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2. The Gaia-ESO Survey: properties of newly discovered Li-rich giants

Author

Smiljanic, R., primary, Franciosini, E., additional, Bragaglia, A., additional, Tautvaišienė, G., additional, Fu, X., additional, Pancino, E., additional, Adibekyan, V., additional, Sousa, S. G., additional, Randich, S., additional, Montalbán, J., additional, Pasquini, L., additional, Magrini, L., additional, Drazdauskas, A., additional, García, R. A., additional, Mathur, S., additional, Mosser, B., additional, Régulo, C., additional, de Assis Peralta, R., additional, Hekker, S., additional, Feuillet, D., additional, Valentini, M., additional, Morel, T., additional, Martell, S., additional, Gilmore, G., additional, Feltzing, S., additional, Vallenari, A., additional, Bensby, T., additional, Korn, A. J., additional, Lanzafame, A. C., additional, Recio-Blanco, A., additional, Bayo, A., additional, Carraro, G., additional, Costado, M. T., additional, Frasca, A., additional, Jofré, P., additional, Lardo, C., additional, de Laverny, P., additional, Lind, K., additional, Masseron, T., additional, Monaco, L., additional, Morbidelli, L., additional, Prisinzano, L., additional, Sbordone, L., additional, and Zaggia, S., additional

Published
2018
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4. Galactic archaeology with asteroseismology and spectroscopy: Red giants observed by CoRoT and APOGEE

Author

Anders, F., primary, Chiappini, C., additional, Rodrigues, T. S., additional, Miglio, A., additional, Montalbán, J., additional, Mosser, B., additional, Girardi, L., additional, Valentini, M., additional, Noels, A., additional, Morel, T., additional, Johnson, J. A., additional, Schultheis, M., additional, Baudin, F., additional, de Assis Peralta, R., additional, Hekker, S., additional, Themeßl, N., additional, Kallinger, T., additional, García, R. A., additional, Mathur, S., additional, Baglin, A., additional, Santiago, B. X., additional, Martig, M., additional, Minchev, I., additional, Steinmetz, M., additional, da Costa, L. N., additional, Maia, M. A. G., additional, Allende Prieto, C., additional, Cunha, K., additional, Beers, T. C., additional, Epstein, C., additional, García Pérez, A. E., additional, García-Hernández, D. A., additional, Harding, P., additional, Holtzman, J., additional, Majewski, S. R., additional, Mészáros, Sz., additional, Nidever, D., additional, Pan, K., additional, Pinsonneault, M., additional, Schiavon, R. P., additional, Schneider, D. P., additional, Shetrone, M. D., additional, Stassun, K., additional, Zamora, O., additional, and Zasowski, G., additional

Published
2016
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5. Young [α/Fe]-enhanced stars discovered by CoRoT and APOGEE: What is their origin?

Author

Chiappini, C., primary, Anders, F., additional, Rodrigues, T. S., additional, Miglio, A., additional, Montalbán, J., additional, Mosser, B., additional, Girardi, L., additional, Valentini, M., additional, Noels, A., additional, Morel, T., additional, Minchev, I., additional, Steinmetz, M., additional, Santiago, B. X., additional, Schultheis, M., additional, Martig, M., additional, da Costa, L. N., additional, Maia, M. A. G., additional, Allende Prieto, C., additional, de Assis Peralta, R., additional, Hekker, S., additional, Themeßl, N., additional, Kallinger, T., additional, García, R. A., additional, Mathur, S., additional, Baudin, F., additional, Beers, T. C., additional, Cunha, K., additional, Harding, P., additional, Holtzman, J., additional, Majewski, S., additional, Mészáros, Sz., additional, Nidever, D., additional, Pan, K., additional, Schiavon, R. P., additional, Shetrone, M. D., additional, Schneider, D. P., additional, and Stassun, K., additional

Published
2015
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6. OH and H2O maser variations in W33B

