Dynamical evolution of fractal structures in star-forming regions

The Q-parameter is used extensively to quantify the spatial distributions of stars and gas in star-forming regions as well as older clusters and associations. It quantifies the amount of structure using the ratio of the average length of the minimum spanning tree, (m) over bar, to the average length within the complete graph, (s) over bar. The interpretation of the Q-parameter often relies on comparing observed values of Q, (m) over bar, and (s) over bar to idealized synthetic geometries, where there is little or no match between the observed star-forming regions and the synthetic regions. We measure Q, (m) over bar, and (s) over bar over 10Myr in N-body simulations, which are compared to IC 348, NGC 1333, and the ONC. For each star-forming region, we set up simulations that approximate their initial conditions for a combination of different virial ratios and fractal dimensions. We find that the dynamical evolution of idealized fractal geometries can account for the observed Q,(m) over bar, and (s) over bar values in nearby star-forming regions. In general, an initially fractal star-forming region will tend to evolve to become more smooth and centrally concentrated. However, we show that different initial conditions, as well as where the edge of the region is defined, can cause significant differences in the path that a star-forming region takes across the (m) over bar-(s) over bar plot as it evolves. We caution that the observed Q-parameter should not be directly compared to idealized geometries. Instead, it should be used to determine the degree to which a star-forming region is either spatially substructured or smooth and centrally concentrated.