1. Stars Physics 360 - Astrophysics

3. Brightness Different brightness. Different color. How bright are they really? What is due to distance? What is due to luminosity?

4. Spectral Classification

5. 0.005 arcsec Mass

6. Stellar Radii How big are stars? Stars have different sizes. If you know: –Distance –Angular size Learn real size. 50 mas

7. Sizes of Stars Supergiants, Giants and Dwarfs

8. The Sun, Our Star The Sun is an average star. From the Sun, we base our understanding of all stars in the Universe. No solid surface.

9. Vital Statistics Radius = 100 x Earth (696,000 km) Mass = 300,000 x Earth (1.99 x 10 30 kg) Surface temp = 5,800 K Core temp = 15,000,000 K Luminosity = 4 x 10 26 Watts Solar “Day” = –24.9 Earth days (equator) –29.8 Earth days (poles)

10. Interior Properties Core = 20 x density of iron Surface = 10,000 x less dense than air Average density = Jupiter Core = 15,000,000 K Surface = 5800 K

11. 1. The Core Scientific Method: –Observations –Make hypothesis (a model) Models make predictions –Test predictions Compare results of predictions with observations –Revise model if necessary.

12. Testing the Core Observe Sun’s: –Mass (how?) –Composition (how?) –Radius Use physics to make a model Sun. Predict: –Surface temp/density (how do you test?) –Surface Luminosity (how do you test?) –Core temp/density  Fusion Rate  neutrino rate (test?)

13. In The Core Density = 20 x density of Iron Temperature = 15,000,000 K Hydrogen atoms fuse together. Create Helium atoms.

14. Nuclear Fusion 4H  He The mass of 4 H nuclei (4 protons): 4 x (1.6726 x10 -27 kg) = 6.690 x 10 -27 kg The mass of He nuclei: = 6.643 x 10 -27 kg Where does the extra 4.7 x 10 -29 kg go? ENERGY!  E = mc  E = (4.7 x 10 -29 kg ) x (3.0 x 10 8 m/s) 2 E = hc/  = 4.6 x 10 -14 m (gamma rays) So: 4H  He + light

15. 2. Helioseismology Continuous monitoring of Sun. –Ground based observatories –One spacecraft (SOHO) Surface of the Sun is ‘ringing’ Sound waves cross the the solar interior and reflect off of the surface (photosphere).

16. Solar Interior Core –Only place with fusion Radiation Zone –Transparent Convections Zone –Boiling hot

17. Convection A pot of boiling water: Hot material rises. Cooler material sinks. The energy from the pot’s hot bottom is physically carried by the convection cells in the water to the surface. Same for the Sun.

18. Solar Cross-Section Progressively smaller convection cells carry the energy towards surface. See tops of these cells as granules.

19. The Photosphere This is the origin of the 5,800 K thermal radiation we see. = k/T = k/(5800 K)  =480 nm (visible light) This is the light we see. That’s why we see this as the surface.

20. 3. Solar Activity and Earth Is there a connection between Solar Activity and Earth’s Climate? Observation: –Little Ice Age –Maunder Minimum

21. What is Solar Activity? Sunspots Magnetic Fields Coronal Mass Ejections Solar Wind Magnetic Storms Aurora Other effects?

22. What is Solar Activity? Sunspots Magnetic Fields Coronal Mass Ejections Solar Wind Magnetic Storms Aurora Other effects?

23. Sunspots 11-year sunspot cycle. Center – Umbra: 4500 K Edge – Penumbra: 5500 K Photosphere: 5800 K

24. Magnetic fields and Sunspots At kinks, disruption in convection cells. Sunspots form.

25. Magnetic fields and Sunspots Where magnetic fields “pop out” of Sun, form sunspots. Sunspots come in pairs.

26. Prominences Hot low density gas = emission lines

28. Corona and Solar Wind Hot, low density, gas emits the radiation we see as the Corona: 1,000,000 K Solar Wind: Like steam above our boiling pot of water, the gas ‘evaporates’. Carries away a million tons of Sun’s mass each second! Only 0.1% of total Sun’s mass in last 4.6 billion years.

30. Solar Cycle Increase in solar wind activity - Coronal Mass Ejections Increase in Auroral displays on Earth Increase in disruptions on and around Earth. Courtesy of SOHO/LASCO/EIT consortium.