0 Assigned ID: 938 ----- Attempting Submission 1 (Fri Apr 11 22:12:58 GMT 2014) ----- Triggered star formation (TSF) occurs when supersonic flows generated by distant supernova blast waves, stellar winds (wind blown bubbles) or ionization fronts (D-type fronts in HII regions) sweep over a stable cloud. TSF may play a role in massive regions of star formation where winds, HII regions and, eventually, blast-waves sweep through dense, heterogeneous molecular material. In addition TSF has played an important role in discussions of the formation of our own solar system because it offers a natural way of injecting short lived radioactive isotopes (SLRI's) like 26^Al into material which will then form planetary bodies. The purpose of this proposal is to use advanced numerical tools to explore the physics of TSF in greater detail than has been attempted before. Previous studies have not been able to follow triggering past the early stages before a star forms. Our 3-D Adaptive Mesh Refinement (AMR) MHD code contains well tested physics modules which will allow us to track the influence of self-gravity, radiation-transport, cooling by molecules/neutrals/atoms and, finally, the collapse of gas into stars (i.e.condensed gravitating point-like objects or "sink-particles"). With this tool we will follow triggering well past the formation of the star to explore the creation of accretion disks and their properties. In addition the microphysics routines in the code allow us to make detailed contact with HST observations such as the pillars in the Carina nebula via synthetic observations of line profiles, proper motions, Position-Velocity diagrams and statistics. RESOLVED STAR FORMATION Default Medium false false false false true SUPPORTED