  There has been recent speculation (Davies & King 2005) that the cores of
intermediate-mass stars stripped of their envelopes by tidal interaction with
the supermassive black hole in the Galactic centre could form a population
observationally similar to the so-called Sgr A* cluster or `S' stars, which
have close eccentric orbits around the hole. We model the evolution of such
stars, and show that the more luminous end of the population may indeed appear
similar to young B stars within the observational limits of the Galactic Centre
region. Whether some or all of these cluster stars can be accounted for in this
manner depends strongly on the assumed IMF of the loss cone stars and the
scattering rate. If most of the observed stars are in fact scattered from the
Galactic Centre inner cusp region itself then the population of ~20 to current
observational limits may be reproduced. However, this only works if the local
relaxation time is small and relies on the cusp stars themselves being young,
i.e. it is dependent on some star formation being possible in the central few
parsecs. Conversely, we obtain a possible constraint on the tidal stripping
rate of `normal'-IMF stars if there are not to be red stars visible in the Sgr
A* cluster.
