Models of Stellar structure for asteroseismology

Simple item page
dc.creatorD'Antona, F.
dc.creatorMontalban, J.
dc.creatorMazzitelli, I.
dc.date2004-09-07
dc.date.accessioned2026-07-07T02:14:29Z
dc.date.available2026-07-07T02:14:29Z
dc.descriptionAmong the problems still open in the study of stellar structure, we discuss in particular some issues related to the study of convection. We have recently built up complete stellar models, adopting a consistent formulation of convection both in the non gray atmosphere and in the interior, to be used for non adiabatic pulsational analysis, and discuss in some details two problems which have been clarified by these models: the physical interpretation of one of the main sequence "Boehm-Vitense gaps", and the necessity of parametrizing pre main sequence convection differently from the main sequence convection. We also report preliminary results of the application to the solar model of the non--local turbulence equations by Canuto and Dubovikov (1998) in the down-gradient approximation.
dc.description10 pages and 11 figures, invited talk at the 2nd Eddington Workshop 'Stellar Structure and Habitable Planet Finding', Palermo, 9-11 April 2003
dc.identifierhttps://arxiv.org/abs/astro-ph/0409146
dc.identifierhttp://arxiv.org/abs/astro-ph/0409146
dc.identifierpublished in 'Stellar Structure and Habitable Planet Finding', ESA SP-530, Jan. 2004, F. Favata, S. Aigrain eds., p. 13-22
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8132
dc.subjectAstrophysics
dc.titleModels of Stellar structure for asteroseismology
dc.typetext

Files

Collections

arXiv