1. Be able to describe the following methods or concepts
   1. trigonometric parallax (parallax angle, parsec)
   2. inverse square law
   3. apparent magnitude
   4. absolute magnitude
   5. distance modulus
2. Define and give an example of the use of
   1. blackbody radiation
   2. Wien's Law
   3. Stefan-Boltzmann equation
   4. Planck function
3. Explain what the color index is and how it is obtained for a star
4. Describe what a color-magnitude diagram and a color-color diagram are and why they are convenient for astronomers to use
5. Reproduce a "prototype" H-R Diagram labeling the main sequence, sub-giant, giant, supergiant, and white dwarf regions (luminosity classes V - I)
6. State, in general, what may be happening in the interiors of the stars at each of the above luminosity classes
7. Explain the basis for the Morgan-Keenan (M-K) system of spectral classification
8. Show how the Boltzmann equation leads to the concept of partition functions and the Saha equation.
9. Explain what is meant by statistical weights and partition functions.
10. Use the Boltzmann equation to calculate distribution of electrons between energy levels.
11. Use the Saha equation to calculate ratios of ionization stages.
12. Summarize how our knowledge of the Boltzmann and Saha equations leads to an understanding of the classification of stars (OBAFGKM) based upon the strengths of the absorption lines of elements

1. Kirchhoff's Laws
2. Doppler Shift

1. Define the following:
   1. specific intensity
   2. specific energy density
   3. radiation constant
   4. radiative flux
   5. blackbody radiation pressure
   6. line blanketing
   7. local thermodynamic equilibrium
   8. opacity (absorption coefficient)
   9. optical depth
   10. scattering
   11. Rossland Mean Opacity
   12. gaunt factor
2. Describe the physical underpinnings of
   1. bound-bound transitions
   2. bound-free absorption
   3. free-free absorption
   4. electron scattering
3. Explain why temperatures must decrease outwards from a star if absorption lines are to form.
4. Relate Kirchhoff's laws to optical depth
5. Give the basis for the limb darkening seen in the Sun
6. Define
   1. emission coefficient
   2. source function
   3. equation of radiative transfer
   4. plane-parallel
   5. gray atmosphere
   6. Eddington approximation

MORE WILL BE ADDED WHEN THE TIME COMES

1. Write code for solving the Saha equation
2. Successfully program the individual contributions to the continuous opacity
   1. Neutral hydrogen (bound-free, free-free)
   2. H-negative ion (bound-free, free-free)
   3. A "metal" that supplies electrons
   4. Thompson scattering
   5. Rayleigh scattering
3. Graph the results that show the opacity of each with respect to temperature
4. State the effect that electron pressure has on the contributions to the continuous opacity

Theory: Introduction to Modeling Stellar Interiors

1. Explain what is meant by:
   1. hydrostatic equilibrium
   2. mass conservation
   3. pressure equation of state
   4. pressure integral
   5. mass fraction
   6. degree of freedom
2. Follow the logic given for deriving the condition of hydrostatic equilibrium.
3. Follow the logic given for deriving the pressure integral.
4. Summarize what is meant by a "homologous" star and when such an approximation is reasonably accurate.
5. Explain or define the following:
   1. Kelvin-Helmholtz time scale
   2. nuclear time scale
   3. electron screening
   4. equilibrium abundances
6. Summarize the major fusion cycles and under what conditions each dominates.
7. Distinguish among radiation, convection, and conduction as means of energy transport in stars.
8. Define or explain the following:
   1. pressure scale height
   2. first law of thermodynamics
   3. specific heat
   4. adiabatic process
   5. superadiabatic
   6. mixing length (mixing length theory)
   7. characteristic length
   8. convective overshooting
   9. thermal and radiative equilibrium
   10. temperature gradient
9. Schematically explain how convection "works."
10. Summarize the major points of the mixing length theory.

