1. Astronomy Picture of the Day

2. The Sun Core temperature - 15 million K Surface temperature - 6000 K 99.9% of all of the matter in the solar system Entirely gaseous Supplies the energy essential for life on Earth All normal matter was created inside a star similar to the sun!

3. The Sun The Sun in X-rays over several years The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 330,000 M Earth Radius of Sun = 109 R Earth Luminosity of Sun = 4 x 10 26 Watts (Equivalent to 100 billion 1-megaton explosions every second!)‏ Why doesn't the sun blow itself apart?

4. Hydrostatic Equilibrium Internal heat and pressure directed outward Gravity pulling mass inward Two forces balance When all hydrogen transformed to helium, Sun will begin to collapse

5. Let's start with the core, where the Sun's energy is generated. The Interior Structure of the Sun Core - nuclear fusion Radiation zone - completely ionized => no photon absorption Convection zone - less ionization => photon absorption Photosphere - radiation, the part of the sun that we see How do we get this info?

6. What Powers the Sun? Nuclear Fusion: An event where the nuclei of two atoms join together. Need high temperatures. Why? To overcome electric repulsion. Energy is produced. (A small amount of mass = a lot of energy)‏ E = mc 2. Sum of mass and energy always conserved in reactions. Mass is just “frozen” energy.

7. Why High Temperatures? To overcome electric repulsion High temp => fast atomic motion (Molecular Motion Demo)‏ Nuclear forces - very short range (10 -15 m)‏ 100 times EM force 10 39 times gravity (“Fusion” Demo)‏

8. How does energy get from core to surface? core "radiation zone": photons slowly drift outwards "convection zone" "surface" or photosphere: photons escape into space. photon path

9. Sunspots (evidence for 11 year cycle)‏ Roughly Earth-sized Last ~2 months Usually in pairs Follow motion of sunspots => can determine rotation rate (Sunspot Demo) ‏

10. Magnetic Fields Rotating Earth generates a magnetic field - Like bar magnet aligned with Earth’s axis Influences paths of electrically charged particles

11. Aurorae Charged particles from solar wind spiral towards poles Collide with and excite atmospheric molecules Emission spectra!

12. The Sun's Rotation The Sun exhibits Differential Rotation just like the Jovian planets. ~25-36 days What is this? (animation)‏ What might this mean for the magnetic field of the Sun?

13. Sun’s Magnetic Field Rotating sun also generates a magnetic field Differential rotation => magnetic field distortion Loops extending beyond photosphere can form

14. Sunspots They are darker because they are cooler (4500 K vs. 5800 K). Related to loops in the Sun's magnetic field. radiation from hot gas flowing along magnetic field loop of Sun.

15. Solar Flares Violent ejection of large amount of particles from Sun surface. (animation) ‏

16. Above the photosphere, there is the chromosphere, transition zone, and... The Corona Best viewed during eclipses. Solar wind => Evaporation 1 million tons/s lost. But Sun has lost only 0.1% of its mass from solar wind in its 4.6 billion year lifetime.

17. Apparent Brightness vs. Luminosity Luminosity – Intrinsic power output Apparent Brightness – Perceived intensity when viewed from some distance Does an object emitting light appear brighter or dimmer as it moves away from you?

18. Apparent Brightness and Distance Calculate luminosity, measure apparent brightness => figure out distance!