Robert T. Chamberlain

TL;DR: In this paper, a simple model, based on spherical collapse, was presented to accurately predict the location of the splashback without any free parameters, which is produced by splashback material on its first apocentric passage after accretion.

TL;DR: In this paper, a simple model, based on spherical collapse, was presented to accurately predict the location of the splashback without any free parameters, which is produced by splashback material on its first apocentric passage after accretion.

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 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, 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.