ASTR 413
Building Stars: A Physical Model of Stellar Structure Fall 2024
Division III Q Quantitative/Formal Reasoning

Class Details

How does the Sun shine? How does the Sun evolve with time? What physical processes determine the power output of the Sun? In this course we will explore our modern understanding of how stars work, and why they have a range of sizes, temperatures, and luminosities. As we go, we will discuss the laws of physics at work in our Sun and other stars. Over the course of the semester, we will build a working computer model of the Sun using the basic laws of nuclear fusion, radiative transfer, thermal mechanics, and hydrostatic equilibrium.
The Class: Format: lecture; Lectures will include time for computer programming work
Limit: 10
Expected: 6
Class#: 1928
Grading: no pass/fail option, no fifth course option
Requirements/Evaluation: weekly problem sets, weekly coding homework assignments, two mid-term exams, and a final project
Prerequisites: PHYS 142 or 151, any prior class that makes use of programming, or permission of instructor
Enrollment Preferences: Astronomy, Astrophysics, or Physics majors, with first preference to Astronomy or Astrophysics majors
Distributions: Divison III Quantitative/Formal Reasoning
QFR Notes: In this course, students will use differential equations and numerical coding techniques to test and explore the relationships between physical laws using the Sun and other stars as examples. They will make quantitative comparisons between their calculations and observed stellar properties.

Class Grid

Updated 11:13 am

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