太阳子午流速度和磁通量传输
Speed of Meridional Flows and Magnetic Flux Transport on the Sun
摘要：
我们利用磁蝶图来确定太阳表面向两极的磁通量传输速度。通量传输的表现形式是从太阳黑子带延伸到极地地区的细长结构。这些结构的斜率被测量和解释为纬向磁通量传输速度。在3.5- 12微米深度上，与时距日震学测量的纬向流平均速度比较，大体上是一致的，但在磁场所占的区域，通量输送和纬向流的速度有很大的不同。活动区附近的局地环流，特别是活动区赤道一侧的强向赤道气流，影响日震学计算的平均速度廓线，但不影响磁通量输运。结果表明，在太阳发电机模型中，不能直接采用日震学测量的平均纵向平均纬向流来描述磁通量输运，而必须考虑这些流的纵向结构。
英文摘要：
We use the magnetic butterfly diagram to determine the speed of the magnetic flux transport on the solar surface towards the poles. The manifestation of the flux transport is clearly visible as elongated structures extended from the sunspot belt to the polar regions. The slopes of these structures are measured and interpreted as meridional magnetic flux transport speed. Comparison with the time-distance helioseismology measurements of the mean speed of the meridional flows at the depth of 3.5--12 Mm shows a generally good agreement, but the speeds of the flux transport and the meridional flow are significantly different in areas occupied by the magnetic field. The local circulation flows around active regions, especially the strong equatorward flows on the equatorial side of active regions affect the mean velocity profile derived by helioseismology, but do not influence the magnetic flux transport. The results show that the mean longitudinally averaged meridional flow measurements by helioseismology may not be used directly in solar dynamo models for describing the magnetic flux transport, and that it is necessary to take into account the longitudinal structure of these flows.
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