<?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%">Petropoulou, M.</style></author><author><style face="normal" font="default" size="100%">Vasilopoulos, G.</style></author><author><style face="normal" font="default" size="100%">Christie, I. M.</style></author><author><style face="normal" font="default" size="100%">Giannios, D.</style></author><author><style face="normal" font="default" size="100%">Coe, M. J.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">X-ray mapping of the stellar wind in the binary PSR J2032+4127/MT91 213</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%">Astrophysics - High Energy Astrophysical Phenomena</style></keyword><keyword><style  face="normal" font="default" size="100%">pulsars: individual: PSR J2032+4127</style></keyword><keyword><style  face="normal" font="default" size="100%">radiation mechanisms: non-thermal</style></keyword><keyword><style  face="normal" font="default" size="100%">stars: massive</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%">2018</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2018/02/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2018MNRAS.474L..22P</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">OUP</style></publisher><volume><style face="normal" font="default" size="100%">474</style></volume><pages><style face="normal" font="default" size="100%">L22 - L26</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%">PSR J2032+4127 is a young and rapidly rotating pulsar on a highly eccentric orbit around the high-mass Be star MT91 213. X-ray monitoring of the binary system over an ∼4000 d period with Swift has revealed an increase of the X-ray luminosity which we attribute to the synchrotron emission of the shocked pulsar wind. We use Swift X-ray observations to infer a clumpy stellar wind with r&lt;SUP&gt;-2&lt;/SUP&gt; density profile and constrain the Lorentz factor of the pulsar wind to 10&lt;SUP&gt;5&lt;/SUP&gt; &lt; γ&lt;SUB&gt;w&lt;/SUB&gt; &lt; 10&lt;SUP&gt;6&lt;/SUP&gt;. We investigate the effects of an axisymmetric stellar wind with polar gradient on the X-ray emission. Comparison of the X-ray light curve hundreds of days before and after the periastron can be used to explore the polar structure of the wind.</style></abstract></record></records></xml>