Learning Outcomes for Astronomy 4101B, Stellar Astrophysics

• Apply the concept of dimensional analysis to estimate the self-gravitational energy and free-fall time of a star
• Understand the Jeans criterion for gravitational collapse and its relation to the Bonnor-Ebert sphere
• Be able to calculate the electrical and gravitational binding energies of objects of different masses and calculate the mass range in which each dominates
• Understand the quantum mechanical origin of degeneracy pressure and be able to estimate the relative importance of degeneracy pressure in a star by calculating the degeneracy parameter
• Identify the mechanisms of energy transport within a star and explain the conditions under which each will dominate, including being able to explain the criterion for the onset of convective instability
• Understand the dependence of nuclear binding energy per nucleon versus nucleon number in a nucleus, and how this accounts for nuclear energy generation in the universe. Master the use of the liquid drop model to estimate nuclear binding energies
• Understand all steps of the derivation of the Lane-Emden equation for stellar structure, including the applicability of polytropic relations to some stars and white dwarfs. Furthermore, students should be able to derive analytic solutions to the Lane-Emden equations where such solutions exist. Finally, know how to use a simple first or second-order numerical integration scheme to find numerical solutions to the Lane-Emden equation, and present them in a written report
• Identify and understand the full equations of stellar evolution including equations for energy transport and generation
• Be able to describe the key stages of evolution of both low mass and high mass stars, from the main sequence phase till the end of their life
• Understand the fate of stellar remnants as either a white dwarf, neutron star, or black hole, and the criteria for each outcome