恒星对流区底部附近的抗磁泵
Diamagnetic pumping near the base of a stellar convection zone
摘要：
导电流体中的非均匀湍流将大尺度磁场沿湍流强度减小的方向排出，这一性质对恒星对流区底部附近的磁场动力学具有重要意义。向下的反磁泵限制了辐射核中的化石内部磁场，使得场的几何形状适合于形成太阳速跃层。对于太阳年龄的恒星，只有当对流区的湍流磁扩散率与辐射区的（微观或湍流）扩散率之比大于10^5时，抗磁约束才是有效的。年轻恒星的禁闭需要更大的扩散率比。因此，对年轻太阳型恒星持续磁场结构的观测可以为恒星内部不存在近红外线和辐射核中湍流水平提供证据。
英文摘要：
The property of inhomogeneous turbulence in conducting fluids to expel large-scale magnetic fields in the direction of decreasing turbulence intensity is shown as important for the magnetic field dynamics near the base of a stellar convection zone. The downward diamagnetic pumping confines a fossil internal magnetic field in the radiative core so that the field geometry is appropriate for formation of the solar tachocline. For the stars of solar age, the diamagnetic confinement is efficient only if the ratio of turbulent magnetic diffusivity of the convection zone to the (microscopic or turbulent) diffusivity of the radiative interiour is larger than 10^5. Confinement in younger stars require still larger diffusivity ratio. The observation of persistent magnetic structures on young solar-type stars can thus provide evidences for the nonexistence of tachoclines in stellar interiors and on the level of turbulence in radiative cores.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
