The Physics of the Interstellar Medium (AY208, v.Y2K)
Summary: This course is intended to give its students a broad knowledge of how the various constituents of the Interstellar Medium (ISM) interact physically with each other. A detailed outline of the topics to be discussed is provided beginning on the next page. The course will have bi-weekly meetings, and will rely on student preparation and participation.
Prerequisites: Familiarity with Radiative Transfer; good knowledge of Quantum Mechanics; familiarity with Basic Astronomy.
Readings: Sections of texts will be assigned with each Problem Set and will be on reserve in Wolbach Library. In addition, seminal and/or recent relevant journal articles will be assigned, and will be used in class as a launching point for discussion.
Course Meetings: Two 1.5-hour meetings per week. Students should read the assigned journal articles & review the relevant text sections as the course progresses. Normally, Tuesday meetings will be "lecture"-style, Thursdays will be half lecture, half discussion. The discussions will focus on one relevant research article, and will be led by a different student each week. Lecture notes will be posted to the course Web site weekly.
Guest Lectures: Occasionally during the term, ISM experts from the CfA will give a guest lecture on their specialty. These lectures will cover material already listed in the syllabus below.
Problem Sets: Approximately every two weeks. Problems will cover the "basics," along with more in-depth questions that will often require some research in the literature. Several of the problems will be based on the journal articles that form part of the assigned readings.
Exams: The course will have a take-home final exam, and no in-class exams.
Journal Article Presentations: Throughout the term, each student will be responsible for leading an in-class discussion on one Journal article. In addition to leading the discussion, the student will post, at least 42 hours in advance of the article discussion, a web page that includes a short summary and critique of the article, and relevant links to other sites. Instructions on how to post the page will be sent by email.
Grading: 40% final exam; 35% problem sets; 25% Journal article presentation (web & oral)
Course Web Site: http://cfa-www.harvard.edu/~agoodman/astro208/ Links to problem sets, reading assignments, WWW links relevant to the course, and lecture notes will be posted here.
Instructor: Alyssa Goodman, office hours by appointment. Room M-330 at the 160 Concord Avenue building of the Center for Astrophysics, 495-9278, firstname.lastname@example.org.
Teaching Fellow: Hannah Jang-Condell, office hours by appointment, and TBA. Room P-202 at the 60 Garden Street building of the Center for Astrophysics, 495-2536, email@example.com.
The Physics of the Interstellar Medium
Introduction: Defining Features of "a" galactic ISM
The "Modern" View & How we Got It
Nature of the ISM: Above "Variables" Inseparable
Kinetic Equilibrium & Radiative Processes: Overview
- Gas, Dust, Electrons, Cosmic Rays, Photons
- Scale Height & Radial Distribution
- Interstellar "Clouds"
- Extragalactic Perspective
- Comparison with Stellar Distribution
- Temperature Structure
- The "Hot," "Cold," and "Warm" ISM
- Ionization State
- Interactions with of ISM & Stars
- example: Strömgren Sphere Analysis
- Influence of Cosmic Rays
- Density Structure
- Measures of Column Density and Volume Density
- Hierarchy of Interstellar "Clouds"
- Velocity Structure
- Galactic Scales
- Within Individual "Clouds"
- Magnetic Field Structure
- Flux-freezing & Ambipolar Diffusion
- Measurement Techniques
- Confinement of Cosmic Rays & "Support" of Clouds
- Time Scales & Stability
- Virial Equilibrium
- Instabilities (e.g. Jeans)
- Partition Function
- Kinetic, Excitation, Color, Antenna, Bolometric, and Other "Temperatures"
- Non-equilibrium Distributions
- Non-LTE (Pumping)
The ISM of the Milky Way
- Radiative Transfer Definitions
- Emission & Absorption Coefficients
- Continuum Emission
- Bremsstrahlung & Synchrotron
- Scattering Processes
- The Influence of Shocks
- In SNe, Star-forming Regions, and in Accretion Disks (more below)
- What combination of the above will be observed where?
- Depends on l.o.s. Temperature, Density, Abundance, and Velocity Distribution
Introduction: The Multi-Phase Paradigm
The "Cold" ISM
- Basic Assumptions
- Pressure, Mass, and Energy Balance
- Time Dependence
- History and Definitions
- "Out the window"
- Permitted and Forbidden Transitions
- Critical Density
- Atomic Gas (H I)
- Origin of the 21-cm Line: Flipping a Spin
- 21-cm line Surveys
- Collisional Excitation
- Optical Depth Considerations
- High-Velocity and High-Latitude Clouds
- Origin & Evolution
- Molecular Gas
- The Difficulty in Directly Observing H2
- Role of "Trace" Species"
- Molecular Line Mapping
- Masers (more in AGN discussion)
Molecules & Dust Together
- What is dust?
- Cause of interstellar extinction
- Range of Sizes from "Big Molecules" to Planetesimals
- Measured/Measurable Properties
- Optical Efficiency Factors
- Cross-sections for emission, absorption & scattering
- Extinction as a function of
- Total-to-Selective Extinction
- Spectral "features"
- Thermal Emission as a function of
- Is the blackbody approximation adequate?
