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The central density rho_0 of a stellar cluster is an important physicalparameter for determining its evolutionary and dynamical state. How much masssegregation there is, or whether the cluster has undergone core collapse bothdepends on rho_0. We reanalyze the results of a previous paper that gives themass density profile of R136 and combine them with both a conservative upperlimit for the core parameter and a more uncertain recent measurement. We thusplace a lower limit on rho_0 under reasonable and defensible assumptions aboutthe IMF, finding rho_0 >~ 1.5x10^4 Msun/pc^3 for the conservative assumption a< 0.4 pc for the cluster core parameter. If we use the lower, but moreuncertain value a = 0.025 pc, the central density estimate becomes greater than10^7 Msun/pc^3. A mechanism based on the destruction of a large number ofcircumstellar disks is posited to explain the hitherto unexplained increase inreddening presented in that same work.

The central density of R136 in 30 Doradus