Young
stellar clusters are thought to form in small groups which merge into a final
cluster. One method to computationally test this theory is using numeric
quantities such as the fractal dimension or minimum separation of members to
measure the "clumpiness" of star clusters of different ages. In this
work, I analyze the structure of simulated systems by calculating the fractal
dimension and the Q parameter of these clusters during
formation and early evolution in their natal gas clouds. I then attempt to
correlate changes in these quantities to structural changes in the young
clusters.
