Table of ContentsObserving Star-Formation From the Interstellar Medium to Star-Forming Cores On-Line Version, 1999 Observing Star Formation From the ISM to Star-Forming Cores History: Theory and Optical Observations PPT Slide Important Distinction to Keep in Mind Spectral-Line Mapping Adds Velocity Dimension Orion: 13CO Channel Maps Molecular Outflows Jeans Mass, Virial Mass, and Filling Factors in the ISM What do we need to explain? Self-similar Structure on Scales from 100 pc to 0.1 pc...in Orion ìClumpî Mass Distribution ìLarsonís Lawî Scaling Relations (1981) PPT Slide Rough Virial Equilibrium in Star-forming regions Density-Velocity-Magnetic Field Structure Velocity Structure Velocity Coherent Cores* Where does the self-similarity end? PPT Slide Similar ìTransitionî Found in Spatial Distribution of Stars PPT Slide Magnetic Field Structure Using Polarization to Map Magnetic Fields Using Polarimetry to Map Field Structure PPT Slide Magnetic Field Structure: Emission Polarimetry Cloud Lifetimes The Effects of a Previous Generation of Stars Density-Velocity-Magnetic Field Structure Initial Conditions for Star-Formation (Version 99) PPT Slide Thanks to: What now? The Pleiades Bright Nebula: Orion Dark Nebula: The Horsehead The Electromagnetic Spectrum A Dense Core: L1489 A Dark Cloud: IC 5146 |
Author: Alyssa A. Goodman
Email: agoodman@cfa.harvard.edu Home Page: http://cfa-www.harvard.edu/~agoodman Other information: |