemical and dynamical properties of the Milky Way. Here, we identify the very bright, naked-eye star $\nu$\,Indi as a probe of the age of the early in situ population of the Galaxy. We combine asteroseismic, spectroscopic, astrometric, and kinematic observations to show that this metal-poor, alpha-element-rich star was an indigenous member of the halo, and we measure its age to be $11.0 \pm 0.7$ (stat) $\pm 0.8$ (sys)$\,\rm Gyr$. The star bears hallmarks consistent with it having been kinematically heated by the \textit{Gaia}-Enceladus collision. Its age implies that the earliest the merger could have begun was 11.6 and 13.2 Gyr ago at 68 and 95% confidence, respectively. Input from computations based on hierarchical cosmological models tightens (i.e. reduces) slightly the above limits

Learning about protein solubility from bacterial inclusion bodies.

The progressive solving of the conformation of aggregated proteins and the conceptual understanding of the biology of inclusion bodies in recombinant bacteria is providing exciting insights on protein folding and quality. Interestingly, newest data also show an unexpected functional and structural complexity of soluble recombinant protein species and picture the whole bacterial cell factory scenario as more intricate than formerly believed

The Functional quality of soluble recombinant polypeptides produced in Escherichia coli is defined by a wide conformational spectrum.

We have observed that a soluble recombinant green fluorescent protein produced in Escherichia coli occurs in a wide conformational spectrum. This results in differently fluorescent protein fractions in which morphologically diverse soluble aggregates abound. Therefore, the functional quality of soluble versions of aggregation-prone recombinant proteins is defined statistically rather than by the prevalence of a canonical native structure

Systems-level analysis of protein quality in inclusion body-forming Escherichia coli cells

Recombinant proteins produced in Escherichia coli often aggregate as amorphous masses of insoluble material known as inclusion bodies. Being quite homogeneous in their composition, inclusion bodies display amyloid-like properties such as sequence-dependent protein-protein interactions, seeding-driven deposition of their components and β-sheet intermolecular architecture. However, inclusion bodies formed by different proteins and enzymes also show important extents of native-like secondary structure and include significant proportions of properly folded, functional protein, which makes them suitable to be used in catalytic processes. Inclusion bodies are formed as a result of the incapability of the quality control cell system to cope with the non physiological amounts of misfolding-prone proteins produced upon recombinant gene expression. Multiple cellular proteins involved in the quality control, namely chaperones and proteases, participate in their formation and co-ordinately determine the amount of aggregated protein, the size of aggregates and the main structural and functional properties of the embedded polypeptides, such as their inner molecular organization. © 2009 Springer Netherlands

Systems-level analysis of protein quality in inclusion body-forming Escherichia coli cells

Recombinant proteins produced in Escherichia coli often aggregate as amorphous masses of insoluble material known as inclusion bodies. Being quite homogeneous in their composition, inclusion bodies display amyloid-like properties such as sequence-dependent protein-protein interactions, seeding-driven deposition of their components and β-sheet intermolecular architecture. However, inclusion bodies formed by different proteins and enzymes also show important extents of native-like secondary structure and include significant proportions of properly folded, functional protein, which makes them suitable to be used in catalytic processes. Inclusion bodies are formed as a result of the incapability of the quality control cell system to cope with the non physiological amounts of misfolding-prone proteins produced upon recombinant gene expression. Multiple cellular proteins involved in the quality control, namely chaperones and proteases, participate in their formation and co-ordinately determine the amount of aggregated protein, the size of aggregates and the main structural and functional properties of the embedded polypeptides, such as their inner molecular organization. © 2009 Springer Netherlands