  The last decade has seen the detection of fast moving stars in the Galactic
halo, the so-called hypervelocity stars (HVSs). While the bulk of this
population is likely the result of a close encounter between a stellar binary
and the supermassive black hole (MBH) in the Galactic Centre (GC), other
mechanims may contribute fast stars to the sample. Few observed HVSs show
apparent ages which are shorter than the flight time from the GC, thereby
making the binary disruption scenario unlikely. These stars may be the result
of the breakup of a stellar triple in the GC which led to the ejection of a
hypervelocity binary (HVB). If such binary evolves into a blue straggler star
due to internal processes after ejection, a rejuvenation is possible that make
the star appear younger once detected in the halo. A triple disruption may also
be responsible for the presence of HVBs, of which one candidate has now been
observed. We present a numerical study of triple disruptions by the MBH in the
GC and find that the most likely outcomes are the production of single HVSs and
single/binary stars bound to the MBH, while the production of HVBs has a
probability $\lesssim 1\%$ regardless of the initial parameters. Assuming a
triple fraction of $\approx 10\%$ results in an ejection rate of $\lesssim 1\
\mathrm{Gyr}^{-1}$, insufficient to explain the sample of HVSs with lifetimes
shorter than their flight time. We conclude that alternative mechanisms are
responsible for the origin of such objects and HVBs in general.
