Uncertainties in models of stellar structure and evolution
arXiv:1409.2281 · doi:10.1007/978-3-319-10993-0_19
Abstract
Numerous physical aspects of stellar physics have been presented in Ses- sion 2 and the underlying uncertainties have been tentatively assessed. We try here to highlight some specific points raised after the talks and during the general discus- sion at the end of the session and eventually at the end of the workshop. A table of model uncertainties is then drawn with the help of the participants in order to give the state of the art in stellar modeling uncertainties as of July 2013.
Proc. of the workshop "Asteroseismology of stellar populations in the Milky Way" (Sesto, 22-26 July 2013), Astrophysics and Space Science Proceedings, (eds. A. Miglio, L. Girardi, P. Eggenberger, J. Montalban)
References in corpus (7)
- Thermohaline mixing: A physical mechanism governing the photospheric composition of low-mass giants
- Deep Mixing of He-3: Reconciling Big Bang and Stellar Nucleosynthesis
- An asteroseismic signature of helium ionization
- The First Empirical Mass Loss Law for Population II Giants
- Inhibition of thermohaline mixing by a magnetic field in Ap star descendants: Implications for the Galactic evolution of 3He
- Prospects for asteroseismic inference on the envelope helium abundance in red giant stars
- Modelling the components of binaries in Hyades: The dependence of the mixing-length parameter on stellar mass