Our Sun and Stellar Structure

Contents

• Introduction
• The Sun--An Average Star
  • Size
  • Composition
  • The Sun's Interior
    1. Core
    2. Radiative Zone
    3. Convective Zone
  • The Sun's Surface
    1. Measuring the Sun's Temperature
    2. Features on the Photosphere (sunspots, prominences, flares)
  • Solar Atmosphere
    1. Chromosphere
    2. Corona
    3. Review Questions
• The Sun's Power Source
  First a detailed explanation of why we think nuclear fusion is the energy source and then an outline.
  • Solar Luminosity---huge energy output!
  • Possible Sources of Energy
  • Gravitational Contraction Doesn't Power the Sun Long Enough
  • Nuclear Fusion Needs Extreme Temperatures and Densities
  • Some Mass is Converted to Energy in Fusion Reactions
  • Why Stars Use a Complicated Chain Reaction
  • Hydrostatic Equilibrium Controls the Reaction Rates
  • Summary
• Neutrino
  • Description
  • Solar Neutrino Problem
  • Explorations of Neutrino Detectors
• Helioseismology
  • Links to Centers Probing the Sun's Interior
  • Review Questions
• Interior Structure of Stars
  • Mathematical Models
    1. Temperature
    2. Pressure
    3. Mass Density
  • Equation of State The ideal gas law relates temperature, pressure, and density.
  • Gravity Holds a Star Together Hydrostatic Equilibrium
  • Other Pieces
    1. Continuity of Mass -- conservation of mass
    2. Continuity of Energy -- conservation of energy
    3. Energy Transport: radiation, convection, conduction
    4. Opacity: how well the gas absorbs light
  • Mass-Luminosity Relation Explained
  • Mass Cutoff Explained
  • Review Questions