Rotating stellar models of low-mass, pre-main sequence stars with an imposed magnetic field

Mendes Luiz, luizt@cpdee.ufmg.br, Departamento de Eng. Eletronica, Universidade Federal de Minas Gerais, Brazil
Landin Natalia, nlandin@ufv.br, Departamento de Fisica, Universidade Federal de Vicosa
Vaz Luiz, vaz@fisica.ufmg.br, Departamento de Fisica, Universidade Federal de Minas Gerais

Abstract
The ATON 2.3 stellar evolution code has been improved in order to fully incorporate the effects of a magnetic field on the stellar structure and evolution. The technique introduced by Lydon & Sofia (1996), which modifies the equations of stellar structure and also the mixing-length theory, was adopted for that purpose; due to the one-dimensional nature of the ATON code, only some simplified magnetic field geometries can be explored. In this context, stellar models of rotating, low-mass stars have been computed in order to investigate the effects of a radially-varying imposed magnetic field, covering both the pre-main sequence and the main-sequence phases. Here we report preliminary results on some stellar properties of those models, with particular emphasis on the magnetic field impact on convection and the associated lithium depletion.