  We compute the high frequency quasi-normal modes (QNM) for scalar
perturbations of spherically symmetric single horizon black-holes in
$(D+2)$-space-time dimensions with generic curvature singularities and having
metrics of the form $ds^2 = \eta x^p (dy^2-dx^2) + x^q d\O_D^2$ near the
singularity $x=0$. The real part of the QN frequencies is shown to be
proportional to $\log \le[ 1 + 2\cos \le(\p \le[ qD -2 \ri]/2 \ri) \ri]$ where
the constant of proportionality is equal to the Hawking temperature for
non-degenerate black-holes and inverse of horizon radius for degenerate
black-holes. Apart from agreeing with the QN frequencies that have been
computed earlier, our results imply that the horizon area spectrum for the
general spherically symmetric black-holes is equispaced. Applying our results,
we also find the QNM frequencies for extremal Reissner-Nordstr\"om and various
stringy black-holes.
