Volume 521, October 2010
|Number of page(s)||26|
|Section||Stellar structure and evolution|
|Published online||21 October 2010|
AmFm and lithium gap stars
Stellar evolution models with mass loss
GRAAL UMR 5024, Université Montpellier II,
CC072, Place E. Bataillon,
34095 Montpellier Cedex 05,
2 Département de physique, Université de Montréal, Montréal, Québec, H3C 3J7, Canada e-mail: [mathieu.vick;jacques.richer]@umontreal.ca; email@example.com; firstname.lastname@example.org
3 LUTH, Observatoire de Paris, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
Accepted: 13 June 2010
Aims. 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.
Methods. Self-consistent stellar evolution models of 1.3 to 2.5 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 previous calculations with turbulent mixing.
Results. Models with unseparated mass loss rates between 5 × 10-14 and 10-13 reproduce observations for many cluster AmFm stars as well as Sirius A and o Leonis. These models also explain cool Fm stars, but not the Hyades lithium gap. Like turbulent mixing, these mass loss rates reduce surface abundance anomalies; however, their effects are very different with respect to internal abundances. For most of the main-sequence lifetime of an A or F star, surface abundances in the presence of such mass loss depend on separation which takes place between log ΔM/M* = -6 and -5.
Conclusions. The current observational constraints do not allow us to conclude that mass loss is to be preferred over turbulent mixing (induced by rotation or otherwise) in order to explain the AmFm phenomenon. Internal concentration variations which could be detectable through asteroseismic tests should provide further information. If atomic diffusion coupled with mass loss are to explain the Hyades Li gap, the wind would need to be separated.
Key words: diffusion / stars: mass-loss / stars: evolution / stars: chemically peculiar / stars: abundances / open clusters and associations: individual: Hyades
© ESO, 2010
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.