7 results on '"Martell S.L."'
Search Results
2. Light-element abundance variations in globular clusters
- Author
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Martell, S.L., primary
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- 2011
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3. Total serum creatine kinase and isozyme concentrations in the owl monkey
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Weller, R.E., primary, Buschbom, R.L., additional, Martell, S.L., additional, Baer, J.F., additional, Málaga, C.A., additional, and Ragan, H.A., additional
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- 1991
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4. The Gaia-ESO survey: galactic evolution of lithium from iDR6
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Grazina Tautvaisiene, Guillaume Guiglion, Andreas Korn, V. Grisoni, P. Bonifacio, Rodolfo Smiljanic, G. Casali, E. Franciosini, Donatella Romano, Paula Jofre, P. de Laverny, R. D. Jeffries, Thomas Bensby, Alessio Mucciarelli, Francesco Damiani, E. Pancino, S. L. Martell, D. Montes, Sofia Randich, Antonella Vallenari, Lorenzo Spina, Cristina Chiappini, Maria Bergemann, A. Bragaglia, F. M. Jiménez-Esteban, M. L. Gutiérrez Albarrán, M. Bellazzini, X. Fu, G. Carraro, Laura Magrini, F. Matteucci, Paolo Ventura, Anais Gonneau, C. C. Worley, Romano D., Magrini L., Randich S., Casali G., Bonifacio P., Jeffries R.D., Matteucci F., Franciosini E., Spina L., Guiglion G., Chiappini C., Mucciarelli A., Ventura P., Grisoni V., Bellazzini M., Bensby T., Bragaglia A., De Laverny P., Korn A.J., Martell S.L., Tautvaisiene G., Carraro G., Gonneau A., Jofre P., Pancino E., Smiljanic R., Vallenari A., Fu X., Gutierrez Albarran M.L., Jimenez-Esteban F.M., Montes D., Damiani F., Bergemann M., Worley C., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)
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Astrofísica ,Metallicity ,FOS: Physical sciences ,chemistry.chemical_element ,Astrophysics ,7. Clean energy ,01 natural sciences ,evolution [Galaxy] ,Astronomi, astrofysik och kosmologi ,Abundance (ecology) ,0103 physical sciences ,stellar content [Galaxy] ,Astronomy, Astrophysics and Cosmology ,010303 astronomy & astrophysics ,ComputingMilieux_MISCELLANEOUS ,nuclear reactions ,Physics ,Galaxy: evolution ,Galaxy: stellar content ,[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] ,010308 nuclear & particles physics ,abundances ,Stars: abundances ,White dwarf ,abundances [Galaxy] ,nucleosynthesis ,Astronomy and Astrophysics ,Open clusters and associations: general ,Astrophysics - Astrophysics of Galaxies ,abundances [stars] ,Galaxy: abundance ,Astronomía ,Stars ,Supernova ,Meteorite ,chemistry ,13. Climate action ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Lithium ,general [open clusters and associations] ,Nuclear reactions, nucleosynthesis, abundance ,Open cluster - Abstract
We exploit the unique characteristics of a sample of open clusters (OCs) and field stars for which high-precision 7Li abundances and stellar parameters are homogeneously derived by the Gaia-ESO Survey (GES). We derive possibly undepleted 7Li abundances for 26 OCs and star forming regions with ages from young to old spanning a large range of Galactocentric distances, which allows us to reconstruct the local late Galactic evolution of lithium as well as its current abundance gradient along the disc. Field stars are added to look further back in time and to constrain 7Li evolution in other Galactic components. The data are then compared to theoretical tracks from chemical evolution models that implement different 7Li forges. We find that the upper envelope of the 7Li abundances measured in field stars of nearly solar metallicities traces very well the level of lithium enrichment attained by the ISM as inferred from observations of cluster stars. We confirm previous findings that the abundance of 7Li in the solar neighbourhood does not decrease at supersolar metallicity. The comparison of the data