Star Formation in a Dynamic Interstellar Medium Workshop

Star Formation in a Dynamic Interstellar Medium Workshop hosted by the Yale University Astronomy Department May 20, 2002 Simulation is a preview of work by Bate, Bonnell & Bromm…stay tuned

The Plan Time Speaker Topic 09: 40 Alyssa Goodman (Cf. A/Yale) Introduction 10: 00 Phil Myers (Cf. A) What are the properties of the observed environment for star formation? 10: 40 Coffee Break 11: 00 Richard Larson What are the real observational constraints on the IMF? 11: 40 Paolo Padoan (Caltech/JPL) What have we learned from numerical simulations of the star-forming ISM, on >1 pc scales? 12: 20 Lunch 1: 50 Bruce Elmegreen (IBM) On what scale is an IMF determined, and how might the answer to this question change? (Opinion #1) 2: 30 Ian Bonnell (U. St. Andrews) On what scale is an IMF determined, and how might the answer to this question change? (Opinion #2; simulation figure above from Bate, Bonnell & Bromm) 3: 10 Coffee Break 3: 30 Richard Larson (Yale) 4: 00 Thoughts, and an open fourm, on the day's presentations Meeting Adjourns, but those interested stay on to chat

Questions Raised by a Dynamic View of Star Formation

“ 4. Powering source of (some) outflows may move rapidly through ISM. ” Goodman & Arce 2002

“Giant” Herbig-Haro Flow in PV Ceph 1 pc Reipurth, Bally & Devine 1997

PV Ceph: Episodic ejections from precessing or wobbling moving source Implied source motion ~7 km/s (3 mas/year) assuming jet velocity ~100 km/s Goodman & Arce 2002

“ 4. Powering source of (some) outflows may move rapidly through ISM. ” Goodman & Arce 2002

HST WFPC 2 Overlay: Padgett et al. 2002 Goodman & Arce 2002 Arce & Goodman 2002

Trail & Jet Goodman & Arce 2002

How much gas will be pulled along for the ride? Goodman & Arce 2002

Insights from a “Plasmon” Model Initial jet 250 km s-1; star motion 10 km s-1

Insights from a “Plasmon” Model