I. Astrophysical Processes
	Radiative transfer
		Equation of radiative transfer
		Kirchoff's law
		Blackbody radiation
		Behr absorption law
		Two conditions for emission lines
		Eddington-Barbier relation -- Gray atmosphere approximation
		Limb Darkening
	Opacity mechanisms
		Free-free, bound-free, bound-bound
		Absorption relative to H (n=3) in the Sun
			Negative H ion absorption (continuum)
			Helium absorption
			Metallic absorption
		Thomson scattering
		Rosselind mean opacity
		Boltzmann equation
		Saha equation
	Theory of line formation
		Voigt profile
		Turbulent line broadening
		Curve of growth
			Three components
			Calibrating curve of growth
			Finding excitation, ionization and kinetic temperatures
			Finding electron density and electron pressure
			Finding abundances
		Why are metal lines stronger in the blue region?
		Metallicty Effects
			Stellar lifetimes vs. metallicity
			Giants vs. main sequence stars -- metallic lines
			Line strengths vs. abundance of metals
	Hydrogen lines
		Stark effect
		Gravitational effects (giants vs. dwarfs)
		Temperature effects
		Dependence on He abundance (line wings)
		Hot stars vs cool stars
			Balmer discontinuity
			line strengths
		Stromgren photometry
			Determining ages from Stromgren colors
			Determining luminosity and effective Temperature
			Determining metallic line strengths
	Temperature stratification in stellar atmospheres
		Eddington approximation
		Two conditions for outward-increasing temperature gradient
		Explanation of the transition layer
		Emission/Absorption change in Sun at 1700 Angstroms
		Effect of temperature stratification on line depth
		Flux iteration method
	Pressure stratification
		Hydrostatic equilibrium
		Pressure and effective gravity
	Two color diagram
		What we expect vs. what we see
		Color change mechanisms
		Main sequence stars vs. giants
	Hydrodynamics
		Eulerian vs. Lagrangean view
		Basic equations (5 --> 1)
		Radiative flux and Milne-Eddington approximation
		Boussinesq approximation
		Rayleigh number and Prandtl number
		Turbulence
			Kolmogorov spectrum
			Conditions for applicability
	Shock waves
		Typical equations
			Hugoniot relation
			Stellar wind equation
		Structure behind the shock wave (pressure and temperature)
		Shocks and HII regions
		Supernovae remnants (optical depth vs. time)
	Magnetohydrodynamics
		Alfven's theorem
		Magnetic Reynolds number
		Force-free fields
		MHD convection
		Alfven waves
	Thermodynamics
		Gibbs vs. Boltzmann distribution
		Partition function
	Degeneracy
		Gamma factor = Coulomb/Thermal energy
		Chemical potential
		Relativistic vs. non-relativistic
		Coulomb interactions and density
		Electron vs. proton degeneracy
		Debye theory
		Hot Thomas-Fermi model
	Neutrinos
		Solar neutrino problem, pp chains
		Cl-37 and GA-71 detectors
		MSW effect
	Pulsars
		Structure
		Power sources
	Cosmic abundances (elements and isotopes)
		R and S process
		Nucleosynthesis (see Hot Big Bang)
		Milky Way vs. Magellanic clouds

II.  Solar System
	Origin of the solar system
		Cameron-Pine model
		Planetary accretion
		Goldreich-Ward hypothesis
		Safronov accretion
		Equilibrium condensation
			Evidence for condensation
			Condensation temperatures
		Carbon and Oxygen abundances (Cold Trap)
		Small masses of Mars and Mercury
		Jupiter
		Age of the solar system, time scale for formation
		Mg-26 and Ne-22 excesses, Pu-244
		Oort cloud
	Planetary detection techniques
		Evidence of other planetary systems
		Vega and Beta Pictoris
	Planetary atmospheres
		Earth and volatiles
		Meteors from the outer solar system (asteroid belt)
		Mars
		Volatile vs. refractory elements
		Venus
		Titan
		Triton
		Pluto
	Meteorites
		Classes of meteorites
		Chondrules
		Dust
			Poynting-Robertson effect
			IRAS dust bands
		Parent bodies
		KT event -- pro and con
	Volcanism
		Earth vs. Io
		Venus
		Mars
	The moon
		Origin theories
		Oxygen isotopes
		Mare formation and early bombardment
	Giant planet basics
		Jupiter
			Great red spot
			Moons
		Saturn
		Uranus and Neptune
		Ring systems