Author

Chiappini, C., Anders, F., Rodrigues, T., Miglio, A., Montalban, J., Mosser, B., Girardi, L., Valentini, M., Noels, A., Morel, T., Minchev, I., Steinmetz, M., Santiago, B., Schultheis, M., Martig, M., da Costa, L., Maia, M., Allende Prieto, C., de Assis Peralta, R., Hekker, S., Themessl, N., Kallinger, T., Garcia, R., Mathur, S., Baudin, F., Beers, T., Cunha, K., Harding, P., Holtzman, J., Majewski, S., Mészáros, Sz., Nidever, D., Pan, K., Schiavon, R., Shetrone, M., Schneider, D., Stassun, K., Colom, P., Lekht, E., Pashchenko, M., Rudnitskij, G., Leibniz-Institut für Astrophysik Potsdam (AIP), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Département d'astrophysique, Géophysique et Océanographie (AGO), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Liverpool John Moores University (LJMU), Laboratoire Géosciences Océan (LGO), Université de Bretagne Sud (UBS)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), School of Physics and Astronomy, University of Birmingham [Birmingham], Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de Physique du Globe de Paris (IPG Paris), Space Science Institute [Boulder] (SSI), Commissariat à l'énergie atomique et aux énergies alternatives - Laboratoire d'Electronique et de Technologie de l'Information (CEA-LETI), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Center for the Study of Cosmic Evolution (CSCE), Michigan State University [East Lansing], Michigan State University System-Michigan State University System, Department of Geography, Department of geography, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut Français de Recherche pour l'Exploitation de la Mer - Brest (IFREMER Centre de Bretagne), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université de Bretagne Sud (UBS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris, Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Bretagne Sud (UBS)-Université de Brest (UBO)-Institut Universitaire Européen de la Mer (IUEM), and Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
individual objects, 85A15, lines and bands -ISM, Astrophysics::High Energy Astrophysical Phenomena, Central object, FOS: Physical sciences, Astrophysics, 01 natural sciences, W33B, law.invention, Radio telescope, symbols.namesake, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Maser, masers -ISM, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, magnetic fields -ISM, Line (formation), [PHYS]Physics [physics], Physics, Zeeman effect, 010308 nuclear & particles physics, molecules -ISM, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Magnetic field, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Excitation
Abstract

The active star-forming region W33B is a source of OH and H2O maser emission located in distinct zones around the central object. The aim was to obtain the complete Stokes pattern of polarised OH maser emission, to trace its variability and to investigate flares and long-term variability of the H2O maser and evolution of individual emission features. Observations in the OH lines at a wavelength of 18 cm were carried out on the Nan\c{c}ay radio telescope (France) at a number of epochs in 2008--2014; H2O line observations (long-term monitoring) at a wavelength of 1.35 cm were performed on the 22-metre radio telescope of the Pushchino Radio Astronomy Observatory (Russia) between 1981 and 2014. We have observed strong variability of the emission features in the main 1665- and 1667-MHz OH lines as well as in the 1612-MHz satellite line. Zeeman splitting has been detected in the 1665-MHz OH line at 62 km/s and in the 1667-MHz line at 62 and 64 km/s. The magnetic field intensity was estimated to be from 2 to 3 mG. The H2O emission features form filaments, chains with radial-velocity gradients, or more complicated structures including large-scale ones. Long-term observations of the hydroxyl maser in the W33B region have revealed narrowband polarised emission in the 1612-MHz line with a double-peak profile characteristic of Type IIb circumstellar masers. The 30-year monitoring of the water-vapour maser in W33B showed several strong flares of the H2O line. The observed radial-velocity drift of the H2O emission features suggests propagation of an excitation wave in the masering medium with a gradient of radial velocities. In OH and H2O masers some turbulent motions of material are inferred., Comment: 18 pages, 12 figures

Published
2015

7. Galactic archaeology with asteroseismology and spectroscopy: Red giants observed by CoRoT and APOGEE.

Author

Anders, F., Chiappini, C., Rodrigues, T. S., Miglio, A., Montalbán, J., Mosser, B., Girardi, L., Valentini, M., Noels, A., Morel, T., Johnson, J. A., Schultheis, M., Baudin, F., de Assis Peralta, R., Hekker, S., Themeß, N., Kallinger, T., García, R. A., Mathur, S., and Baglin, A.

Subjects
OPEN clusters of stars, GALACTIC evolution, SPACE archaeology, RED giants, MILKY Way
Abstract

