Coronal bright points (CBPs) are small-scale and long-duration brighteningsin the lower solar corona. They are often explained in terms of magneticreconnection. We aim to study the sub-structures of a CBP and clarify therelationship among the brightenings of different patches inside the CBP. Theevent was observed by the X-ray Telescope (XRT) aboard the Hinode spacecraft on2009 August 22$-$23. The CBP showed repetitive brightenings (or CBP flashes).During each of the two successive CBP flashes, i.e., weak and strong flasheswhich are separated by $\sim$2 hr, the XRT images revealed that the CBP wascomposed of two chambers, i.e., patches A and B. During the weak flash, patch Abrightened first, and patch B brightened $\sim$2 min later. During thetransition, the right leg of a large-scale coronal loop drifted from the rightside of the CBP to the left side. During the strong flash, patch B brightenedfirst, and patch A brightened $\sim$2 min later. During the transition, theright leg of the large-scale coronal loop drifted from the left side of the CBPto the right side. In each flash, the rapid change of the connectivity of thelarge-scale coronal loop is strongly suggestive of the interchangereconnection. For the first time we found reciprocatory reconnection in theCBP, i.e., reconnected loops in the outflow region of the first reconnectionprocess serve as the inflow of the second reconnection process.
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