Isolated Star Formation: From Cloud Formation to Core Collapse
Derek Ward-Thompson
The formation of stars is one of the most fundamental
problems in astrophysics, as it underlies many other questions, on
scales from the formation of galaxies to the formation of the solar
system. The physical processes involve the turbulent behavior of a
partially ionized medium containing a non-uniform magnetic field.
Current debate centers around the time taken for turbulence to decay
and the relative importance of the roles played by magnetic fields and
turbulence. Technological advances such as millimeter-wave cameras have
made possible observations of the temperature and density profiles, and
statistical calculations of the lifetimes, of objects collapsing under
their own self-gravity and those on the verge of collapse. Increased
computing power allows more complex models to be made that include
magnetic and turbulent effects. No current model can reproduce all of
the observations.
Department of Physics and Astronomy, Cardiff University, Post
Office Box 913, Cardiff, UK. E-mail: D.Ward-Thompson{at}astro.cf.ac.uk
