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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 byExpand
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Gravitational Radiation Instability in Hot Young Neutron Stars
We show that gravitational radiation drives an instability in hot young rapidly rotating neutron stars. This instability occurs primarily in the l=2 r-mode and will carry away most of the angularExpand
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The effect of viscosity on neutron star oscillations
The rate at which neutron star oscillations are damped by the presence of viscosity and thermal conductivity in the neutron matter is computed. Fully relativistic equations are used to describe theExpand
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A New Generalized Harmonic Evolution System
A new representation of the Einstein evolution equations is presented that is first order, linearly degenerate and symmetric hyperbolic. This new system uses the generalized harmonic method toExpand
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Stability and causality in dissipative relativistic fluids
The standard theory of relativistic dissipative fluid mechanics developed by Eckart contains several undesirable features: thermal and viscous fluctuations propagate acausally; there exist genericExpand
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Second-order rotational effects on the r-modes of neutron stars.
Techniques are developed here for evaluating the r-modes of rotating neutron stars through second order in the angular velocity of the star. Second-order corrections to the frequencies andExpand
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Effect of hyperon bulk viscosity on neutron-star r-modes
Neutron stars are expected to contain a significant number of hyperons in addition to protons and neutrons in the highest density portions of their cores. Following the work of Jones, we calculateExpand
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Determining the nuclear equation of state from neutron-star masses and radii
A method is developed for determining the nuclear equation of state directly from a knowledge of the masses and radii of neutron stars. This analysis assumes only that equilibrium neutron-star matterExpand
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Spectral representations of neutron-star equations of state
Methods are developed for constructing spectral representations of cold (barotropic) neutron-star equations of state. These representations are faithful in the sense that every physical equation ofExpand
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