Casey, AR and Ruchti, G and Masseron, T and Randich, S and Gilmore, G and Lind, K and Kennedy, GM and Koposov, SE and Hourihane, A and Franciosini, E and Lewis, JR and Magrini, L and Morbidelli, L and Sacco, GG and Worley, CC and Feltzing, S and Jeffries, RD and Vallenari, A and Bensby, T and Bragaglia, A and Flaccomio, E and Francois, P and Korn, AJ and Lanzafame, A and Pancino, E and Recio-Blanco, A and Smiljanic, R and Carraro, G and Costado, MT and Damiani, F and Donati, P and Frasca, A and Jofre, P and Lardo, C and de Laverny, P and Monaco, L and Prisinzano, L and Sbordone, L and Sousa, SG and Tautvaisiene, G and Zaggia, S and Zwitter, T and Delgado Mena, E and Chorniy, Y and Martell, SL and Aguirre, VS and Miglio, A and Chiappini, C and Montalban, J and Morel, T and Valentini, M (2016) The Gaia-ESO Survey: revisiting the Li-rich giant problem. Monthly Notices of the Royal Astronomical Society, 461 (3). 3336 - 3352. ISSN 1365-2966

R Jeffries - The Gaia ESO Survey - revisiting the Li-rich giant problem.pdf - Published Version

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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 that 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.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society
Uncontrolled Keywords: stars, abundances
Subjects: Q Science > QB Astronomy > QB460 Astrophysics
Q Science > QB Astronomy > QB799 Stars
Divisions: Faculty of Natural Sciences > School of Physical and Geographical Sciences
Related URLs:
Depositing User: Symplectic
Date Deposited: 07 Nov 2016 15:20
Last Modified: 06 Nov 2017 11:29

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