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UA Course Catalog Prerequisites:
It would also help undergraduates to have taken at least AY 101, Introductory Astronomy for non-science majors, or, preferably, AY 204 and 206, Introductory Astronomy for science majors. For graduate students, no prior astronomy courses are expected.
Course Description and Credit Hours
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Lecture Meeting: Monday, Wednesday, and Friday 12:00-12:50 in 328 Gallalee Hall.
Required Texts from UA Supply Store:
- HANSEN / STELLAR INTERIORS (W/CD) (Required)
- HANSEN (RENTAL) / (RENTAL) STELLAR INTERIORS (W/CD) (RENTAL)
- BINNEY / GALACTIC ASTRONOMY (Optional)
- BINNEY (RENTAL) / (RENTAL) GALACTIC ASTRONOMY (RENTAL)
- CLAYTON / PRINCIPLES OF STELLAR EVOLUTION & NUCLEOSYNTHESIS (Required)
Texts:Stellar Interiors by Hansen, Kawaler, and Trimble; Principles of Stellar Evolution and Nucleosynthesis by Clayton
Supplementary text: Galactic Astronomy by Binney and Merrifield
A note on texts: Most material will be drawn from Hansen, Kawaler, & Trimble, which is quite readable. Some topics requiring more detail on nuclear processes will be drawn from Clayton. Binney and Merrifield is a suggested reference text for general astronomical background, conventions, and arcana. Other upper-level general astronomy texts can fill a similar role.
Student Learning Outcomes
Course goals phrased as learning outcomes:
At the conclusion of this course, all students will be able to
describe the interior structure, appearance, and activity of stellar objects from formation to remnant, and how it depends on the star's mass.
demonstrate understanding of the macrophysical or microphysical process that governs the transitions of stars from one stage of their life cycle to the next, and dominates their behavior during each stage.
demonstrate in what way many gross stellar properties arise from simple scaling relations, how such relations can capture basic physical understanding, and be able to apply scaling relations to triage and assess new astrophysical problems.
discuss and draw conclusions about how the physics-based components (e.g. microphysical material properties; measured and calculated nuclear interactions) of modern numerical models of stars, stellar processes or stellar populations can influence the outcome of calculations for both individual stars and stellar populations, clusters and galaxies, and their products.
In addition, graduate students will be able to
understand the context of ongoing research in stars, stellar populations and stellar physics, at a level that enables comprehension of the content and scope of research literature which is not exclusively specialist (reviews, ApJ letters, proposals, topical sessions at national meetings, well-written topical articles).
identify the areas of ongoing research into stellar processes and the physics which is important for stellar properties and products, characterize the unanswered questions, and integrate future developments in these areas into their understanding of stars.
Other Course Materials
Students are expected to have access to a unix computing environment of some form. Mac OS X, Linux, or others are all sufficient. Students should consult with the instructor if they need assistance with this, as some university facilities are available, though typically a student's personal computer is most convenient.
Lecture notes, homeworks and various other resources (figures from class, links to papers, inlists for MESA) will be available through the public class webpage or the class page on blackboard.
Outline of Topics
Hydrostatics and thermodynamics of self-gravitating objects
Hydrostatic equilibrium in spherical symmetry, Virial theorem
Equations of state
Simple stellar models and gravitational contraction
Importance of radiation pressure
Diffusion of heat and stellar luminosities
Gravitational collapse of molecular clouds, Jeans mass
Evolution of protostars, fully convective models. The Hayashi track
Life on the main sequence
Thermonuclear energy generation - processes and rates
CNO vs. pp burning, the Solar neutrino problem
Degeneracy and brown dwarf formation
Stellar masses, temperature, radii and lifetimes. IMF
Convection. where and why it occurs
The Saha equation, simple atmospheres, spectroscopy
Life after the main sequence
Degeneracy during stellar evolution. Chandrasekhar limit.
