Major Theme: The Sun is our local stellar laboratory
Learning Objectives
- Describe the balance between the forces that determine the structure of the Sun.
- Explain how mass is converted into energy in the Sun’s core and how long it will take the Sun to use up its fuel.
- Sketch a physical model of the Sun’s interior, and list the different ways that energy moves outward from the Sun’s core toward its surface.
- Describe the solar activity cycles of 11 and 22 years, and explain how these cycles are related to the Sun’s changing magnetic field.
Outline
Solar structure:
- Interior
- Atmosphere: Photosphere, chromosphere, corona, solar wind
Energy formation within the sun:
- Hydrostatic equilibrium: balance of gas / radiation pressure and gravity.
- Ideal gas law
- Nuclear fusion proton: proton – proton reaction
- Energy transport from the solar core to the exterior.
Active solar phenomena: the effects of strong magnetic fields
- sun spots, prominence, flares, CMEs
- The effects of solar storms on Earth
Activities:
- Read charter 14
- Unit Notes Folder
- Phet: The Sun’s Photosphere and magnetism
- Lab 4: (use Internet Explorer for all links)
- Structure of the Sun: Interior and Atmosphere
- Solar Rotation using differential rotation(If the Quick time file doesn’t load, then use the SpaceWeather archives for 2013)
- Solar Rotation (another approximation)
- Sunspot cycles data
- Research on the Sun and sunspots
- Viewing Sunspots: use the Space Weather Center images.
Online Resources:
- Visit the Space Weather website.
- Read the Many Faces of the Sun
- Nuclear Fusion: the source of engine for the sun.
