  We present a new analytical solution to the steady-state distribution of
stars close to a central supermassive black hole of mass $M_{\bullet}$ in the
center of a galaxy. Assuming a continuous mass function of the form $dN/dm
\propto m^{\gamma}$, stars with a specific orbital energy $x = GM_{\bullet}/r -
v^2/2$ are scattered primarily by stars of mass $m_{\rm d}(x) \propto
x^{-5/(4\gamma+10)}$ that dominate the scattering of both lighter and heavier
species at that energy. Stars of mass $m_{\rm d}(x)$ are exponentially rare at
energies lower than $x$, and follow a density profile $n(x') \propto x'^{3/2}$
at energies $x' \gg x$. Our solution predicts a negligible flow of stars
through energy space for all mass species, similarly to the conclusions of
Bahcall & Wolf (1977), but in contrast to the assumptions of Alexander & Hopman
(2009). This is the first analytic solution which smoothly transitions between
regimes where different stellar masses dominate the scattering.