With the advent of the space missions CoRoT and Kepler, it has recently become feasible to determine precise asteroseismic masses and relative ages for large samples of red giant stars. We present the CoRoGEE dataset, obtained from CoRoT light curves for 606 red giants in two fields of the Galactic disc that have been co-observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). We used the Bayesian parameter estimation code PARAM to calculate distances, extinctions, masses, and ages for these stars in a homogeneous analysis, resulting in relative statistical uncertainties of .2% in distance, ~4% in radius, ~9% in mass and ~25% in age. We also assessed systematic age uncertainties stemming from different input physics and mass loss. We discuss the correlation between ages and chemical abundance patterns of field stars over a broad radial range of the Milky Way disc (5 kpc < RGal < 14 kpc), focussing on the [ /Fe]-[Fe/H]-age plane in five radial bins of the Galactic disc. We find an overall agreement with the expectations of pure chemical-evolution models computed before the present data were available, especially for the outer regions. However, our data also indicate that a significant fraction of stars now observed near and beyond the solar neighbourhood migrated from inner regions. Mock CoRoGEE observations of a chemodynamical Milky Way disc model indicate that the number of high-metallicity stars in the outer disc is too high to be accounted for even by the strong radial mixing present in the model. The mock observations also show that the age distribution of the [ /Fe]-enhanced sequence in the CoRoGEE inner-disc field is much broader than expected from a combination of radial mixing and observational errors. We suggest that a thick-disc/bulge component that formed stars for more than 3 Gyr may account for these discrepancies. Our results are subject to future improvements due to (a) the still low statistics, because our sample had to be sliced into bins of Galactocentric distances and ages; (b) large uncertainties in proper motions (and therefore guiding radii); and (c) corrections to the asteroseismic mass-scaling relation. The situation will improve not only upon the upcoming Gaia data releases, but also with the foreseen increase in the number of stars with both seismic and spectroscopic information. [ABSTRACT FROM AUTHOR]

Published
2017
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8. A new method for extracting seismic indices and granulation parameters: Results for more than 20,000 CoRoT and Kepler red giants.

Author

de Assis Peralta, R., Samadi, R., and Michel, E.

Subjects
*STELLAR granulation, *RED giants, *STELLAR evolution, *ASTRONOMICAL photometry, *STELLAR oscillations
Abstract

We have developed a new automated method intended to perform the simultaneous—and thus more consistent—measurement of both the seismic indices characterizing the oscillations and the parameters characterizing the granulation signature of red giant stars. This method, called MLEUP, takes advantage of the Maximum Likelihood Estimate (MLE) algorithm combined with the parameterized representation of red giant pulsation spectra following the universal pattern (UP). Its performances have been tested on Monte Carlo simulations for observation conditions representative of CoRoT and Kepler data. These simulations allowed us to determine, calibrate, and propose corrections for the biases on the parameter estimates as well as on the error estimates produced with MLEUP. Finally, we applied MLEUP to CoRoT and Kepler data. In total, MLEUP yields seismic indices for 20,122 red giant stars and granulation parameters for 17,109 of them. These data have been made available in the stellar seismic indices database ( http://ssi.lesia.obspm.fr/). [ABSTRACT FROM AUTHOR]

Published
2018
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9. The Gaia -ESO Survey: Properties of newly discovered Li-rich giants

