The research is mostly concentrated on studies of the dynamics of binary star formation, Beta Pictoris-type planetary systems, and planet formation in discs.
A pre-main sequence binary star system may contain two circumstellar discs and a circumbinary disc. Disc structure and evolution are modified by the binary, and vice versa, due to resonant emission of waves. Disc gap size and shape, as well as the characteristic features at its edge are indicative of binary star parameters. Artymowicz and Lubow have overturned a decade-long conviction that gas cannot accrete from circumbinary discs onto the binary stars or their discs, and thus resupply them. Their theory of mass flow through gaps received strong support from the photometry and spectroscopy of PMS binaries, imaging, and other observations.
Within the past decade, astronomers have found direct evidence of extrasolar planetary systems, and we contributed to several theories addressing their surprising diversity. We challenged two recent theories connecting the nature of Vega/Beta Pictoris-type systems (planetesimal/dust discs surrounding at least 15 percent of normal stars) with the ISM dust bombardment, showing instead that dusty discs evolve from high to low dustiness stage as a result of internal dust erosion and the so-called dust avalanches.
High-resolution hydrodynamical simulations of disc-planet interaction (cf.
http://www.astro.su.se/ 
pawel) were produced. They showed that mass
can flow through a gap created in the disc by the protoplanet. This opens
a possibility that super-Jovian mass planets recently found may have formed
in discs (and need not be brown dwarfs). Moreover, disc-planet interaction
will also produce the observed high eccentricities of orbits of the
superplanets.