磁特征跟踪，是什么决定了速度？
Magnetic feature tracking, what determines the speed?
摘要：
最近的观测表明，太阳表面丰富的小磁性元素以低于等离子体速度$U_θ$的速度向极移动。Guerrero等人（2011）将这种差异解释为$|U_θ|$的正径向梯度导致磁性元素扩散扩散的结果。由于梯度的符号（由当地日震学推断）仍然不清楚，本文研究了具有负梯度的情况。在这种情况下，磁示踪剂的速度比等离子体的速度大，与观测结果不一致。提出了独立解释它们的替代机制。对于湍流磁抽运，它表明，它必须是不切实际的强大，以协调模型与观测。
英文摘要：
Recent observations revealed that small magnetic elements abundant at the solar surface move poleward with a velocity which seems to be lower than the plasma velocity $U_θ$. Guerrero et al. (2011) explained this discrepancy as a consequence of diffusive spreading of the magnetic elements due to a positive radial gradient of $|U_θ|$. As the gradient's sign (inferred by local helioseismology) is still unclear, cases with a negative gradient are studied in this paper. Under this condition, the velocity of the magnetic tracers turns out to be larger than the plasma velocity, in disagreement with the observations. Alternative mechanisms for explaining them independently are proposed. For the turbulent magnetic pumping it is shown that it has to be unrealistically strong to reconcile the model with the observations.
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