Observing Star-Formation From the Interstellar Medium to Star-Forming Cores On-Line Version, 1999

2/12/99


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Table of Contents

Observing 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

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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

žClumpÓ Mass Distribution

žLarsonŪs LawÓ Scaling Relations (1981)

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Rough Virial Equilibrium in Star-forming regions

Density-Velocity-Magnetic Field Structure

Velocity Structure

Velocity Coherent Cores* Where does the self-similarity end?

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Similar žTransitionÓ Found in Spatial Distribution of Stars

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Magnetic Field Structure

Using Polarization to Map Magnetic Fields

Using Polarimetry to Map Field Structure

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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)

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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:
Presentation prepared in conjunction with Astronomy 97, Harvard University, Spring 1999.

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