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Molecular Cloud Turbulence and Star Formation

Molecular Cloud Turbulence and Star Formation. Javier Ballesteros-Paredes 1 , Ralf Klessen 2 , Mordecai-Mark Mac Low 3 , Enrique Vazquez-Semadeni 1. 1 UNAM Morelia, Mexico, 2 AIP, Potsdam, Germany, 3 AMNH New York, USA. Protostars & Planets V: Oct. 24, 2005. Overview.

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1.02k views • 68 slides

Jets, Disks, and Protostars

Jets, Disks, and Protostars. 5 May 2003 Astronomy G9001 - Spring 2003 Prof. Mordecai-Mark Mac Low. How does collapse proceed?. Singular isothermal spheres have constant accretion rates Observed accretion rates appear to decline with time (older objects have lower L bol )

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352 views • 23 slides

Turbulence, Feedback, and Slow Star Formation

Turbulence, Feedback, and Slow Star Formation. Mark Krumholz Princeton University Hubble Fellows Symposium, April 21, 2006 Collaborators:

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347 views • 22 slides

Planetesimals in Turbulent Disks

Planetesimals in Turbulent Disks. Mordecai-Mark Mac Low Chao-Chin Yang American Museum of Natural History Jeffrey S. Oishi University of California at Berkeley Kristen Menou Columbia University. Planetesimals form within gas disks Laminar disks cause migration

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205 views • 20 slides

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Mac low - PowerPoint PPT Presentation

Molecular Cloud Turbulence and Star Formation

Jets, Disks, and Protostars

Turbulence, Feedback, and Slow Star Formation

Planetesimals in Turbulent Disks