Retrograde Accretion Disks in High-Mass Be/X-ray Binaries
Abstract
We have compiled a comprehensive library of all X-ray observations of Magellanic pulsars carried out by {\it XMM-Newton}, {\it Chandra}, and {\it RXTE} in the period 1997-2014. In this work, we use the data from 53 high-mass Be/X-ray binaries in the Small Magellanic Cloud to demonstrate that the distribution of spin-period derivatives vs. spin periods of spinning-down pulsars is not at all different than that of the accreting spinning-up pulsars. The inescapable conclusion is that the up and down samples were drawn from the same continuous parent population, therefore Be/X-ray pulsars that are spinning down over periods spanning 18 years are in fact accreting from retrograde disks. The presence of prograde and retrograde disks in roughly equal numbers supports a new evolutionary scenario for Be/X-ray pulsars in their spin period-period derivative diagram.
Keywords
Cite
@article{arxiv.1704.06364,
title = {Retrograde Accretion Disks in High-Mass Be/X-ray Binaries},
author = {D. M. Christodoulou and S. G. T. Laycock and D. Kazanas},
journal= {arXiv preprint arXiv:1704.06364},
year = {2017}
}
Comments
To appear in MNRAS Letters