III.  Stellar Structure and Evolution
	Stellar models (basics)
		Limits to pressure and temperature
		Homologous stars
		4 basic equations
		Numerical techniques (Schwarzschild vs. Henyey)
		Polytropic stars
	Convection and mixing
		Schwarzschild criterion
		Mixing length theory
			Biermann theory and Peclet number
			Energy transport vs. mixing length
			Temperature stratification vs. mixing length
			Observational evidence of mixing
			Lithium gap
			Mixing during the Helium flash
		Convective overshoot
		Deep convection zones in F and G stars
	Protostars
		Observational evidence
		T Tauri stars
		Herbig Ae stars
		YY Ori stars
	Hayashi track
		Where is it located?
		Why are Hayashi track stars convective?
		Dependence on metallicity
		Hayashi vs Henyey phase
		Protostar formation
	Helioseismology
		Problems that can be addressed
		Non-radial oscillations (pressure and gravity waves)
	Chromosphere
		Spicules
		Upper chromosphere
		Granulation
			Characteristics
			Supergranulation
			Observations of granulation
	Solar corona
		L-corona
		K-corona
		F-corona
		Coronal temperatures
		Baumbach-Allen method
		Recombination processes
		Radio corona
	Solar activity
		Sunspots
		Prominences
		Solar flares
		Six phenomena associated with flares
	Main-Sequence spin down
	White Dwarfs
		DA's vs. non-DA's
		M-R relation
		Metals in atmospheres
		Crystal structure
		Four current problems
		Debye cooling
	Cepheids
		Instability strip
		Period-density relation, free-fall time
		PL & PLC relation
		Pop I vs. pop II  (Mass-Luminosity relation)
		IR observations
		Cepheids vs. RR Lyrae stars
	Novae
		Accretion disks
		Eruptions
	Mass loss
		P Cygni profiles
		Evidence from CO imaging
		Eddington luminosity
		R Cr B stars
		Miscellaneous stellar types
	Mass-Radius relation
		Equation of state
		Conditions for such a relation
		Nuclear energy generation rate
		Opacity mechanism
		Dependence on convection zones
		White Dwarfs (relativistic vs. non-relativistic)
	Herbig-Haro objects

IV.  Interstellar Medium
	HII regions
		Detailed balancing vs Rosselind uncompensated cycles
		Milne relations
		Stromgren spheres
		Spectral features
		Milky Way vs. Magellanic Clouds
		Wolf-Rayet bubbles
		Formation
	Planetary Nebulae
		Spectral features
		Ionization equilibrium (and statistical equilibrium)
		Saha equation -- why is it not a good appx. to ion. state?
	21 cm radiation
		Stimulated vs. spontaneous decay
		Equation of detailed balancing
	4 major phases of ISM
		Density
		Temperature
		Pressure
		Ionization states
		Distribution
		Detection techniques
		Absorption properties with respect to wavelength
		Balmer and Paschen lines as measure of reddening (elec. T)
		C-O observations (what does CO trace)

V.  Galaxies and Cosmology
	Galaxy classification
		Hubble "tuning fork" diagram
		Brightness profiles
		Ellipticals vs. spirals
	Globular clusters
		Distance determination methods
		Abundances and the H-R diagram
		Age vs. abundaces
		Relaxation time
		Dynamical time
	Tracers
		Spiral arms
		Scale heights of various things
	Galactic abundances
		General equations
		G-dwarf problem
	Tensor Virial Theorem
	Galactic Dynamics
		Integrals of motion
		Oort constants
		Solar motion
		Sprial structure
		Initial mass function
		Luminosity function
	QSO's and AGN's
	Galactic distances
	Evidence for dark matter
		Oort's analysis
		Galaxy rotation curves
		Galaxy cluster dynamics
		Lyman-alpha forest
		X-ray background
		Candidates for dark matter
	Cosmological models
		Newtonian cosmology
			Friedman equation
			Redshift dependencies
			Deceleration parameter
			Equations of state
		Cosmological masses
		Perturbations
		Microwave background radiation
			Sources of anisotropy
			Evidence of universal nature
		Inflation
		Birkhoff's theorem
	Hot Big Bang
		Chronology
		Baryon density
		Nucleosynthesis
			Inhomogeneities
			Abundances and constraints
	Hubble's Law
		Evidence for variations from the Hubble flow
		Problems with high and low values of H

VI.  Observational Techniques; Miscellaneous
	Hour angle, sidereal time
	Ultraviolet observations
		Dominant UV sources
		Problems with satellite UV observations
	X-ray observations
		X-ray bursts
		X-ray background
		Thermal bremmstrahlung, synchrotron radiation
		Inter-Galactic Medium
			Cooling mechanisms
			Total mass
	CCD observations
		Extinction
		Three sources of night-sky brightness
		Signal-to-Noise ratio
		Read noise, shot noise, binning
		Effects of co-adding images
		Sensitivity ranges of plates, photometers and CCD's