  In this article we present results from three on-going projects related to
the formation of protoplanets in protostellar discs. We present the results of
simulations that model the interaction between embedded protoplanets and disc
models undergoing MHD turbulence. We review the similarities and differences
that arise when the disc is turbulent as opposed to laminar (but viscous), and
present the first results of simulations that examine the tidal interaction
between low mass protoplanets and turbulent discs. We describe the results of
simulations of Jovian mass protoplanets forming in circumbinary discs, and
discuss the range of possible outcomes that arise in hydrodynamic simulations.
Finally, we report on some preliminary simulations of three protoplanets of
Jovian mass that form approximately coevally within a protostellar disc. We
describe the conditions under which such a system can form a stable three
planet resonance.
