标题： 对流区中的磁场 显示英文标题

标题： The Magnetic Field in the Convection Zone

摘要： 太阳物理学中尚未解决的关键问题之一是关于对流层底部磁场强度及其分布的问题。 磁通管的动力学要求对流层底部存在强度高达10万高斯的环向磁场。 动能与磁场能量的等效性论证则导致了较小的场强估算。 为了用 helioseismic 方法可能探测到这些相对较小（与压力效应相比）的场强，了解场强范围及其分布是很重要的。 我们利用球壳中的发电机模拟来估计对流层底部环向磁场强度的范围。 这些模拟包含了由 GONG 和 MDI 数据的 helioseismic 反演所提供的旋转分布。 结合模拟与观测到的表面径向磁场，我们提取了对流层底部平均环向磁场的空间模式和强度。 显示英文摘要

摘要： One of the key questions in solar physics that remains to be answered concerns the strength and the distribution of the magnetic fields at the base of the convection zone. The flux tube dynamics requires that toroidal fields of strength as large as 100 kilogauss be present at the base of the convection zone. The kinetic-magnetic equipartition argument leads to smaller field strengths. For possible detection of these relatively small (compared to pressure effects) fields by helioseismic methods it is important to know the range of the field strengths and their distribution. We estimate a range for the toroidal magnetic field strengths at the base of the convection zone using dynamo simulations in a spherical shell. These simulations involve the distribution of rotation provided by helioseismic inversions of the GONG and MDI data. Combining the simulations with the observed line-of-sight surface poloidal field we extract the spatial pattern and magnitude of the mean toroidal magnetic field at the base of the convection zone.