1	Astr 1050 Wed. Mar. 9, 2005 Today: Hw 7 solutions Review topics chapters 5-9
2	Review Chapters 5-9 Chapter 5: Just a few topics Telescope resolution Function of size, wavelength Observations at different wavelengths Electromagnetic Spectrum Telescopes in space (why)
3	Review Chapters 5-9 Chapter 6: Starlight and Atoms Model Atom, parts, energy levels Emission and Absorption Lines Blackbody Radiation Wien’s Law, Steffan-Boltzmann Law Spectra of Stars Balmer thermometer, spectral types (OBAFGKM) Doppler Effect
4	Review Chapters 5-9 Chapter 7: The Sun Atmospheric Structure Temperature, density, etc., with radius Sunspots/Magnetic Phenomena What are they? Why do they exist? Nuclear Fusion – proton-proton chain What is it? How does it produce energy? Solar Neutrino “Problem” What is it? Is it still a problem?
5	Review Chapters 5-9 Chapter 7: The Sun – example question Q. The fusion process in the sun, the "proton-proton" chain, requires high temperatures because: c of the ground-state energy of the Hydrogen atom. c of the presence of Helium atoms. c the colliding protons need high energy to overcome the Coulomb barrier. c of the need for low density. c the neutrinos carry more energy away than the reaction produces.
6	Review Chapters 5-9 Chapter 8: The Properties of Stars Distances to Stars Parallax and Parsecs Spectroscopic Parallax Intrinsic Brightness: Luminosity Absolute Magnitude Luminosity, Radius, and Temperature Hertzsprung-Russell (H-R) Diagram Luminosity Classes (e.g., Main Sequence, giant) Masses of Stars Binary Stars and Kepler’s Law Mass-Luminosity Relationship
7	Review Chapters 5-9 Chapter 8: Properties of Stars—example question Q. A star’s luminosity depends only on the star’s: c distance and diameter. c temperature and distance. c distance. c temperature and diameter. c apparent magnitude Another version of the question can be made for apparent magnitude .
8	Review Chapters 5-9 Ch. 9: The Formation & Structure of Stars Interstellar Medium Types of Nebulae (emission, reflection, dark) Interstellar Reddening from dust Star formation Protostar Evolution on H-R Diagram Fusion (CNO cycle, etc.) Pressure-Temperature “Thermostat” Stellar Structure (hydrostatic equilibrium, etc.) Convection, radiation, and opacity Stellar Lifetimes