Objectives: Properties of Stars

Chapter Objectives: In this chapter we learn that our Sun is a very average star that falls in the middle of the stellar range of possible luminosities, surface temperatures, and masses. We will study the laws of nuclear physics in order to understand how stars are able to release tremendous amounts of energy and yet remain so stable during their main sequence lifetimes. We will use stellar models to describe the energy transport that takes place in the hidden interiors of stars. We will show how astronomers determine the distances to stars and how they trace their motions in our sky. The H-R Diagram will be introduced as a graphical summary of some important characteristics of stars.

Chapter Skills: After studying this chapter you should be able to

  1. Explain the mass-energy conversion relation contained in Einstein's famous equation E=mc2.
  2. Relate "missing mass" and binding energy to the release of energy during nuclear fission and nuclear fusion.
  3. Describe the balance maintained in hydrostatic equilibrium.
  4. Discuss how energy produced in a star's core is transported to the surface.
  5. Describe the solar neutrino problem and possible solutions.
  6. Illustrate how parallax is used to measure the distances to our close neighboring stars.
  7. Define the different units used to designate the distances to stars.
  8. Describe how stars are seen to move in our sky and their actual motion through space.
  9. Define apparent magnitude and absolute magnitude and their relationship to a star's intrinsic luminosity.
  10. List and describe the main classes within the Harvard Spectral Sequence.
  11. Show how the H-R Diagram graphically demonstrates the relationship between important stellar parameters.