with the chemical evolution model predictions favours a scenario in which the majority of the 7Li abundance in meteorites comes from novae. Current data also seem to suggest that the nova rate flattens out at later times. This requirement might have implications for the masses of the white dwarf nova progenitors and deserves further investigation. Neutrino-induced reactions taking place in core-collapse supernovae also produce some fresh lithium. This likely makes a negligible contribution to the meteoritic abundance, but could be responsible for a mild increase of the 7Li abundance in the ISM of low-metallicity systems that would counterbalance the astration processes., 17 pages, 10 figures, 3 tables (full tables 1 and 3 only available at the CDS), accepted for publication in Astronomy and Astrophysics. Version 2 includes corrections from language editor
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- 2021
5. Gaia-ESO Survey: Detailed elemental abundances in red giants of the peculiar globular cluster NGC 1851
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Nicoletta Sanna, R. Minkeviciute, L. Morbidelli, Rodolfo Smiljanic, A. Bragaglia, Gerry Gilmore, Maria Bergemann, Thomas Bensby, S. L. Martell, E. Pancino, Laura Magrini, Šarūnas Mikolaitis, Guillaume Guiglion, M. Ambrosch, Arnas Drazdauskas, Carmela Lardo, Ulrike Heiter, G. Carraro, Anais Gonneau, Grazina Tautvaisiene, Andreas Korn, Y. Chorniy, E. Stonkute, E. Franciosini, V. Bagdonas, Sofia Randich, Simone Zaggia, ITA, GBR, DEU, AUS, LTU, POL, SWE, Tautvaisiene G., Drazdauskas A., Bragaglia A., Martell S.L., Pancino E., Lardo C., Mikolaitis S., Minkeviciute R., Stonkute E., Ambrosch M., Bagdonas V., Chorniy Y., Sanna N., Franciosini E., Smiljanic R., Randich S., Gilmore G., Bensby T., Bergemann M., Gonneau A., Guiglion G., Carraro G., Heiter U., Korn A., Magrini L., Morbidelli L., and Zaggia S.
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Physics ,stars: abundances ,stars: evolution ,globular clusters: individual: NGC 1851 ,abundance ,Star ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Globular cluster ,Stars ,Astrophysics - Astrophysics of Galaxies ,Astrophysics - Solar and Stellar Astrophysics ,NGC 1851 ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,evolution ,individual ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
Context. NGC 1851 is one of several globular clusters for which multiple stellar populations of the subgiant branch have been clearly identified and a difference in metallicity detected. A crucial piece of information on the formation history of this cluster can be provided by the sum of A(C+N+O) abundances. However, these values have lacked a general consensus thus far. The separation of the subgiant branch can be based on age and/or A(C+N+O) abundance differences. Aims. Our main aim was to determine carbon, nitrogen, and oxygen abundances for evolved giants in the globular cluster NGC1851 in order to check whether or not the double populations of stars are coeval. Methods. High-resolution spectra, observed with the FLAMES-UVES spectrograph on the ESO VLT telescope, were analysed using a differential model atmosphere method. Results. We provide abundances of up to 29 chemical elements for a sample of 45 giants in NGC 1851. The investigated stars can be separated into two populations with a difference of 0.07 dex in the mean metallicity, 0.3 dex in the mean C/N, and 0.35 dex in the mean s-process dominated element-to-iron abundance ratios [s/Fe]. No significant difference was determined in the mean values of A(C+N+O) as well as in abundance to iron ratios of carbon, alpha- and iron-peak-elements, and of europium. Conclusions. As the averaged A(C+N+O) values between the two populations do not differ, additional evidence is given that NGC 1851 is composed of two clusters, the metal-rich cluster being by about 0.6 Gyr older than the metal-poor one. A global overview of NGC 1851 properties and the detailed abundances of chemical elements favour its formation in a dwarf spheroidal galaxy that was accreted by the Milky Way., Comment: 13 pages, 17 figures, accepted to Astronomy and Astrophysics
