@article {21740,
	title = {Radio emission from Sgr A*: pulsar transits through the accretion disc},
	volume = {468},
	year = {2017},
	month = {2017/06/1},
	pages = {L26 - L30},
	abstract = {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{\textquoteright}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{\textquoteright}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<SUB>sd</SUB> \~{} 3 {\texttimes} 10<SUP>35</SUP> erg s<SUP>-1</SUP> and a wind Lorentz factor of γ<SUB>w</SUB> \~{} 10<SUP>4</SUP> a quasi-steady synchrotron emission is established with luminosities in the 1-10 GHz range comparable to the observed one.},
	keywords = {Astrophysics - High Energy Astrophysical Phenomena, Galaxy: centre, pulsars: general, radiation mechanisms: non-thermal, radio continuum: galaxies},
	isbn = {0035-8711},
	url = {https://ui.adsabs.harvard.edu/abs/2017MNRAS.468L..26C},
	author = {Christie, I. M. and Petropoulou, M. and Mimica, P. and Giannios, D.}
}