- Are grains fractal?
- Polarization as afunction of
- Polarization due to Scattering
- Polarization due to Aligned Grains
- Using Polarization to Map B
- Polarization of Background Starlight
- Polarization of Thermal Emission
Heating & Cooling
- Formation of Molecules
- on Dust
- in the Gas Phase
- Destruction of Molecules
- by cosmic rays
- by photons
- by electrons & collisions
The "Hot" ISM
- Atomic & Molecular Coolants
- Dust Heating & Cooling
X-rays as a "Probe" of the ISM
- The Warm Neutral Medium: Broad H I lines
- The Warm Ionized Medium: Absorption Line Observations
- Radio Continuum Emission & Pulsars as Probes
- Distinguishing Bremsstrahlung from Synchrotron from Thermal Emission
- Polarization of Synchrotron Emission
- Rotation and Dispersion Measure
- Faraday Rotation
- RM/DM of Pulsars as a Probe of B
How Appropriate are Multi-Phase Models?
Interaction of Photons with the ISM
- X-ray "Shadows" of Molecular Clouds
- Calibration of the CO/H2 ratio (a.k.a. the "X-factor")
H II Regions & Photon-Dominated Regions
Heating and Cooling in H II Regions
Ionization Fraction & Chemical Balance in PDRs
- Strömgren Spheres
- "Clumpy" H II Regions
- Radio Recombination Lines
- General Shock Physics (Basic Equations, More Later)
- Compact and Ultra-Compact H II Regions
- Cometary H II Regions & Bow shock models
- Champagne-flow models
The Effect of High-Energy Photons on Molecular Clouds (e.g. in AGNe)
Star Formation in Molecular Clouds
- Measurements & Theories
- Effects on Ion-Neutral Coupling
Giant Molecular Clouds, Dark Clouds, Cloud Cores & the "Modern" Star Formation Paradigm
Cloud Support & Dynamics
The Role of Magnetic Fields in Star-Forming Regions (Part II)
- "Larsons Laws" & Virial Equilibrium
- Role of Magnetic Fields (Part I)
- Pressure Confinement
- Self-similar Structure
- What matters: Static Fields, Turbulence and/or Waves?
- Measurements of Field Strength
- Measurements of Field Structure
- MHD Simulations
Infall & Outflow
- Radiated Spectrum & Dependence on Viewing Angle
- The Role of Scattered Light
- Fragmentation & Instabilities
- Planet Formation
What Determines the Initial Mass Function of Stars?
- Expectations & Observations of Inflow
Interaction of Stellar Winds with the ISM
- Agglomeration Theories
- Fragmentation Scenarios
- "Fractal" Scenarios & Speculation
Winds from Young Stars
Mass Loss from Main Sequence & Evolved Stars
- Observed Properties of Outflows (on ~pc scales)
- Comparison of Outflow Mechanical Luminosity & Protostars Luminosity
- Aspect Ratio
- "Hubble Flow"
- Observed Properties of Jets (on ~0.1 pc scales)
- Emission from Herbig-Haro Objects and "Shocked" H2
- Continuum and Line Radiation Produced in Shocks
- Temperature, Ionization & Velocity Structure of Jets
- Energy dissipated
- Collimation Mechanism
- The "X-wind Model"
- Other proposals
- Origin of the Relevant B-field: Stellar or Interstellar?
- Jet-driven Outflows
- (M)HD Simulations of Jets & Outflows
- FU Orionis Activity & Episodic Jets: Magnetic Variability?
- Production of Dust
- Subsequent Processing to Produce Observed I-S Dust
- Planetary Nebulae
The ISM in External Galaxies at z~0
- Multi-Wavelength Radiation
- Optical Line & Continuum Emission
- Synchrotron Radiation
- Shock Physics & Chemistry
- Time Evolution: Phases in the Expansion
- Energy Deposited into ISM
Variations with the Realm of "Normal" Galaxies
"Active" and "Starburst" Galaxies
- Density Structure
- Velocity Structure & Rotation Curves
- Origin of High-velocity Clouds
- Metallicity Variations
- Magnetic Field Structure
The Intergalactic Medium
- The Cause(s) of Starbursts
- Jets and Disks in AGNe
Observations: Present & Future
Relationship of the ISM & IGM
- Lyman- clouds, Lyman Limit systems and the Lyman Forest
- Metal-line systems
The "ISM" at z>>0
- Coronal Gas?
- Intracluster Gas in Galaxy Clusters
- Highly Redshifted CO
- Future Prospects: Other lines, other techniques
Polarization of the Microwave Background
- Lower Metallicity?
- Origin of the Intergalactic & Interstellar Magnetic Fields
- Observational Feasibility Estimates
…Specific "historical" lectures are not included in this outline. Instead, I will incorporate an historical perspective into topical lectures, whenever it is appropriate. For example, in presenting what appear to be "simple models" like the Strömgren sphere or Jeans collapse, I will discuss the observations Strömgren or Jeans would have had available at the time they made their models.
…Similarly, specific "observational technique" lectures are not included. Techniques will be discussed in context.