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- 2021
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6. The Gaia-ESO Survey: revisiting the Li-rich giant problem
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L. Morbidelli, Tomaž Zwitter, Thomas Masseron, Grant M. Kennedy, Lorenzo Monaco, S. G. Sousa, Rodolfo Smiljanic, A. Hourihane, Loredana Prisinzano, Giovanni Carraro, Laura Magrini, Angela Bragaglia, E. Franciosini, Alejandra Recio-Blanco, P. de Laverny, Clare Worley, Gražina Tautvaišienė, G. Ruchti, A. C. Lanzafame, P. Donati, G. G. Sacco, M. T. Costado, Sofia Randich, Karin Lind, Thierry Morel, Andreas Korn, Marica Valentini, E. Delgado Mena, Luca Sbordone, Simone Zaggia, Sergey E. Koposov, V. Silva Aguirre, Cristina Chiappini, Antonio Frasca, R. D. Jeffries, Francesco Damiani, P. Francois, Paula Jofre, James R. Lewis, Andrea Miglio, Ettore Flaccomio, Gerard Gilmore, Thomas Bensby, Y. Chorniy, Elena Pancino, Carmela Lardo, Sofia Feltzing, Sarah L. Martell, Josefina Montalbán, Andrew R. Casey, Antonella Vallenari, Casey, Andrew [0000-0003-0174-0564], Gilmore, Gerard [0000-0003-4632-0213], Kennedy, Grant [0000-0001-6831-7547], Koposov, Sergey [0000-0003-2644-135X], Worley, Clare [0000-0001-9310-2898], Apollo - University of Cambridge Repository, Casey A.R., Ruchti G., Masseron T., Randich S., Gilmore G., Lind K., Kennedy G.M., Koposov S.E., Hourihane A., Franciosini E., Lewis J.R., Magrini L., Morbidelli L., Sacco G.G., Worley C.C., Feltzing S., Jeffries R.D., Vallenari A., Bensby T., Bragaglia A., Flaccomio E., Francois P., Korn A.J., Lanzafame A., Pancino E., Recio-Blanco A., Smiljanic R., Carraro G., Costado M.T., Damiani F., Donati P., Frasca A., Jofre P., Lardo C., de Laverny P., Monaco L., Prisinzano L., Sbordone L., Sousa S.G., Tautvaisiene G., Zaggia S., Zwitter T., Mena E.D., Chorniy Y., Martell S.L., Aguirre V.S., Miglio A., Chiappini C., Montalban J., Morel T., and Valentini M.
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stars: abundancess ,astro-ph.SR ,stars: abundances ,Metallicity ,Bright giant ,FOS: Physical sciences ,CLUSTER NGC 362 ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,GALACTIC BULGE ,01 natural sciences ,Abundance ,Planet ,QB460 ,0103 physical sciences ,Hot Jupiter ,EVOLVED STARS ,Astrophysics::Solar and Stellar Astrophysics ,010303 astronomy & astrophysics ,Stellar evolution ,QC ,Solar and Stellar Astrophysics (astro-ph.SR) ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,010308 nuclear & particles physics ,MASS RED GIANTS ,Astronomy ,Astronomy and Astrophysics ,PLANET FORMATION ,Giant star ,Stars ,Accretion (astrophysics) ,Astrophysics - Solar and Stellar Astrophysics ,Space and Planetary Science ,K-GIANTS ,LITHIUM ABUNDANCES ,STELLAR EVOLUTION ,PRE-MAIN-SEQUENCE ,SUN-LIKE STARS ,Astrophysics::Earth and Planetary Astrophysics ,QB799 - Abstract
The discovery of lithium-rich giants contradicts expectations from canonical stellar evolution. Here we report on the serendipitous discovery of 20 Li-rich giants observed during the Gaia-ESO Survey, which includes the first nine Li-rich giant stars known towards the CoRoT fields. Most of our Li-rich giants have near-solar metallicities, and stellar parameters consistent with being before the luminosity bump. This is difficult to reconcile with deep mixing models proposed to explain lithium enrichment, because these models can only operate at later evolutionary stages: at or past the luminosity bump. In an effort to shed light on the Li-rich phenomenon, we highlight recent evidence of the tidal destruction of close-in hot Jupiters at the sub-giant phase. We note that when coupled with models of planet accretion, the observed destruction of hot Jupiters actually predicts the existence of Li-rich giant stars, and suggests Li-rich stars should be found early on the giant branch and occur more frequently with increasing