Do Neutron Star Gravitational Waves Carry Superfluid Imprints?

@article{Comer2002DoNS,
  title={Do Neutron Star Gravitational Waves Carry Superfluid Imprints?},
  author={G L Comer},
  journal={Foundations of Physics},
  year={2002},
  volume={32},
  pages={1903-1942}
}
  • G. Comer
  • Published 29 July 2002
  • Physics
  • Foundations of Physics
Isolated neutron stars undergoing non-radial oscillations are expected to emit gravitational waves in the kilohertz frequency range. To date, radio astronomers have located about 1,300 pulsars, and can estimate that there are about 2×108 neutron stars in the galaxy. Many of these are surely old and cold enough that their interiors will contain matter in the superfluid or superconducting state. In fact, the so-called glitch phenomenon in pulsars (a sudden spin-up of the pulsar's crust) is best… 
Theoretical analysis of the vibrational dynamics of neutron star interiors
Just as the observations of oscillations of ordinary stars can be used to determine their composition and structure, the oscillations of neutron stars could potentially be used to determine the
Inertial modes of non-stratified superfluid neutron stars
We present results concerning adiabatic inertial-mode oscillations of non-stratified superfluid neutron stars in Newtonian gravity, using the anelastic and slow-rotation approximations. We consider a
Inertial modes of neutron stars with a superfluid core
We investigate the modal properties of inertial modes of rotating neutron stars with a core filled with neutron and proton superfluids, taking account of entrainment effects between the superfluids.
Relativistic tidal properties of superfluid neutron stars
We investigate the tidal deformability of a superfluid neutron star. We calculate the equilibrium structure in the general relativistic two-fluid formalism with entrainment effect where we take
Gravitational Radiation from Nonaxisymmetric Spherical Couette Flow in a Neutron Star
The gravitational-wave signal generated by global, nonaxisymmetric shear flows in a neutron star is calculated numerically by integrating the incompressible Navier-Stokes equation in a spherical,
r-modes in low temperature color-flavor-locked superconducting quark stars
We present the first multifluid analysis of a dense neutron star core with a deconfined color-flavor-locked superconducting quark component. Accounting only for the condensate and (finite
Lagrangian perturbation theory of non-relativistic rotating superfluid stars
We develop a Lagrangian perturbation framework for rotating non-relativistic superfluid neutron stars. This leads to the first generalization of classic work on the stability properties of rotating
Relativistic fluid dynamics: physics for many different scales
The relativistic fluid is a highly successful model used to describe the dynamics of many-particle systems moving at high velocities and/or in strong gravity. It takes as input physics from
Post inflationary evolution of inflation-produced large-scale magnetic fields using a generalised cosmological Ohm's law and both standard and modified Maxwell's equations
In most of the literature on evolution of cosmological magnetic fields, it is found that large-scale magnetic fields evolve as $B^{2}\propto a^{-4}$ (adiabatic magnetic decay) where $a$ is the
Oscillations of general relativistic multifluid/multilayer compact stars
We develop the formalism for determining the quasinormal modes of general relativistic multifluid compact stars in such a way that the impact of superfluid gap data can be assessed. Our results
...
...

References

SHOWING 1-10 OF 74 REFERENCES
Gravitational waves from hot young rapidly rotating neutron stars
Gravitational radiation drives an instability in the r-modes of young rapidly rotating neutron stars. This instability is expected to carry away most of the angular momentum of the star by
Gravitational Radiation Limit on the Spin of Young Neutron Stars
A newly discovered instability in rotating neutron stars, driven by gravitational radiation reaction acting on the stars' r-modes, is shown here to set an upper limit on the spin rate of young
On the dynamics of superfluid neutron star cores
We discuss the nature of the various modes of pulsation of superfluid neutron stars using comparatively simple Newtonian models and the Cowling approximation. The matter in these stars is described
Quaking Neutron Stars
Gravitational, magnetic, and superfluid forces can stress the crust of an evolving neutron star. Fracture of the crust under these stresses could affect the star's spin evolution and generate
Oscillations of general relativistic superfluid neutron stars
We develop a general formalism to treat, in general relativity, the nonradial oscillations of a superfluid neutron star about static (non-rotating) configurations. The matter content of these stars
r -modes in superfluid neutron stars
The analogues of r-modes in superfluid neutron stars are studied here. These modes, which are governed primarily by the Coriolis force, are identical to their ordinary-fluid counterparts at the
Towards gravitational wave asteroseismology
We present new results for pulsating neutron stars. We have calculated the eigenfrequencies of the modes that one would expect to be the most important gravitational wave sources: the fundamental
Quasinormal modes of general relativistic superfluid neutron stars
We develop a general formalism to treat, in general relativity, the linear oscillations of a two-fluid star about static (non-rotating) configurations. Such a formalism is intended for neutron stars,
Slowly rotating general relativistic superfluid neutron stars
We present a general formalism to treat slowly rotating general relativistic superfluid neutron stars. As a first approximation, their matter content can be described in terms of a two-fluid model,
A new class of g-modes in neutron stars
Because a neutron star is born hot, its internal composition is close to chemical equilibrium. In the fluid core, this implies that the ratio of the number densities of charged particles (protons
...
...