Ka Ho Lo

TL;DR: In this article, the authors investigated a model of the accreting millisecond X-ray pulsars and showed that the magnetic poles of these stars are close to their spin axes, and the gas is channeled along different field lines to different locations on the stellar surface.

TL;DR: In this article, the authors used the energy-dependent waveforms of the X-ray flux oscillations seen during some thermonuclear bursts from some neutron stars to constrain the mass M and radius R of neutron stars.

TL;DR: In this article, the authors investigated a model of the accreting millisecond X-ray pulsars and showed that the magnetic poles of these stars are close to their spin axes, and the gas is channeled along different field lines to different locations on the stellar surface.

TL;DR: In this paper, the authors explore how well mass and radius of neutron stars can be determined by generating, and analyzing using Bayesian techniques, synthetic energy-resolved X-ray data that they produce assuming a future space mission having 2-30 keV energy coverage and an effective area of 10 m$^2.

TL;DR: In this paper, it was shown that moving the emitting area from very close to the spin axis to approximately 10 deg. away can increase the fractional rms amplitude from approx < 0.5% to a few percent, which is easily detectable.