Low mass stars: red giants, mass loss, shell burning
Massive stars: CO burning, Ne photodisintegration, neutrinos
Collapse of Iron cores, core collapse supernovae, nucleosynthesis
Colapsed star: structure and emission in isolation
White dwarf formation, thermal cooling and observations
Neutron star formation, structure and cooling
Approximate Daily Topic Schedule
Part 1: Hydrostatics and thermodynamics of self-gravitating objects
Course overview, observed stellar properties
Stellar structure equations, Stars in the galaxy
MESA getting started day
Thermodynamics of a (quasi-)hydrostatic star
Polytropes, Eddington Standard Model
Heat transport by convection
Part 2: Star formation
Star formation, protostars
Energy and contraction
Initial mass function, starting nuclear fusion
Nuclear fusion: tunneling
Nuclear fusion for a star
First fusion stages
Part 3: Life on the main sequence
Deuterium, Lithium burning
pp and CNO cycles
CNO burning stars
Upper and lower main sequence (CNO and core convection)
Surface T and Saha equation for ionization
Core hydrogen burning evolution
Hydrogen depletion, the S-C threshold for the helium core
after helium core formation, helium ignition
Part 4: Life after the main sequence
How to burn helium
-- (fall break)
Helium core flash, beginning of the end for <6Msun
Asymptotic giants and thermal pulses
white dwarf masses, start advance burning stages (MESA project topics due)
Advanced burning stages
Inert core formation, Chandrasekhar mass
Supernova explosive nucleosynthesis
Part 5: Collapsed stars
White dwarf cooling
-- (thanksgiving holiday)
MESA project workshop
White dwarf interior, crystallization
MESA project presentations
MESA project presentations
Final Exam (time by appointment)
Exams and Assignments
Semi-weekly (approximately every other week) homeworks will be assigned. Each student is expected to complete the homework individually, though discussion among students is fine. Each homework will consist of some problems for undergraduates (AY 450), some shared problems for both undergraduate and graduate students, and some problems for graduate students only (AY 550).
Each student will perform a semester project on a topic of their choosing using the MESA stellar evolution code. Results will be presented in an in-class presentation of about 10 minutes and written up briefly in about 5 pages. The topic will be chosen by the date indicated in the class schedule, in consultation with the instructor. Graduate student (AY 550) projects are expected to be broader in scope, for example exploring multiple parameters or more subtle questions, than undergraduate (AY 450) projects.
The final exam will be an individually administered oral exam with the instructor approximately 30 minutes in length. Undergraduates enrolled in AY 450 will have a lower expectation of performance than graduate students enrolled in AY 550.
45% homework, 30% project based on MESA stellar evolution code, 25% oral final exam
Policy on Missed Exams and Coursework
All coursework must be completed. Late work will be accepted with a documented excuse. Generally late work received after solutions are distributed and without appropriate arrangements with the instructor will receive a large penalty.
Attendance and participation in all classes is expected (except for circumstances outside of the student's control) despite attendence not forming any part of the formal grade.
Notification of Changes
The instructor will make every effort to follow the guidelines of this syllabus as listed; however, the instructor reserves the right to amend this document as the need arises. In such instances, the instructor will notify students in class and/or via email and will endeavor to provide reasonable time for students to adjust to any changes.
Statement on Academic Misconduct
Students are expected to be familiar with and adhere to the official Academic Misconduct Policy provided in the Online Catalog.
Statement On Disability Accommodations
Contact the Office of Disability Services (ODS) as detailed in the Online Catalog.
Severe Weather Protocol
Please see the latest Severe Weather Guidelines in the Online Catalog.
Pregnant Student Accommodations
Title IX protects against discrimination related to pregnancy or parental status. If you are pregnant and will need accommodations for this class, please review the University’s FAQs on the UAct website.
Under the Guidelines for Religious Holiday Observances, students should notify the instructor in writing or via email during the first two weeks of the semester of their intention to be absent from class for religious observance. The instructor will work to provide reasonable opportunity to complete academic responsibilities as long as that does not interfere with the academic integrity of the course. See full guidelines at Religious Holiday Observances Guidelines.
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