metallicity. A comprehensive review of all known Li-rich giant stars reveals that this scenario is consistent with the data. However more evolved or metal-poor stars are less likely to host close-in giant planets, implying that their Li-rich origin requires an alternative explanation, likely related to mixing scenarios rather than external phenomena., This work is based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 188.B-3002. These data products have been processed by the Cambridge Astronomy Survey Unit (CASU) at the Institute of Astronomy, University of Cambridge, and by the FLAMES/UVES reduction team at INAF/Osservatorio Astrofisico di Arcetri. These data have been obtained from the $\textit{Gaia}$-ESO Survey Data Archive, prepared and hosted by the Wide Field Astronomy Unit, Institute for Astronomy, University of Edinburgh, which is funded by the UK Science and Technology Facilities Council. This work was partly supported by the European Union FP7 programme through ERC grant number 320360 and by the Leverhulme Trust through grant RPG-2012-541. We acknowledge the support from INAF and the Ministero dell'Istruzione, dell'Università e della Ricerca (MIUR) in the form of the grant Premiale VLT 2012 and the Chemical and Dynamical Evolution of the Milky Way and Local Group Galaxies (prot. 2010LY5N2T). The results presented here benefit from discussions held during the $\textit{Gaia}$-ESO workshops and conferences supported by the ESF (European Science Foundation) through the GREAT Research Network Programme. GR acknowledges support from the project grant ‘The New Milky Way’ from the Knut and Alice Wallenberg Foundation. GMK is supported by the Royal Society as a Royal Society University Research Fellow. LS acknowledges support provided by the Chilean Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to the Millennium Institute of Astrophysics, MAS. Funding for the Stellar Astrophysics Centre is provided by the Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement no. 267864). VSA acknowledges support from VILLUM FONDEN (research grant 10118). SLM acknowledges support from the Australian Research Council through DECRA fellowship DE140100598. TM acknowledges financial support from Belspo for contract PRODEX Gaia-DPAC. JM acknowledges the support from the European Research Council Consolidator Grant funding scheme (project STARKEY, G.A. no. 615604). This research has made use of the ExoDat Database, operated at LAM-OAMP, Marseille, France, on behalf of the CoRoT/Exoplanet programme. This research made use of astropy, a community-developed core python package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of NASA's Astrophysics Data System Bibliographic Services., This is the final version of the article. It first appeared from Oxford University Press via http://dx.doi.org/10.1093/mnras/stw1512
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- 2016
7. CNO abundances in giants of the peculiar globular cluster NGC 1851
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Arnas Drazdauskas, Gražina Tautvaišienė, E. Stonkutė, Elena Pancino, Carmela Lardo, Sarah L. Martell, Tautvaisiene G., Drazdauskas A., Lardo C., Martell S.L., Pancino E., and Stonkute E.
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Physics ,Stars: abundance ,Metallicity ,globular clusters: individual (NGC 1851) ,Astronomy ,Astronomy and Astrophysics ,Horizontal branch ,Blue straggler ,Spectral line ,Stars ,Space and Planetary Science ,Abundance (ecology) ,Globular cluster ,stars: evolution ,Spectrograph - Abstract
We provide CNO and Fe abundance investigations for a sample of up to 45 NGC 1851 giants. High-resolution spectra were obtained with the VLT UVES spectrograph in the framework of the Gaia-ESO Survey. The stars in our sample can be separated into two groups with a difference of 0.1 dex in the mean metallicity, 0.3 dex in the mean C/N, and no significant difference in the mean values of C+N+O.
- Published
- 2015
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