Gas flows from interacting galaxies are postulated to represent an
important source of future star formation fuel. However, how exactly gas
ends up back into galaxies is still not understood.
The closeby Magellanic Stream offers a unique window into understanding
the role and fate of interacting tails of gas and details of
their structure, dynamics and evolution.
I will present highlights from recent observational studies
which show that the Stream is significantly more extended than
previously thought, and contains a significant abundance of
small-scale structure.
By undertaking a systematic study of neutral hydrogen morphology
and kinematics, we can investigate the aging of the Stream gas
through various hydrodynamical instabilities, as well as
its interaction with the Galactic halo.
By working backward, starting from the northern extension of the Stream
which has been exposed the longest to the hot Galactic halo,
we can provide important constraints for the orbital evolution of the
Magellanic Clouds, the topic still under heated debate.