Lectures topic-by-topic
This is a rough schedule of the topics we will cover. However, we may not get to all topics, depending on progress throughout the semester and student interests. The order roughly follows the presentation in Prof. Onno Pols' notes, but it is subject to changes as the course progresses.
N.B.: The notes provided here are intended to complement, not substitute other sources. You are strongly encouraged to consult books (e.g., Kippenhahn et al. 2012) and Prof. Onno Pols' notes.
- Color-magnitude and Hertzsprung-Russell diagram
Aim: Introduce color-magnitude diagrams, theoretical HR diagram, and how they relate to each other. Review some black body radiation and the basics of spectral formation to introduce spectral types.
- Binaries and mass measurements
Aim: Introduce the concept of binarity of stars as something not exotic. Walk through some classes of binaries based on how we observe them (astrometric, visual, spectroscopic, eclipsing) and how they can be used for empirical mass determination.
- Equation of state 1
Aim: Introduce Polytropic and ideal gas equation of state.
- Virial theorem
Aim: Introduce the Virial theorem in various forms. Demonstrate that stars "become hotter as they lose energy".
- Equation of state 2
Aim: Introduce other relevant equations of state
- Degenerate and non-relativistic gas
- Degenerate and relativistic gas
- Radiation-dominated EOS
- Radiative energy transport & conduction
Aim: Energy transport in radiative layers, the third stellar structure equation for non-polytropic models, and local energy conservation
- Opacities
Aim: discuss opacity, Rosseland mean opacities, atomic physics and other sources of opacity in a star
- Convection
Aim: Introduce convective instability, mixing length theory, and its limitations
- Nuclear energy generation
Aim: Introduce basics of nuclear energy generation through fusion, recall basic quantum mechanics elements, Gamow peak
- Nuclear reaction chains
Aim: Introduce pp chain, CN-NO bi-cycle, 3α burning, and later burning phases.
- Neutrino cooling + stellar evolution codes
Aim: discuss neutrino physics relevant to stars, cooling processes and thus complete the physics needed for 1D stellar evolution calculation. Introduce general principles of stellar structure and evolution codes and population synthesis.
- Guest lecture: Neutrinos in stars and using neural networks for Si burning
Guest lecturer: Dr. Aldana Grichener
- Guest Lecture: Roche potential
Guest Lecturer: Dr. Koushik Sen
- Notes from Dr. Sen available here
- (Notes from previous semester: Notes)
- Special Guest Lecture: Asteroseismology
Guest Lecturer: Prof. Conny Aerts from KU Leuven
- Recent review article
- Slides are available on d2l (enrolled students only)
Participation from Steward Observatory and NOIR lab will be encouraged
- Stellar atmospheres and outer boundary conditions
Aims: discuss in more detail the following:
- outer boundary conditions
- Saha equation
- line formation region
- line broadening mechanisms
- In class activity: Evolution 1
Aim: discuss the evolution of stars in an in-class activity based on
MESA-web models precomputed by the students
- In class activity: Evolution 2
Aim: discuss the evolution of stars in an in-class activity based on
MESA-web models precomputed by the students
- In class activity: Evolution 3
Aim: discuss the evolution of stars in an in-class activity based on
MESA-web models precomputed by the students
- In class activity: Evolution 4
Aim: discuss the evolution of stars in an in-class activity based on
MESA-web models precomputed by the students
Discuss written and oral presentations, and refereeing process.
- Supernovae
Aim: Introduce the nomenclature for supernovae, discuss the physics of core-collapse and the formation of compact objects
- Gravitational wave progenitors
Aim: introduce gravitational wave formation scenario (isolated binary and dynamical assembly), discuss some known uncertainties.
- Two student presentations
Aim: students will present a topic in stellar evolution to the class. The details of the schedule will be communicated on D2L
- Two student presentations
Aim: students will present a topic in stellar evolution to the class. The details of the schedule will be communicated on D2L
- Two student presentations
Aim: students will present a topic in stellar evolution to the class. The details of the schedule will be communicated on D2L
- Two student presentations
Aim: students will present a topic in stellar evolution to the class. The details of the schedule will be communicated on D2L
- Two student presentations
Aim: students will present a topic in stellar evolution to the class. The details of the schedule will be communicated on D2L
- One student presentations
Extra time can be used as backup