On MHD rotational transport,instabilities and dynamo action in stellar radiation zones
Magnetic field is an essential dynamical process in stellar radiation zones. Moreover,it has been suggested that a dynamo action,sustained by a MHD instability which affects the toroidal axisymmetric magnetic field,could lead to a strong transport of angular momentum and of chemicals in such regions. Here,we recall the different magnetic transport and mixing processes in radiative regions. Next,we show that the dynamo cannot operate as described by Spruit (2002) and recall the condition required to close the dynamo loop. We perform high-resolution 3D simulations with the ASH code,where we observe indeed the MHD instability,but where we do not detect any dynamo action,contrary to J. Braithwaite (2006). We conclude on the picture we get for magnetic transport mechanisms in radiation zones and the associated consequences for stellar evolution.
MHD Sun:magnetic fields Sun:interior stars:magnetic fields stars:interiors
S.Mathis J.-P.Zahn A.-S.Brun
Laboratoire AIM,CEA/DSM-CNRS-Universite Paris Diderot,IRFU/Sap,F-91191 Gif-sur-Yvette Cedex,France;L LUTH,Observatoire de Paris-CNRS-Université Paris Diderot,5 Place Jules Janssen,F-92195 Meudon Cedex,
国际会议
The 252th Symposium of the International Astronomical Union(国际天文学联合会第252届研讨会)
海南三亚
英文
255-256
2008-04-06（万方平台首次上网日期，不代表论文的发表时间）