| Chapter 5: Just a few topics | |||
| Telescope resolution | |||
| Function of size, wavelength | |||
| Telescopes in space (why) | |||
| Telescopes in different parts of the spectrum | |||
| 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 | |||
| 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? | |||
| 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. |
| 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 | |||
| Problem from textbook: | |
| mV MV d (pc) P (arcsec) | |
| ___ 7 10 _______ | |
| 11 ___ 1000 _______ | |
| ___ -2 ____ 0.025 | |
| 4 ___ ____ 0.040 |
| Problem #4: | |
| m MV d (pc) P (arcsec) | |
| 7 7 10 0.1 | |
| 11 1 1000 0.001 | |
| 1 -2 40 0.025 | |
| 4 2 25 0.040 |
| 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 . | ||
| Chapter 9: Formation and Structure of Stars | ||
| Interstellar Medium and different sorts of nebulae, reddening | ||
| Protostars, star formation (on HR diagram) | ||
| Fusion in stars | ||
| CNO cycle | ||
| Heavy element fusion | ||
| Lifetimes on the main sequence | ||
| The Orion Nebula as a star-forming region | ||