PERSISTENT MAGNETIC WREATHS IN A RAPIDLY ROTATING SUN

被引:179
作者
Brown, Benjamin P. [1 ,2 ]
Browning, Matthew K. [3 ]
Brun, Allan Sacha [4 ,5 ]
Miesch, Mark S. [6 ]
Toomre, Juri [1 ,2 ]
机构
[1] Univ Colorado, JILA, Boulder, CO 80309 USA
[2] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA
[3] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada
[4] Univ Paris 07, CNRS, CEA, UMR AIM, F-91191 Gif Sur Yvette, France
[5] CEA Saclay, DSM, IRFU, SAp, F-91191 Gif Sur Yvette, France
[6] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA
基金
美国国家科学基金会; 欧洲研究理事会;
关键词
convection; magnetohydrodynamics (MHD); stars: interiors; stars: magnetic field; stars: rotation; Sun: interior; FLUX TRANSPORT DYNAMO; SOLAR DIFFERENTIAL ROTATION; FULLY CONVECTIVE STARS; MAIN-SEQUENCE STARS; LARGE-SCALE DYNAMOS; DIGITAL SKY SURVEY; X-RAY-EMISSION; LOW-MASS STARS; TURBULENT CONVECTION; ANGULAR-MOMENTUM;
D O I
10.1088/0004-637X/711/1/424
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
When our Sun was young it rotated much more rapidly than now. Observations of young, rapidly rotating stars indicate that many possess substantial magnetic activity and strong axisymmetric magnetic fields. We conduct simulations of dynamo action in rapidly rotating suns with the three-dimensional magnetohydrodynamic anelastic spherical harmonic (ASH) code to explore the complex coupling between rotation, convection, and magnetism. Here, we study dynamo action realized in the bulk of the convection zone for a system rotating at 3 times the current solar rotation rate. We find that substantial organized global-scale magnetic fields are achieved by dynamo action in this system. Striking wreaths of magnetism are built in the midst of the convection zone, coexisting with the turbulent convection. This is a surprise, for it has been widely believed that such magnetic structures should be disrupted by magnetic buoyancy or turbulent pumping. Thus, many solar dynamo theories have suggested that a tachocline of penetration and shear at the base of the convection zone is a crucial ingredient for organized dynamo action, whereas these simulations do not include such tachoclines. We examine how these persistent magnetic wreaths are maintained by dynamo processes and explore whether a classical mean-field alpha-effect explains the regeneration of poloidal field. We find that the global-scale toroidal magnetic fields are maintained by an Omega-effect arising from the differential rotation, while the global-scale poloidal fields arise from turbulent correlations between the convective flows and magnetic fields. These correlations are not well represented by an alpha-effect that is based on the kinetic and magnetic helicities.
引用
收藏
页码:424 / 438
页数:15
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