标题： 活动区通量管在湍流太阳对流包层中的兴起 显示英文标题

标题： The Rise of Active Region Flux Tubes in the Turbulent Solar Convective Envelope

摘要： 我们使用一个细长通量管模型，在旋转的湍流对流壳层中研究活动区尺度的通量管如何从对流层底部浮力上升至接近太阳表面。 我们在对流层底部研究环形通量管，初始纬度范围从1度到40度，磁场强度从15千高斯到100千高斯，总通量为10^22 Mx。 我们发现，随着初始磁场强度从15千高斯增加到100千高斯，通量管的动力学演化从对流主导变为磁浮力主导。 在100千高斯时，Ω形上升环的形成主要由磁浮力不稳定性的发展控制。 然而，在低磁场强度15千高斯时，上升的Ω形环的形成主要由对流流动控制，与没有对流的情况下的先前结果相比，浮现环的特性发生了显著变化。 有对流存在时，上升时间大幅减少（从几年减少到几个月），环能够在低纬度浮现，且对于初始磁场强度大于或等于40千高斯的环，浮现环的倾斜角度符合乔伊定律。 我们还检查了浮现环的前导腿和后随腿之间出现的其他不对称性。 综合所有结果，我们发现中等磁场强度约为40-50千高斯产生的浮现环最符合太阳活动区的观测特性。 显示英文摘要

摘要： We use a thin flux tube model in a rotating spherical shell of turbulent convective flows to study how active region scale flux tubes rise buoyantly from the bottom of the convection zone to near the solar surface. We investigate toroidal flux tubes at the base of the convection zone with field strengths ranging from 15 kG to 100 kG at initial latitudes ranging from 1 degree to 40 degrees with a total flux of 10^22 Mx. We find that the dynamic evolution of the flux tube changes from convection dominated to magnetic buoyancy dominated as the initial field strength increases from 15 kG to 100 kG. At 100 kG, the development of Omega-shaped rising loops is mainly controlled by the growth of the magnetic buoyancy instability. However, at low field strengths of 15 kG, the development of rising Omega-shaped loops is largely controlled by convective flows, and properties of the emerging loops are significantly changed compared to previous results in the absence of convection. With convection, rise times are drastically reduced (from years to a few months), loops are able to emerge at low latitudes, and tilt angles of emerging loops are consistent with Joy's Law for initial field strengths of greater than or equal to 40 kG. We also examine other asymmetries that develop between the leading and following legs of the emerging loops. Taking all the results together, we find that mid-range field strengths of approximately 40 - 50 kG produce emerging loops that best match the observed properties of solar active regions.