An understanding of the process of star formation is an essential requirement of theories of galaxy formation and evolution, and gives direct insights into the formation of our own Sun and the number of extra-solar planets we expect to find in the Galaxy. We use telescopes operating at millimetre and sub-mm wavelengths to observe the cool molecular clouds which are collapsing to form stars and help understand the basic physics of star formation. In particular, we study the supersonic jets ejected during the star formation process, and the accretion disks surrounding the protostars which allow the stars to grow in mass and in which planets are believed to form.

Multi-wavelength studies are used to determine the pattern of star formation in the recent past in a variety of galaxy types and relate this to the observed structure and dynamics in the cold ISM. Of particularly interest is the study of low-metallicity and interacting systems in the local universe which may be typical of systems found at high redshift. We have developed an N-body code in which the star formation process can be modelled on galactic scales enabling various physical processes such as self-regulatory and self-propagating mechanisms of star formation to be investigated theoretically. An important problem is how the star formation rate is regulated (or not) and the complex interactions between galactic dynamics, the interstellar medium and star formation processes.

Last Modified 13 October 1998
Please send comments to John Richer.