<?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%">Christie, I. M.</style></author><author><style face="normal" font="default" size="100%">Petropoulou, M.</style></author><author><style face="normal" font="default" size="100%">Mimica, P.</style></author><author><style face="normal" font="default" size="100%">Giannios, D.</style></author></authors></contributors><titles><title><style face="normal" font="default" size="100%">Radio emission from Sgr A*: pulsar transits through the accretion disc</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%">Galaxy: centre</style></keyword><keyword><style  face="normal" font="default" size="100%">pulsars: general</style></keyword><keyword><style  face="normal" font="default" size="100%">radiation mechanisms: non-thermal</style></keyword><keyword><style  face="normal" font="default" size="100%">radio continuum: galaxies</style></keyword></keywords><dates><year><style  face="normal" font="default" size="100%">2017</style></year><pub-dates><date><style  face="normal" font="default" size="100%">2017/06/1</style></date></pub-dates></dates><urls><web-urls><url><style face="normal" font="default" size="100%">https://ui.adsabs.harvard.edu/abs/2017MNRAS.468L..26C</style></url></web-urls></urls><publisher><style face="normal" font="default" size="100%">OUP</style></publisher><volume><style face="normal" font="default" size="100%">468</style></volume><pages><style face="normal" font="default" size="100%">L26 - L30</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%">Radiatively inefficient accretion flow models have been shown to accurately account for the spectrum and luminosity observed from Sgr A* in the X-ray regime down to mm wavelengths. However, observations at a few GHz cannot be explained by thermal electrons alone but require the presence of an additional non-thermal particle population. Here, we propose a model for the origin of such a population in the accretion flow via means of a pulsar orbiting the supermassive black hole in our Galaxy. Interactions between the relativistic pulsar wind with the disc lead to the formation of a bow shock in the wind. During the pulsar's transit through the accretion disc, relativistic pairs, accelerated at the shock front, are injected into the disc. The radio-emitting particles are long lived and remain within the disc long after the pulsar's transit. Periodic pulsar transits through the disc result in regular injection episodes of non-thermal particles. We show that for a pulsar with spin-down luminosity L&lt;SUB&gt;sd&lt;/SUB&gt; ∼ 3 × 10&lt;SUP&gt;35&lt;/SUP&gt; erg s&lt;SUP&gt;-1&lt;/SUP&gt; and a wind Lorentz factor of γ&lt;SUB&gt;w&lt;/SUB&gt; ∼ 10&lt;SUP&gt;4&lt;/SUP&gt; a quasi-steady synchrotron emission is established with luminosities in the 1-10 GHz range comparable to the observed one.</style></abstract></record></records></xml>