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Project RISARD

Red Dwarfs (RDs) are the most common, low-mass stars (<=0.5 M_sun) in the Solar neighbourhood, and probably in the Universe as well. Most (likely all) young RDs are magnetically active, and therefore it is impossible to measure their radial velocities (RVs) with the accuracy required by contemporary planetary searches (5-50 m/s). Some of RDs are known as a source of variable radio emission at centimetre wavelengths. This radiation is relatively weak (~0.2 to 1 mJy). However, recent development of the EVN and e-VLBI systems in terms of sensitivity gives a new possibility to investigate such stars. Here, we present first results from our ongoing RISARD project (Radio Interferometric Survey of Active Red Dwarfs). The main goal of this project is to detect an exoplanet by direct, precise measurements of a RD position and possible changes to this position caused by the planet.