Author

C. Régulo, Giovanni Carraro, Luca Sbordone, Amelia Bayo, Rafael A. García, E. Franciosini, Thierry Morel, X. Fu, Arnas Drazdauskas, Thomas Bensby, Alejandra Recio-Blanco, Laura Magrini, B. Mosser, Angela Bragaglia, Savita Mathur, Simone Zaggia, L. Prisinzano, L. Morbidelli, R. de Assis Peralta, Lorenzo Monaco, A. C. Lanzafame, Antonio Frasca, Sofia Randich, M. T. Costado, Paula Jofre, V. Adibekyan, P. de Laverny, Karin Lind, Andreas J. Korn, Rodolfo Smiljanic, Grazina Tautvaisiene, L. Pasquini, Elena Pancino, Thomas Masseron, Marica Valentini, S. G. Sousa, Saskia Hekker, Antonella Vallenari, Josefina Montalbán, Gerard Gilmore, D. Feuillet, Carmela Lardo, Sofia Feltzing, Sarah L. Martell, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Matériaux divisés, interfaces, réactivité, électrochimie (MADIREL), Aix Marseille Université (AMU)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Space Science Institute [Boulder] (SSI), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Astrofísica [La laguna], Universidad de La Laguna [Tenerife - SP] (ULL), School of Physics and Astronomy, University of Birmingham [Birmingham], Dipartimento di Scienze e Tecnologie Aerospaziali - Politecnico, Politecnico di Milano [Milan] (POLIMI), Lund Observatory, Lund University [Lund], INAF - Osservatorio Astronomico di Padova (OAPD), Department of Astronomy and Space Physics [Uppsala], Uppsala University, INAF - Osservatorio Astrofisico di Catania (OACT), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole Polytechnique Fédérale de Lausanne (EPFL), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Smiljanic R., Franciosini E., Bragaglia A., Tautvaisiene G., Fu X., Pancino E., Adibekyan V., Sousa S.G., Randich S., Montalban J., Pasquini L., Magrini L., Drazdauskas A., Garcia R.A., Mathur S., Mosser B., Regulo C., De Assis Peralta R., Hekker S., Feuillet D., Valentini M., Morel T., Martell S., Gilmore G., Feltzing S., Vallenari A., Bensby T., Korn A.J., Lanzafame A.C., Recio-Blanco A., Bayo A., Carraro G., Costado M.T., Frasca A., Jofre P., Lardo C., De Laverny P., Lind K., Masseron T., Monaco L., Morbidelli L., Prisinzano L., Sbordone L., Zaggia S., ITA, USA, GBR, FRA, DEU, ESP, AUS, BEL, CHL, DNK, LTU, POL, PRT, SWE, CHE, Universidade do Porto = University of Porto, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Gilmore, Gerard [0000-0003-4632-0213], Apollo - University of Cambridge Repository, Osservatorio Astronomico di Bologna (OABO), Universidade do Porto [Porto], Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional de Colombia, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
barium stars, k-giant, Astrophysics, Stars: late-type, GALACTIC BULGE, mass-loss, 7. Clean energy, 01 natural sciences, LITHIUM ENRICHMENT, Bulge, Planet, Asymptotic giant branch, EVOLVED STARS, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Physics, K-GIANT, [PHYS]Physics [physics], open clusters, red giants, LATE-TYPE STARS, Evolution [Stars], Red-giant branch, evolved stars, Stars: evolution, Astrophysics - Solar and Stellar Astrophysics, late-type [Stars], chemical-composition, Astrophysics::Earth and Planetary Astrophysics, Stars: abundance, stars: abundances, late-type stars, FOS: Physical sciences, Abundances [Stars], Astrophysics::Cosmology and Extragalactic Astrophysics, galactic bulge, CHEMICAL-COMPOSITION, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Infrared excess, 010308 nuclear & particles physics, Astronomy and Astrophysics, MASS-LOSS, BARIUM STARS, Accretion (astrophysics), lithium enrichment, RED GIANTS, Stars, Stars: abundances, Space and Planetary Science, 13. Climate action, OPEN CLUSTERS, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Open cluster
Abstract

Aims. We report 20 new lithium-rich giants discovered within the Gaia-ESO Survey, including the first Li-rich giant with an evolutionary stage confirmed by CoRoT (Convection, Rotation and planetary Transits) data. We present a detailed overview of the properties of these 20 stars., Methods. Atmospheric parameters and abundances were derived in model atmosphere analyses using medium-resolution GIRAFFE or high-resolution UVES (Ultraviolet and Visual Echelle Spectrograph) spectra. These results are part of the fifth internal data release of the Gaia-ESO Survey. The Li abundances were corrected for non-local thermodynamical equilibrium effects. Other stellar properties were investigated for additional peculiarities (the core of strong lines for signs of magnetic activity, infrared magnitudes, rotational velocities, chemical abundances, and Galactic velocities). We used Gaia DR2 parallaxes to estimate distances and luminosities., Results. The giants have A(Li) > 2.2 dex. The majority of them (14 of 20 stars) are in the CoRoT fields. Four giants are located in the field of three open clusters, but are not members. Two giants were observed in fields towards the Galactic bulge, but likely lie in the inner disc. One of the bulge field giants is super Li-rich with A(Li) = 4.0 dex., Conclusions. We identified one giant with infrared excess at 22 mu m. Two other giants, with large v sin i, might be Li-rich because of planet engulfment. Another giant is found to be barium enhanced and thus could have accreted material from a former asymptotic giant branch companion. Otherwise, in addition to the Li enrichment, the evolutionary stages are the only other connection between these new Li-rich giants. The CoRoT data confirm that one Li-rich giant is at the core-He burning stage. The other giants are concentrated in close proximity to the red giant branch luminosity bump, the core-He burning stages, or the early-asymptotic giant branch. This is very clear from the Gaia-based luminosities of the Li-rich giants. This is also seen when the CoRoT Li-rich giants are compared to a larger sample of 2252 giants observed in the CoRoT fields by the Gaia-ESO Survey, which are distributed throughout the red giant branch in the T-eff-log g diagram. These observations show that the evolutionary stage is a major factor for the Li enrichment in giants. Other processes, such as planet accretion, contribute at a smaller scale.

Published
2018

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