Volume 598, February 2017
|Number of page(s)||7|
|Published online||01 February 2017|
Evolution of lithium abundance in the Sun and solar twins
1 Université de La Côte d’Azur, OCA, Laboratoire Lagrange CNRS, BP. 4229, 06304 Nice Cedex, France
2 Sternberg Astronomical Institute, Lomonosov Moscow State University, 119992 Moscow, Russia
Received: 23 July 2016
Accepted: 8 November 2016
Evolution of the 7Li abundance in the convection zone of the Sun during different stages of its life time is considered to explain its low photospheric value in comparison with that of the solar system meteorites. Lithium is intensively and transiently burned in the early stages of evolution (pre-main sequence, pMS) when the radiative core arises, and then the Li abundance only slowly decreases during the main sequence (MS). We study the rates of lithium burning during these two stages. In a model of the Sun, computed ignoring pMS and without extra-convective mixing (overshooting) at the base of the convection zone, the lithium abundance does not decrease significantly during the MS life time of 4.6 Gyr. Analysis of helioseismic inversions together with post-model computations of chemical composition indicates the presence of the overshooting region and restricts its thickness. It is estimated to be approximately half of the local pressure scale height (0.5HP) which corresponds to 3.8% of the solar radius. Introducing this extra region does not noticeably deplete lithium during the MS stage. In contrast, at the pMS stage, an overshooting region with a value of approximately 0.18HP is enough to produce the observed lithium depletion. If we conclude that the dominant lithium burning takes place during the pMS stage, the dispersion of the lithium abundance in solar twins is explained by different physical conditions, primarily during the early stage of evolution before the MS.
Key words: Sun: abundances / Sun: interior / Sun: evolution / stars: solar-type
© ESO, 2017
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