Star Formation in a Dynamic Interstellar Medium

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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
Brommstay tuned
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The Plan
Time Speaker Topic 0940 Alyssa Goodman
(CfA/Yale) Introduction 1000 Phil Myers
(CfA) What are the properties of the observed
environment for star formation? 1040 Coffee
Break 1100 Richard Larson What are the real
observational constraints on the
IMF? 1140 Paolo Padoan (Caltech/JPL) What have
we learned from numerical simulations of the
star-forming ISM, on gt1 pc scales? 1220 Lunc
h 150 Bruce Elmegreen (IBM) On what scale is
an IMF determined, and how might the answer
to this question change? (Opinion 1) 230 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) 310 Coffee Break 330 Richard Larson
(Yale) Thoughts, and an open fourm, on the day's
presentations 400 Meeting Adjourns, but
those interested stay on to chat
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Questions Raised by a Dynamic View of Star
Formation
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4. Powering source of (some) outflows may move
rapidly through ISM.
Goodman Arce 2002
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Giant Herbig-Haro Flow inPV Ceph
1 pc
Reipurth, Bally Devine 1997
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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
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4. Powering source of (some) outflows may move
rapidly through ISM.
Goodman Arce 2002
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HST WFPC2 Overlay Padgett et al. 2002
Arce Goodman 2002
Goodman Arce 2002
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Trail Jet
Goodman Arce 2002
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How much gas will be pulled along for the ride?
Goodman Arce 2002
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Insights from a Plasmon Model
Initial jet 250 km s-1 star motion 10 km s-1
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Insights from a Plasmon Model