A quantitative measure of the structure of gamma‐ray burst time profiles

A cursory examination of cosmic gamma‐ray burst time profiles indicates an inhomogeneous distribution of structure. In the first approximation, there seem to be two types of profiles; smooth ones with little structure and highly variable ones with lots of structure. To put this observation to the test, we have examined the statistical nature of the profile derivative to choose which parameter might best be called the burst ‘‘spikiness.’’ We have found that a good estimator is given by a count of the number of ‘‘spikes’’ (defined by a specific numerical recipe) and not by the rms deviations from either a pre‐burst background or any type of moving average background. The application of this parameter to 30 burst time histories shows it to be consistent over a wide range of profile types. The analysis also reveals a preferred average time between spikes of approximately 1.5 seconds.