<?xml version="1.0" encoding="UTF-8"?><xml><records><record><source-app name="Biblio" version="7.x">Drupal-Biblio</source-app><ref-type>17</ref-type><contributors><authors><author><style face="normal" font="default" size="100%">Karaferias, A. S.</style></author><author><style face="normal" font="default" size="100%">Vasilopoulos, G.</style></author><author><style face="normal" font="default" size="100%">Petropoulou, M.</style></author><author><style face="normal" font="default" size="100%">Jenke, P. A.</style></author><author><style face="normal" font="default" size="100%">Wilson-Hodge, C. A.</style></author><author><style face="normal" font="default" size="100%">Malacaria, C.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">A Bayesian approach for torque modelling of BeXRB pulsars with application to super-Eddington accretors</style></title><short-title><style face="normal" font="default" size="100%">Monthly Notices of the Royal Astronomical Society</style></short-title></titles><keywords><keyword><style  face="normal" font="default" size="100%">Accretion</style></keyword><keyword><style  face="normal" font="default" size="100%">accretion discs</style></keyword><keyword><style  face="normal" font="default" size="100%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">pulsars: individual: RX J0520.5-6932</style></keyword><keyword><style  face="normal" font="default" size="100%">RX J0209-7427</style></keyword><keyword><style  face="normal" font="default" size="100%">Swift J0243.6+6124</style></keyword><keyword><style  face="normal" font="default" size="100%">X-rays: binaries</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2023</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2023/03/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2023MNRAS.520..281K</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">OUP</style></publisher><volume><style face="normal" font="default" size="100%">520</style></volume><pages><style face="normal" font="default" size="100%">281 - 299</style></pages><isbn><style face="normal" font="default" size="100%">0035-8711</style></isbn><language><style face="normal" font="default" size="100%">eng</style></language><abstract><style face="normal" font="default" size="100%">In this study, we present a method to estimate posterior distributions for standard accretion torque model parameters and binary orbital parameters for X-ray binaries using a nested sampling algorithm for Bayesian parameter estimation. We study the spin evolution of two Be X-ray binary systems in the Magellanic Clouds, RX J0520.5-6932 and RX J0209-7427, during major outbursts, in which they surpassed the Eddington limit. Moreover, we apply our method to the recently discovered Swift J0243.6+6124, the only known Galactic pulsating ultra-luminous X-ray source. This is an excellent candidate for studying the disc evolution at super-Eddington accretion rates, because its luminosity spans several orders of magnitude during its outburst, with a maximum L&lt;SUB&gt;X&lt;/SUB&gt; that exceeded the Eddington limit by a factor of ~10. Our method, when applied to RX J0520.5-6932 and RX J0209-7427, is able to identify the more favourable torque model for each system, while yielding meaningful ranges for the NS and orbital parameters. Our analysis for Swift J0243.6+6124 illustrates that, contrary to the standard torque model predictions, the magnetospheric radius (R&lt;SUB&gt;m&lt;/SUB&gt;) and the Alfvén radius (R&lt;SUB&gt;A&lt;/SUB&gt;) are not proportional to each other when surpassing the Eddington limit. Reported distance estimates of this source range between 5 and 7 kpc. Smaller distances require non-typical neutron star properties (i.e. mass and radius) and possibly lower radiative efficiency of the accretion column.</style></abstract></record></records></xml>