Topics

The list below is a tentative list of topics to be covered in this course. The list includes references to sectins of some of the textbooks where those topics are covered. The actual topics covered in class may depart somewhat from this list.

Introduction and Fundamentals

• Fundamental properties of stars and how they are measured
  [A-292 notes; Guidry §1, Bohm §1]

• The H-R diagram and a rapid summary of stellar evolution (to set the stage)
  [A-292 notes; Prialnik §1.4; Guidry §2]

• Correlations between stellar properties
  [Illustrations and references therein]

The Equations of Stellar Structure

• Mass continuity, hydrostatic equilibrium, energy generation and transport, thermal structure.
  [Prialnik §§2.1–2.3; Guidry §§4.1–4.3; Bohm §§2.1,3.1]

• Overview of Classical Thermodynamics
  [Prialnik §§2.1–2.3; Guidry §§3.3,4.1–4.3]

• The Virial Theorem for a Star and Applications
  [Prialnik §§4.5–4.6; Guidry  §§4.5–4.7 ]

• Important Stellar Time scales
  [Prialnik §2.8; Guidry §§4.4,4.9]

Radiative Energy Transport in Stellar Interiors

• Physics of heat transport by particle diffusion 

• Radiative transfer (more formal treatment)

• Sources of opacity 

Convection

[Bohm §§5, 6.1–6.4; Prialnik §§6.5–6.6]

• Criteria for convective (in)stability

• Convective energy transport

• Triggering of convection

• First encounter with internal structure of the Sun. Convection in the Sun

The Equation of State (i.e., what sets the pressure)

• The pressure integral

• Pressure by a gas of classical, non-Relativistic particles

• Pressure by a gas of quantum-mechanical particle (in general terms)

• Degeneracy Pressure

Nuclear Energy Generation

• Notation and conventions

• Non-resonant reactions and tunneling, Resonant reactions.

• Formalism for nuclear reaction rates 

• Hydrogen burning via the p–p chain

• Hydrogen burning via the CNO cycle

• Helium burning via the 3α process

• Burning of heavier elements

Homology Relations and Simple Stellar Models

• Homology in mathematical terms 

• Simple stellar models based on homology 

• Polytropic models and the Lane-Emden Equation 

• Comparison of simple models with observations 

• Luminosity evolution on the Main Sequence

More Sophisticated Models and the Main Sequence

• Internal structure of the Sun, revisited

• Structure and characteristics of main sequence stars

Dynamic Homology and Stability 

• Homologous expansion and contraction

• Gravothermal specific heat

• Stability of core burning

• Stability of shell burning

Post-Main Sequence Evolution

• Leaving the main sequence and crossing the Hertzsprunbg gap

• The red giant phase and the He flash

• Core He burning and the  horizontal branch

• AGB evolution an thermal pulses

If time permits, we will continue to cover some of the following topics, although not at the same depth as the previous topics.

Late Stages of Stellar Evolution and Stellar Remnants

• Low-mass stars: mass loss and the planetary nebula phase

• Intermediate-mass stars and "advanced" nuclear burning

• White dwarfs

• High-mass stars: "advanced" burning and supernovae (nucleosynthesis during supernovae)

• Neutron stars and black holes

Interacting Binary Stars

• Phenomenology of interacting binaries

• The Roche potential and mass transfer

• Stability of mass transfer and orbital evolution

• Accretion

• Evolutionary pathways for compact binaries and gravitational wave sources