Towards a 3D dynamo model of the PMS star BP Tau

被引：7

作者：

Bessolaz, N. ^{[1
]}

Brun, A. S. ^{[1
]}

机构：

[1] Irfu Univ Paris Diderot CNRS, Lab AIM Paris Saclay, CEA, INSU, F-91191 Gif Sur Yvette, France

来源：

ASTRONOMISCHE NACHRICHTEN | 2011年 / 332卷 / 9-10期

基金：

欧洲研究理事会;

关键词：

convection; magnetohydrodynamics (MHD); stars: individual (BP Tau); stars: pre-main sequence; stars: rotation; T Tauri stars; turbulence; MAGNETOSPHERIC ACCRETION; DIFFERENTIAL ROTATION; TURBULENT CONVECTION; STELLAR EVOLUTION; MAGNETIC-FIELDS; SIMULATIONS;

D O I：

10.1002/asna.201111612

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Studying how convective and magnetic properties of pre-main sequence stars change during their evolution towards the zero-age main sequence is a growing area of research triggered by the development of efficient spectropolarimeters. 3D simulations can help to identify the key parameters to understand the diversity (strength, topology) of magnetic fields observed. We present results of a dynamo computation done with the ASH code for a 0.7 M-circle dot pre-main sequence star with a 7.6 day rotation period which is nearly fully convective, using a realistic stratification contrast to resolve 90% of the convective zone. This star corresponds to the target star BP Tau already observed with spectropolarimetry (Donati et al. 2008). We particularly compare the magnetic field properties found in our simulation with the observational constraints. (C) 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim

引用

页码：1045 / 1051

页数：7

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