标题： 太阳耀斑中的能量释放率和重联率测量 显示英文标题

标题： Measurement of the Energy Release Rate and the Reconnection Rate in Solar Flares

摘要： 利用伊部等（2002年）提出的方法，确定了三次双带状耀斑爆发相的无量纲重联速度Vin/Va，其中Vin是重联流入速度，Va是阿尔芬速度。无量纲重联速度对于约束磁重联的理论模型非常重要。为了减少重联速度的不确定性，从观测数据中尽可能准确地确定耀斑的能量释放率是至关重要的。为此，我们对一次耀斑环进行了单维流体动力学模拟，并合成了由Yohkoh卫星上的软X射线望远镜（SXT）探测到的计数率。我们发现，根据SXT数据推导出的耀斑拱形结构热能含量的时间导数比实际能量释放率小0.3至0.8倍，这取决于环的长度和能量释放率。模拟结果在文中给出，并用于计算重联速度。我们发现，2000年11月24日的X2.3级耀斑的重联速度为0.047，2000年7月14日的M3.7级耀斑为0.015，2000年11月16日的C8.9级耀斑为0.071。这些值与横山等（2001年）通过直接观测重联流入得到的结果相似，并且与Petschek（1964年）提出的快速重联模型一致。 显示英文摘要

摘要： By using the method presented by Isobe et al. (2002), the non-dimensional reconnection rate Vin/Va has been determined for the impulsive phase of three two-ribbon flares, where Vin is the velocity of the reconnection inflow and Va is the Alfven velocity. The non-dimensional reconnection rate is important to make a constraint on the theoretical models of magnetic reconnection. In order to reduce the uncertainty of the reconnection rate, it is important to determine the energy release rate of the flares from observational data as accurately as possible. To this end, we have carried out one dimensional hydrodynamic simulations of a flare loop and synthesized the count rate detected by the soft X-ray telescope (SXT) aboard Yohkoh satellite. We found that the time derivative of the thermal energy contents in a flare arcade derived from SXT data is smaller than the real energy release rate by a factor of 0.3 - 0.8, depending on the loop length and the energy release rate. The result of simulation is presented in the paper and used to calculate the reconnection rate. We found that reconnection rate is 0.047 for the X2.3 flare on 2000 November 24, 0.015 for the M3.7 flare on 2000 July 14, and 0.071 for the C8.9 flare on 2000 November 16. These values are similar to that derived from the direct observation of the reconnection inflow by Yokoyama et al. (2001), and consistent with the fast reconnection models such as that of Petschek (1964).