Radio Emission from Masuda Sources

We note that different models, providing comparably good interpretation of the hard X-ray properties of so-called Masuda sources, can make distinctly different predictions for the radio emission produced at the Masuda source by the same population of accelerated electrons. Accordingly, we calculate the radio emission within a few competing models, i. e., those involving magnetic, turbulent, and collisional trapping of the fast electrons in the coronal source. We show that even available incomplete radio observations of the classical Masuda event and a Masuda-like event on 31 December 2007, recently reported by Krucker et al. (Astrophys. J. 714, 1108, 2010) are highly valuable in restricting the physical model of the source. Furthermore, our study proposes that combination of more complete high-resolution X-ray and radio observations can allow unambiguous distinction between the competing Masuda source models.