We investigate the onset conditions for direct resistive heating instabilities coupled with radiative processes within a twisted magnetic flux rope of axisymmetry and relate the helical patterns wrapping along the rope initiated by such instabilities to the collective appearance of compact X‐ray loops in a certain phase of active region development in the solar corona. Since the emergence and the subsequent evolution of a gigantic magnetic flux rope in the solar atmosphere involve complicated physical processes, it is expected that such instabilities occurring in an ensemble of many current sheaths embedded in a stressed, twisted, and bulged magnetic flux rope will manifest as collective X‐ray loop structures on various spatial scales and with varieties of large‐scale morphologies.