The magnetic structure of a coronal X-ray bright point

X-ray bright points are small dynamic loop structures that are observed all over the solar corona. The high spatial and temporal resolution of the TRA CE instrument allows bright points to be studied in much greater detail tha n previously possible. This paper focuses on a specific bright point which occurred for about 20 hours on 13-14 June 1998 and examines its dynamic str ucture in detail. This example suggests that the mechanisms that cause brig ht points to form and evolve are more complex than previously thought. In t his case, reconnection probably plays a major part during the formation and brightening of the loop structure. However, later on the foot points rotat e injecting twist into the bright point which may cause an instability to o ccur with dynamic results.