We report a statistical study of flares observed with the Soft X-Ray Telescope (SXT) on board Yohkoh in the year 2000. We measure physical parameters of 77 flares, such as the temporal scale, size, and magnetic flux density, and find that the sizes of flares tend to be distributed more broadly as the GOES class becomes weaker and that there is a lower limit of magnetic flux density that depends on the GOES class. We also examine the relationships among these parameters and find weak correlation between the temporal and spatial scales of the flares. We estimate reconnection inflow velocity, coronal Alfvén velocity, and reconnection rate using the observed values. The inflow velocities are distributed from a few km s-1 to several tens of km s-1, and the Alfvén velocities in the corona are in the range from 103 to 104 km s-1. Hence, the reconnection rate is 10-3 to 10-2. We find that the reconnection rate in a flare tends to decrease as the GOES class of the flare increases. This value is within 1 order of magnitude of the theoretical maximum value predicted by the Petschek model, although the dependence of the reconnection rate on the magnetic Reynolds number tends to be stronger than that in the Petschek model.
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机译:我们报告了用软X射线望远镜(SXT)在Yohkoh于2000年观测到的耀斑的统计研究。我们测量了77个耀斑的物理参数,例如时间尺度,大小和磁通密度,发现随着GOES等级变弱,火炬的大小往往会分布得更广泛,并且取决于GOES等级的磁通密度的下限也有所降低。我们还检查了这些参数之间的关系,并发现了耀斑的时空尺度之间的弱相关性。我们使用观测值估算重新连接的流入速度,冠状Alfvén速度和重新连接率。流入速度从几公里s-1分布到几十公里s-1,电晕中的Alfvén速度在103到104 km s-1范围内。因此,重新连接速率为10-3至10-2。我们发现,火炬的重新连接率会随着火炬的GOES类的增加而降低。尽管重新连接速率对磁雷诺数的依赖性往往比在Petschek模型中强,但此值在Petschek模型所预测的理论最大值的1个数量级内。
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