• Publications
  • Influence
Matter in strong magnetic fields
  • D. Lai
  • Physics
  • 20 September 2000
The properties of matter are drastically modified by strong magnetic fields, $B\ensuremath{\gg}{m}_{e}^{2}{e}^{3}c/{\ensuremath{\Elzxh}}^{3}=2.35\ifmmode\times\else\texttimes\fi{}{10}^{9}\mathrm{G}$Expand
Physics of strongly magnetized neutron stars
There has recently been growing evidence for the existence of neutron stars possessing magnetic fields with strengths that exceed the quantum critical field strength of 4.4 × 1013 G, at which theExpand
Gravitational radiation from rapidly rotating nascent neutron stars
We study the secular evolution and gravitational wave signature of a newly formed, rapidly rotating neutron star. The neutron star may arise from core collapse in a massive star or from theExpand
Tidal dissipation in planet-hosting stars: damping of spin-orbit misalignment and survival of hot Jupiters
  • D. Lai
  • Physics
  • 22 September 2011
Observations of hot Jupiters around solar-type stars with very short orbital periods (∼1 d) suggest that tidal dissipation in such stars is not too efficient so that these planets can survive againstExpand
It is shown that the cylinder-shaped accretion stream can have an area comparable to that of the planet and a significant optical depth to spectral line absorption, and may produce an earlier ingress of thePlanet transit, as suggested by recent Hubble Space Telescope observations of the WASP-12 system. Expand
Condensed surfaces of magnetic neutron stars, thermal surface emission, and particle acceleration above pulsar polar caps
Recent calculations indicate that the cohesive energy of condensed matter increases with magnetic field strength and becomes very significant at magnetar-like fields (e.g. 10 keV at 3 × 10 14 G forExpand
Resonant Oscillations and Tidal Heating in Coalescing Binary Neutron Stars
Tidal interaction in a coalescing neutron star binary can resonantly excite the g-mode oscillations of the neutron star when the frequency of the tidal driving force equals the intrinsic g-modeExpand
Ellipsoidal figures of equilibrium: Compressible models
The results of Chandrasekhar (1969) are generalized to polytropes, using a formalism based on ellipsoidal energy variational principle to construct approximate stellar equilibrium solutions and studyExpand
Global Nonradial Instabilities of Dynamically Collapsing Gas Spheres
Self-similar solutions provide good descriptions for the gravitational collapse of spherical clouds or stars when the gas obeys a polytropic equation of state, p = Kργ (with γ ≤ 4/3, and γ = 1Expand
Cold equation of state in a strong magnetic field - Effects of inverse beta-decay
The influence of a high magnetic field (B is greater than 10 exp 12 G) on the degenerate matter equation of state appropriate to a neutron star is studied. The regime dominated by relativisticExpand