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 can not 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 _ { sd } \sim 3 \times 10 ^ { 35 } erg s ^ { -1 } and a wind Lorentz factor of \gamma _ { w } \sim 10 ^ { 4 } a quasi-steady synchrotron emission is established with luminosities in the 1 - 10 GHz range comparable to the observed one .