منابع مشابه
Lithium abundances in halo dwarfs
The pioneering observations of Spite & Spite showed lithium abundances in halo dwarfs to be almost uniform, irrespective of metallicity and mass over a range of effective temperatures from ∼5600 K up to the main-sequence turnoff. They inferred that the observed abundance was “hardly altered” from that produced in the hot Big Bang. Subsequent efforts have endeavoured to determine how small or la...
متن کاملLithium abundances in the old open cluster NGC 3960 from VLT/FLAMES observations
Context. Old open clusters are very useful targets to investigate mechanisms responsible for lithium (Li) depletion during the main sequence. Comparison of the Li abundances in clusters of different age allows us to understand the efficiency of the Li destruction process. Aims. Our goal is the determination of membership and Li abundance in a sample of candidate members of the open cluster NGC ...
متن کاملLithium abundances in exoplanet-host stars : modelling
Aims. Exoplanet-host stars (EHS) are known to present superficial chemical abundances different from those of stars without any detected planet (NEHS). EHS are, on the average, overmetallic compared to the Sun. The observations also show that, for cool stars, lithium is more depleted in EHS than in NEHS. The aim of this paper is to obtain constraints on possible models able to explain this diff...
متن کاملInternal Rotation, Mixing and Lithium Abundances
Lithium is an excellent tracer of mixing in stars as it is destroyed (by nuclear reactions) at a temperature around ∼ 2.5 × 10 K. The lithium destruction zone is typically located in the radiative region of a star. If the radiative regions are stable, the observed surface value of lithium should remain constant with time. However, comparison of the meteoritic and photospheric Li abundances in t...
متن کاملYields from Low Metallicity, Intermediate Mass Agb Stars: Their Role for the Cno and Lithium Abundances in Globular Cluster Stars
We present the results of extensive computation of the Thermal Pulse phase AGB evolution of stars of metallicities in mass fraction 2 10 ?4 Z 0:01, for those masses in the range 2:5 M=M 6, which suuer the Hot Bottom Burning (HBB) phase. The evolution is fully computed, by assuming a mass loss rate consistent with the observations of the Magellanic Clouds lithium rich stars, and modelling convec...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2010
ISSN: 0035-8711
DOI: 10.1111/j.1365-2966.2010.17630.x