  We explore full/partial tidal disruption events (TDEs) of stars/planets by
stellar compact objects (Black holes; BHs; or neutron stars; NSs), which we
term micro-TDEs. Disruption of a star/planet with mass $M_{\star}$ may lead to
the formation of a debris disk around the BH/NS. Efficient accretion of a
fraction $(f_{acc}=0.1$ of the debris may then give rise to bright energetic
long ($10^{3}-10^{4}\,s$), X-ray/Gamma-ray flares, with total energies of up to
$(f_{acc}/0.1)\times10^{52}\,(M_{\star}/{0.6\,M_{\odot}})\,$ergs, possibly
resembling ultra-long GRBs/XRFs. The energy of such flares depends on the
poorly constrained accretion processes. Significantly fainter flares might be
produced if most of the disk mass is blown away through strong outflows. We
suggest three dynamical origins for such disruptions. In the first, a
star/planet is tidally disrupted following a close random encounter with a
BH/NS in a dense cluster. We estimate the BH (NS) micro-TDE rates from this
scenario to be few$\times10^{-6}$ (few$\times10^{-7}$) ${\rm yr}^{-1}$ per
Milky-Way galaxy. Another scenario involves the interaction of wide companions
due to perturbations by stars in the field, likely producing comparable but
lower rates. Finally, a third scenario involves a BH/NS which gain a natal
velocity kick at birth, leading to a close encounter with a binary companion
and the tidal disruption of that companion. Such events could be associated
with a supernova, or even with a preceding GRB/XRF event, and would likely
occur hours to days after the prompt explosion; the rates of such events could
be larger than those obtained from the other scenarios, depending on the
preceding complex binary stellar evolution.