1. Recognize the approximations made in the model and how the model could be made more realistic
2. Generate a series of models varying by mass with solar composition
3. Generate a series of models varying by mass for metal-poor stars
4. Generate a series of models varying by mass for metal-rich stars
5. Investigate the structural differences between the various models
6. Identify the convective zones in the models, and the dependency of the zones on the input parameters
7. Summarize how the central temperature, density, energy generation rate, and star's effective temperature vary with model
8. Compare the ZAMS for different metallicities

1. Preview what is meant by "stellar model." Summarize why our stellar models have seen huge leaps in accuracy (as measured by agreement with observations) over the past decade -- there is more than one reason.
2. Describe the foundations for the basic time-independent stellar structure equations.
3. Define or explain the following:
   1. equations of state
   2. constitutive relations
   3. boundary conditions
   4. Vogt-Russell Theorem
   5. polytropes
4. Successfully run BZAMS code by Hansen and Kawaler
5. Summarize the methods used to calculate a stellar model.
6. Outline the Schwarzschild and Henyey method in determining stellar structure.

Observations: Stellar Pulsation and Evolution

1. Terminology (define the following):
   • long-period variables
   • classical cepheids
   • period-luminosity relation
   • phase lag
   • instability strip
   • radial pulsation
   • overtones
   • epsilon-mechanism
   • kappa-mechanism
   • gamma-mechanism
   • nonradial pulsation
   • p-mode, f-mode, g-mode
   • helioseismology
2. State how our knowledge of classical Cepheids would have changed if the Small Magellanic Cloud had no Cepheid variable stars.
3. Explain why there is a phase lag between maximum luminosity and minimum radius for classical Cepheids.
4. Explain why the instability strip has a blue edge and a red edge -- that is, a definite width as a function of temperature and luminosity.
5. Summarize the physical underpinnings of the kappa-mechanism.
6. Summarize the physical underpinnings of the gamma-mechanism.

1. Explain what is meant by
   • interstellar reddening (interstellar de-bluing)
   • reflection nebula
   • translucent molecular clouds
   • giant molecular clouds
   • Bok globules
   • protostars
   • Jeans criterion, mass, and length
   • Hayashi track
   • zero-age main sequence
   • initial mass function
   • T-Tauri star
   • OB association
   • Herbig-Haro (HH) objects
   • circumstellar accretion disk
2. Describe the basic components of the interstellar medium.
3. Summarize the methods we use to observe neutral hydrogen, molecular hydrogen, and ionized hydrogen (HI, H₂, HII regions)
4. Identify the various (and fantastic) processes underway in the Orion star-forming region

1. Define the following:
   1. ZAMS
   2. Kelvin-Helmholtz time scale
   3. degenerate
2. Briefly summarize why there is a main sequence and why stars must increase in luminosity as they age.
3. Briefly summarize how the "thermostat" in the core of a solar-type star works, and why the fusion rate in the core must increase as the star ages.
4. Explain or define the following:
   1. shell fusion
   2. first, second, and third, dredge-up (dredges-up? dredge-ups?)
   3. helium core flash
   4. Explain Fig. 13.5
   5. Summarize the interior processes for subgiant, giant, horizontal branch, and asymptotic branch solar-type stars.
   6. Relate observational evidence for the increase in certain abundances to the "first, second, and third dredge-up" phases.

1. A basic understanding of stellar evolution codes.
2. Knowledge of how observations constrain the theory.
3. Summarize recent results in models of post-MS evolution.

1. Distinguish between Population I and Population II stars in as many ways as you can.
2. Explain or define the following:
   1. open cluster, globular cluster
   2. main-sequence fitting
   3. color-magnitude diagram
   4. isochrone
   5. turn-off point
   6. blue-stragglers
   7. distance modulus

1. An understanding of and appreciation for the nuances of matching observations and theory in color-magnitude diagrams of open and globular clusters.
2. Summarize the status of models where isochrones are used to match observations.
3. Briefly describe the results of recent observations on sub-dwarfs and the implications for stellar evolution. (References to be provided.)