  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.
