论文标题
太阳和恒星耀斑：频率，活动区域和恒星发电机
Solar and stellar flares: frequency, active regions and stellar dynamo
论文作者
论文摘要
我们证明，对于弱耀斑，对斑点的依赖可能相当薄弱。事实是，这种耀斑可以在小型和大型活性区域发生。同时，在大型活跃地区，强大的大型类M和X发生频率更高。在能量估计中，星空中的平均磁场也可以假定等于黑子umbra中的平均磁场。因此，有效的平均磁场为900 mx/cm $^2 $在黑子和2000 mx/cm $^2 $ in Starpots中。此外，能量存储的高度不能与$^{1/2} $完全成比例。对于恒星，拟合因子是较小的数量级。对M和X类强大的太阳X射线耀斑的发生率和星星上的超级弹药的分析表明，随着斑点和活动区域的斑点差异的津贴，可以通过单个模型来描述这两个集合。因此，恒星上的超级流域及其在太阳上的缺失降低到发电机机制有效性差异的问题。
We demonstrate that for weak flares the dependence on spottedness can be rather weak. The fact is that such flares can occur both in small and large active regions. At the same time, powerful large flares of classes M and X occur much more often in large active regions. In energy estimates, the mean magnetic field in starspots can also be assumed equal to the mean field in the sunspot umbra. So the effective mean magnetic field is 900 Mx/cm$^2$ in sunspots and 2000 Mx/cm$^2$ in starspots. Moreover, the height of the energy storage cannot be strictly proportional to A$^{1/2}$. For stars, the fitting factor is an order of magnitude smaller. The analysis of the occurrence rate of powerful solar X-ray flares of class M and X and superflares on stars shows that, with allowance for the difference in the spottedness and compactness of active regions, both sets can be described by a single model. Thus, the problem of superflares on stars and their absence on the Sun is reduced to the problem of difference in the effectiveness of the dynamo mechanisms.
