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In this paper we simulate the cyclic circularly-polarised pulses of theultra-cool dwarf TVLM513-46546, observed with the VLA at 4.88 and 8.44 GHz onMay 2006, by using a 3D model of the auroral radio emission from the stellarmagnetosphere. During this epoch, the radio light curves are characterised bytwo pulses left-hand polarised at 4.88 GHz, and one doubly-peaked (of oppositepolarisations) pulse at 8.44 GHz. To take into account the possible deviationfrom the dipolar symmetry of the stellar magnetic field topology, the modeldescribed in this paper is also able to simulate the auroral radio emissionfrom a magnetosphere shaped like an offset-dipole. To reproduce the timing andpattern of the observed pulses, we explored the space of parameters controllingthe auroral beaming pattern and the geometry of the magnetosphere. Through theanalysis of the TVLM513-46546 auroral radio emission, we derive someindications on the magnetospheric field topology that is able to simultaneouslyreproduce the timing and patterns of the auroral pulses measured at 4.88 and8.44 GHz. Each set of model solutions simulates two auroral pulses (singly ordoubly peaked) per period. To explain the presence of only one 8.44 GHz pulseper period, we analyse the case of auroral radio emission limited only to amagnetospheric sector activated by an external body, like the case of theinteraction of Jupiter with its moons.

Probing the magnetosphere of the M8.5 dwarf TVLM513-46546 by modelling its auroral radio emission. Hint of star exoplanet interaction?