The Galactic center hosts a cluster with a characteristic velocity dispersion of ~$55$ km$/$s within the inner ~$10$ pc$.$ For a star at r$=4$ pc$,$ how does this velocity compare with the circular velocity of an object around the central SMBH$?$ A useful scaling relationship is that the gravitational radius corresponding to a solar mass is $($GM$\_$Sun $\backslash /$c$^2)=1\mathrm{.}495$ km$.$ What does this imply for the majority of the kinetic energy of these stars?