AmFm and lithium gap stars: Stellar evolution models with mass loss

@article{Vick2010AmFmAL,
  title={AmFm and lithium gap stars: Stellar evolution models with mass loss},
  author={M. Vick and G. Michaud and J. Richer and O. Richard},
  journal={arXiv: Solar and Stellar Astrophysics},
  year={2010}
}
A thorough study of the effects of mass loss on internal and surface abundances of A and F stars is carried out in order to constrain mass loss rates for these stars, as well as further elucidate some of the processes which compete with atomic diffusion. Self-consistent stellar evolution models of 1.3 to 2.5 M_sun stars including atomic diffusion and radiative accelerations for all species within the OPAL opacity database were computed with mass loss and compared to observations as well as… Expand
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References

SHOWING 1-10 OF 82 REFERENCES
The Evolution of AmFm Stars, Abundance Anomalies, and Turbulent Transport
Stellar evolution models of stars of 1.45-3.0 M☉ have been calculated, including the atomic diffusion of metals and radiative accelerations for all species in the OPAL opacities. As the abundancesExpand
AmFm Stars as a Test of Rotational Mixing Models
Stellar evolution models have been calculated for stars of 1.7-2.5 M☉ with both the Geneva-Toulouse and Montreal codes. In the Geneva-Toulouse code, the internal evolution of angular momentum isExpand
Models for solar abundance stars with gravitational settling and radiative accelerations: Application to M67 and NGC 188
Evolutionary models taking into account radiative accelerations, thermal diffusion, and gravitational settling for 28 elements, including all those contributing to OPAL stellar opacities, have beenExpand
Abundance Anomalies in Horizontal Branch Stars and Atomic Diffusion
Using stellar evolution models in which atomic diffusion was included self-consistently throughout the evolution of a Population II 0.8 M☉ star (Y = 0.2352, Z = 0.0001, α = 0.3) from the zero-ageExpand
Consistent Evolution of F Stars: Diffusion, Radiative Accelerations, and Abundance Anomalies
Consistent stellar evolution models of F stars (1.1-1.5 M☉) are calculated with radiative forces, opacities, and diffusion for all elements included in OPAL's opacity tables. The opacities andExpand
The lithium abundance in stars
The observations of Li abundances in pre-Main-Sequence, Main-Séquence (Population I and II), sub-giant, and giant stars are reviewed in order to show how Li can be used as a constraint on stellarExpand
Chemical composition of A and F dwarfs members of the Hyades open cluster
Aims. Abundances of 15 chemical elements have been derived for 28 F and 16 A stars members of the Hyades open cluster in order to set constraints on self-consistent evolutionary models that includeExpand
Mass-loss and diffusion in subdwarf B stars and hot white dwarfs: do weak winds exist?
Context. According to previous investigations, the effect of diffusion in the stellar atmospheres and envelopes of hot white dwarfs and subdwarf B (sdB) stars strongly depends on the presence of weakExpand
Stringent limits on the ionized mass loss from A and F dwarfs
Following the suggestion of Willson et al. (1987) that A- and F-type main-sequence stars might undergo significant mass loss due to pulsationally driven winds, upper limits to the ionized mass lossExpand
Implications of WMAP Observations on Li Abundance and Stellar Evolution Models
The Wilkinson Microwave Anisotropy Probe (WMAP) determination of the baryon-to-photon ratio implies, through big bang nucleosynthesis, a cosmological Li abundance larger, by a factor of 2-3, than theExpand
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