Star Formation in a Dynamic Interstellar Medium Workshop hosted by the Yale University Astronomy Department May 20, 2002 Simulation is a preview of work.

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Presentation transcript:

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 TimeSpeakerTopic 09:40Alyssa Goodman (CfA/Yale)Introduction 10:00Phil Myers (CfA)What are the properties of the observed environment for star formation? 10:40Coffee Break 11:00Richard LarsonWhat are the real observational constraints on the IMF? 11:40Paolo Padoan (Caltech/JPL)What have we learned from numerical simulations of the star-forming ISM, on >1 pc scales? 12:20Lunch 1:50Bruce Elmegreen (IBM)On what scale is an IMF determined, and how might the answer to this question change? (Opinion #1) 2:30Ian 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) 3:10Coffee Break 3:30Richard Larson (Yale)Thoughts, and an open fourm, on the day's presentations 4:00Meeting 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 Reipurth, Bally & Devine pc

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 WFPC2 Overlay: Padgett et al Arce & Goodman 2002

Goodman & Arce 2002 Trail & Jet

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