The Sun, our favorite star!

1. The Sun, our favorite star! WE CAN SEE IT REALLY WELL. The Sun is the basis for all of our knowledge of stars. Why?

2. Today we will take a journey to the center of the Sun, starting with what we can see… …and ending up deep in the core.

3. Overview of Solar Structure The Sun is made of mostly HYDROGEN and HELIUM Main Parts:

4. Mass is ejected into space as the solar wind The Corona • Outer layer of the Sun • Millions of degrees but very diffuse • Extends millions of kilometers into space • Hot and energetic, gives off lots of x rays!

5. The Sun has intense magnetic fields • The magnetic fields release energy from the Sun • Release seen in sunspots, flares, coronal mass ejections & other phenomena

6. In detail…

7. Flares This twisting leads to the loopy structures we see!

8. BE AMAZED! Earth to scale. Yes, really.

9. The Sun’s magnetic fields create sunspots The Sun has an 11-year solar cycle Minimum Maximum

10. Visible Sunspots! Ultraviolet 284 nm Ultraviolet -174 nm Ultraviolet - 304 nm Ultraviolet 195 nm

11. temperature is about 5800 K… • Remember how the temperature and color of stars are related? The temperature of our Sun gives it its yellowish color! Our Sun is really yellowish green, but our atmosphere absorbs and scatters some of the blue light.

12. Where is all this energy made? In the core. Why and how? The core is so hot and has such high pressure that FUSION can take place Why are the central pressures so high ????

13. Gravity pulls the surface of the Sun in compresing inner layers and heating them up, but the Sun doesn’t collapse… What is pushing back??? Pressure The pressure of the HOT gas layers below. This applies to all layers of the Sun. Gravity pulls outer layers in, Gas Pressure pushes them out. It is pretty hot at the center!!!!

14. Why does high pressure in the core lead to Fusion? High Temperature and Density allows nuclei to interact! Nuclei can FUSE together: “Nuclear Fusion”

15. p p p n n p p p Energy Production in Stars:The short version. + Energy 4H 1He 4 Hydrogen Atoms fuse to make 1 Helium Atom and a bunch of energy.

16. How does fusion generate energy? The Sun is made mostly of HYDROGEN and HELIUM 4 protons in H are slightly heavier than the 2 protons + 2 neutrons in He Some mass converts to energy!

17. Sunshine = Energy from Fusion E = mc2 Energy Mass Speed of Light Speed of light is BIG-- so a little mass can turn into a LOT of energy!

18. How many students does it take to power a lightbulb? Wanna know what you’re worth, energy-wise? It’s pretty easy to figure out! Take an average student, of about 70kg. E = mc2 So if we turn this whole student from mass into energy in a single second, we get: E = 6.3 x 1018 J If a typical lightbulb is 60 Watts,the energy from a student could keep it lit for… 200 BILLION YEARS! By comparison, the Sun shines with a luminosity of 1026 Watts. (that’s a lot of lightbulbs)

19. review: • Gravity compresses and heats the center of the sun • At the core nuclear reactions take place • The Sun is a giant nuclear reactor • Energy flows from the core outward, but how • does it get out and end up as sunshine? The next two layers of the Sun are all about getting the energy being made in the core out into space! It takes a lot of time, but we get it eventually.

20. How does energy get from one place to another? 1. Convection 2. Conduction 3. Radiation Convection and Radiation are most important for the Sun!

21. Convection Hot stuff rises… Cool stuff sinks! BOILING Conduction Metal of the pan heats by conduction… …heat travels through the atoms of the pan Not very important for stars! Radiation • Photons can “scatter” off of unbound electrons • When they scatter, the photons share their energy with the electrons • The electrons get hotter Ionized gas

22. How do we connect what we see to the Sun’s structure? Sun’s Spectrum has ABSORPTION LINES

23. Hot source makes a continuous thermal spectrum Light passing through a cloud of cooler gas gets some light absorbed out: ABSORPTION SPECTRUM

24. So how does this apply to the Sun? • Outer layers of the Sun are cooler than interior • Interior opaque part of Sun produces a thermal spectrum, while cooler outer layers produce absorption lines!

25. Really high resolution spectrum of the Sun: lots of absorption lines!

26. Compare Burning with Fusion • 1 gallon of gas powers my beautiful red Solara for about 25 miles • 1 gallon of hydrogen fusion would power my solara for 140 million miles and farther • All the way to the Sun!

27. How Much Fusion a Second? • Einstein’s formula • E = m c2 • The luminosity of the Sun is • 4 x 1026 Watts • So … The Sun loses 4 million tons of mass per second!

28. The Sun Takes About 4 Weeks to Rotate

29. What is the sun made of? • We know diameter & mass • Density = mass / volume • Density = 1.4 times water! • Low density + • Hot temperature The Sun is a ball of gas! • Determined from study of spectrum and atomic spectra in the laboratory • 74% Hydrogen • 25% Helium • 1% All other elements

30. Particles emitted by the sun detected on the Earth confirm picture of the Sun given in this power point. Good night.