Comparative Analysis of Two Formation Scenarios of Bursty Radio Emission from Ultracool Dwarfs

A.A. Kuznetsov, J.G. Doyle, S. Yu, G. Hallinan, A. Antonova, & A. Golden

Figure 1. Sketch of the emission source models: a) the model with the star-satellite interaction; b) the model with emission from a set of magnetic field lines (the rotational and magnetic equatorial planes are shown by dotted lines). The magnetic dipole axis is shown by bold arrows.


Recently, a number of ultracool dwarfs have been found to produce periodic radio bursts with high brightness temperature and polarization degree; the emission properties are similar to the auroral radio emissions of the magnetized planets of the Solar System. We simulate the dynamic spectra of radio emission from ultracool dwarfs. The emission is assumed to be generated due to the electron-cyclotron maser instability. We consider two source models: the emission caused by interaction with a satellite and the emission from a narrow sector of active longitudes; the stellar magnetic field is modeled by a tilted dipole. We have found that for the dwarf TVLM 513–46546, the model of the satellite-induced emission is inconsistent with the observations. On the other hand, the model of emission from an active sector is able to reproduce qualitatively the main features of the radio light curves of this dwarf; the magnetic dipole seems to be highly tilted (by about 60°) with respect to the rotation axis.

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Last Revised: 2011 December 1st