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Mature neutron stars are expected to have several superfluid components.Strong evidence for this is provided by the glitches that have been observed indozens of pulsars. The underlying idea behind most glitch models is that, asthe neutron star crust spins down due to the emission of electromagneticradiation, the superfluid component lags behind until a critical point isreached and angular momentum is transferred from the superfluid to the crust,leading to the spin-up associated with the glitch. In this Letter we describe asuperfluid analogue of the two-stream instability that is well known in plasmaphysics, and provide evidence that this instability is likely to be relevantfor neutron stars. This is a new physical mechanism which may play a key rolein explaining the glitch mechanism and which could also prove to be relevant inlaboratory experiments on superfluid Helium.Comment: 5 pages, 1 figure; uses RevTeX4; submitte

Are Pulsar Glitches Triggered by a Superfluid Two-Stream Instability?