  Theory and observations suggest that star formation occurs hierarchically due
to the fragmentation of giant molecular clouds. In this case we would expect
substructure and enhanced stellar multiplicity in the primordial cluster. This
substructure is expected to decay quickly in most environments, however
historic stellar encounters might leave imprints in a protoplanetary disc (PPD)
population. In a low density environment such as Taurus, tidal tails from
violent star-disc or disc-disc encounters might be preserved over time-scales
sufficient to be observed. In this work, we investigate the possibility that
just such an event occured between HV Tau C (itself a component of a triple
system) and DO Tau $\sim 0.1$ Myr ago, as evidenced by an apparent `bridge'
structure evident in the $160$ $\mu$m emission. By modelling the encounter
using smoothed particle hydrodynamics (SPH) we reproduce the main features of
the observed extended structure (`V'-shaped emission pointing west of HV Tau
and a tail-like structure extending east of DO Tau). We suggest that HV Tau and
DO Tau formed together in a quadruple system on a scale of $\sim 5000$ au
($0.025$ pc).
