1. MMSA Earth-Space Science The Sun

2. Energy Output: 4 x 10 26 Watts If we could 1 second of this energy in its entirety, convert it to electricity and sold it at 5 cents / kilowatt, it would make $ 6 x 10 18. Energy generated by Nuclear Fusion at the Sun’s core.

3. The Core Very small. Only 1.5 % of the Sun’s total volume. Temperature: 15.6 million Kelvin Density: 150,000 kg / m 3. About 15 times more dense than Lead. High Density and Temperature are ideal conditions for nuclear fusion! Nuclear fusion: Hydrogen ions (H + ) come within 10 -15 m of each other to form Helium (He) atoms. All of the Sun’s energy is produced in this small region! Hydrogen atom

4. Radiation Zone Comprised of very dense gas. Energy transport to the surface is slow. The temperature of the sun decreases rapidly as you move out from the center. Atoms absorb energy from core. Energy emitted in the form of electromagnetic radiation from atom to atom.

5. Convection Zone -Hot atoms rise to surface, cool atoms fall close in. -Loops of gas form moving energy to sun’s surface

6. Outer Layers of Sun Photosphere: Inner layer of the Sun’s atmosphere. The part visible to us. Comprised of gas dense gas. Chromosphere: Thin region just above photosphere Visible only during total solar eclipses Corona: Outer most layer of sun. Extends far out into space.

7. The Core Very small. Only 1.5 % of the Sun’s total volume. Temperature: 15.6 million Kelvin Density: 150,000 kg / m 3. About 15 times more dense than Lead. High Density and Temperature are ideal conditions for nuclear fusion! Nuclear fusion: Hydrogen ions (H + ) come within 10 -15 m of each other to form Helium (He) atoms. High velocities are necessary for this. 1.) Draw two H ions. 2.) Why are high temperatures and high density necessary for nuclear fusion? Hydrogen atom

8. Class Work Read pgs 80 – 82. Define the following terms in your notes: Sunspots Prominences Solar flares Solar wind