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A number of recent observational studies of Galactic globular clusters havemeasured the variation in the slope of a cluster's stellar mass function$\alpha$ with clustercentric distance $r$. In order to gather a deeperunderstanding of the information contained in such observations, we haveexplored the evolution of $\alpha(r)$ for star clusters with a variety ofinitial conditions using a large suite of $N$-body simulations. We havespecifically studied how the time evolution of $\alpha(r)$ is affected byinitial size, mass, binary fraction, primordial mass segregation, black holeretention, an external tidal field, and the initial mass function itself.Previous studies have shown that the evolution of $\alpha_G$ is closely relatedto the amount of mass loss suffered by a cluster. Hence for each simulation wehave also followed the evolution of the slope of the cluster's global stellarmass function, $\alpha_G$, and have shown that clusters follow a well-definedtrack in the $\alpha_G$-$d\alpha(r)/d(ln(r/r_m))$ plane. The location of acluster on the $\alpha_G-d\alpha(r)/d(ln(r/r_m))$ plane can therefore constrainits dynamical history and, in particular, constrain possible variations in thestellar initial mass function. The $\alpha_G$-$d\alpha(r)/d(ln(r/r_m))$ planethus serves as a key tool for fully exploiting the information contained inwide field studies of cluster stellar mass functions.

Radial Variation in the Stellar Mass Functions of Star Clusters