We describe an experiment in which we induce a heat-driven superfluid flow in a straight tube and monitor the phase difference across the tube’s ends with a superfluid He quantum interference device (SHeQUID). We quantitatively verify the relation vs = (h̄/m)5φ. We also demonstrate the linearization of a SHeQUID using the heat injection method. Superfluid is described by a macroscopic wavefuncti...

On the basis of the neutrino emission from the isotropic S0 neutron superfluid vortexes in neutron star interiors, we propose a rocket model of neutrino jet for the observed pulsar kick.

Based on the Bogoliubov non-ideal gas model, we discuss the energy spectrum and phase transition of the superfluid Fermi gas of atoms with a weak attractive interaction on the canonical noncommutative space. Because the interaction of a BCS-type superfluid Fermi gas originates from a pair of Fermionic quasi-particles with opposite momenta and spins, the Hamiltonian of the Fermi gas on the nonco...

We have investigated the superfluid properties of a ring of weakly interacting and degenerate 1D Bose gas at thermal equilibrium with a rotating vessel. The conventional definition of superfluidity predicts that the gas has a significant superfluid fraction only in the Bose condensed regime. In the opposite regime, it is found that a superfluid behaviour can still be identified when the probabi...

Neutron stars are excellent emitters of gravitational waves. Squeezing matter beyond nuclear densities invites exotic physical processes, many of which violently transfer large amounts of mass at relativistic velocities, disrupting spacetime and generating copious quantities of gravitational radiation. I review mechanisms for generating gravitational waves with neutron stars. This includes grav...

The superfluid phases of helium-3 ((3)He) are predicted to be strongly influenced by mesoscopic confinement. However, mapping out the phase diagram in a confined geometry has been experimentally challenging. We confined a sample of (3)He within a nanofluidic cavity of precisely defined geometry, cooled it, and fingerprinted the order parameter using a sensitive nuclear magnetic resonance spectr...

The inner layers of a neutron star crust, composed of a Coulomb lattice of neutron rich nuclear clusters immersed in a sea of “free” superfluid neutrons, are closely analogous to periodic condensed matter systems such as electronic, photonic or phononic crystals. Applying methods from solid state physics to the neutron star context, we study the transport properties of those “free” neutrons for...

Superfluid vortex avalanches are one plausible cause of pulsar glitch activity. If they occur according to a state-dependent Poisson process, the measured long-term rate is determined by spin-down stellar crust, $\dot{\Omega}_{\rm c}$, and two phenomenological parameters quantifying vortex-nucleus pinning force: crust-superfluid angular velocity lag threshold, $X_{\rm cr}$, reference unpinning ...

The forced motion of superfluid vortices in shear oscillations of rotating solid neutron star matter produces damping of the mode. A simple model of the unpinning and repinning processes is described, with numerical calculations of the consequent energy decay times. These are of the order of 1 s for typical anomalous X-ray pulsars with rotational angular velocity Ω ≈ 1 rad s but become very sho...