  The dynamics of stars in the inner regions of nearby globular clusters (GCs)
such as G1 indicate the presence of central concentrated dark masses, and one
would like to know whether these are indeed intermediate mass black holes
(IMBHs). As the number of surrounding stars, and their motions, are roughly
known, the capture rate can be estimated; the question then arises of whether
the apparent quiescence of the nuclei of these GCs is compatible with the
IMBH's presence. The role of debris from disrupted stars in activating
quiescent nuclei of GCs is studied here employing three-dimensional
hydrodynamics simulations. It is argued that when individual stars are
disrupted, the bulk of the debris would be swallowed or expelled rapidly
compared with the interval between successive disruptions. Only a small
fraction of the tightly bound mass is likely to be swallowed, yielding
radiation with high efficiency, the surplus being expelled in a
radiation-driven wind. A transient (predominantly of soft X-ray emission)
signal could persist steadily with L ~ L_Edd =10^{41}(M_h/10^3M_sun) erg/s for
at most tens of years; thereafter the flare would rapidly fade. While the
infall rate declines as t^{-5/3}, some material may be stored for a longer time
in an accretion disk. The IMBH luminosity could then remain as high as L_X >
10^{39} erg/s for several hundreds of years after disruption. In a given
object, this ultraluminous X-ray activity would have a duty cycle of order
10^{-4}. Quiescent GCs, those with IMBHs now starved of fuel, should greatly
outnumber active ones; observational constraints would not then be stringent
until we had observed enough candidates to constitute a proper ensemble
average.(abridged)
