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The dynamics of stellar streams in rotating barred potentials is explainedfor the first time. Naturally, neighbouring stream stars reach pericentre atslightly different times. In the presence of a rotating bar, these neighbouringstream stars experience different bar orientations during pericentric passageand hence each star receives a different torque from the bar. These differingtorques reshape the angular momentum and energy distribution of stars in thestream, which in turn changes the growth rate of the stream. For a progenitororbiting in the same sense as the bar's rotation and satisfying a resonancecondition, the resultant stream can be substantially shorter or longer thanexpected, depending on whether the pericentric passages of the progenitor occuralong the bar's minor or major axis respectively. We present a full discussionof this phenomenon focusing mainly on streams confined to the Galactic plane.In stark contrast with the evolution in static potentials, which give rise tostreams that grow steadily in time, rotating barred potentials can producedynamically old, short streams. This challenges the traditional viewpoint thatthe inner halo consists of well phase-mixed material whilst thetidally-disrupted structures in the outer halo are more spatially coherent. Weargue that this mechanism plays an important role in explaining themysteriously short Ophiuchus stream that was recently discovered near the bulgeregion of the Milky Way.

Shepherding Tidal Debris with the Galactic Bar: The Ophiuchus Stream