Phys 181

1. Phys 181 Astronomy This Lecture Brought to You in Comic Sans MS

2. “With equal passion I have sought knowledge. I have wished to understand the hearts of [people]. I have wished to know why the stars shine.” -Bertrand Russell "One of the most impressive discoveries was the origin of the energy of the stars. One of the men who discovered this was out with his girl friend the night after he realized that nuclear reactions must be going on in the stars in order to make them shine.She said "Look at how pretty the stars shine!"He said, "Yes, and right now I am the only man in the world who knows why they shine."She merely laughed at him. Well, it is sad to be alone, but that is the way it is in this world.“- Richard Feynman, "The Feynman Lectures“ “A star shines on the hour of our meeting.”- Elvish greeting, "The Lord of the Rings“ “I wonder why. I wonder why. I wonder why I wonder. I wonder why I wonder why I wonder.”- Richard Feynman Quotes

3. Readings Readings: ASTRONOMY TODAY Chapter 16 (excepting section 16.6) Chapter 17 (without exception)

4. General Solar Properties Solar Properties SolarProperties

5. Why does the sun shine? • Why does the sun shine? • Chemical Burning – insufficient radiation • Radiative Cooling – only thousands of years • Gravitational Contraction – only 25 million years

6. E=mc^2 Stars convert energy into matter.

7. Proton-Proton Chain 600 million tons of H -> 598 million tons of He IN ONE SECOND

8. Basic Solar Structure

9. Radiation Pressure The force of gravity inward and the radiation pressure outward balance each other out. Gravitational Equilibrium

10. Spectroscopy Spectroscopy Visible Spectrum 91.2% Hydrogen – 8.7% Helium 0.1% Heavier Elements

11. Luminosity Luminosity The total power output of the sun: 3.8x1024 watts!!! Think of your 60 watt light bulb. 1 second of the earth luminosity contains enough energy to meet our needs for roughly 500,000 years! Only about one two-billionth of that reaches Earth.

12. Sun Spots Sun Spots Not at all dark Roughly the size of the earth Show the differences in rotation: 27 days equator – 31 days poles Only about one two-billionth of that reaches Earth.

13. Granularity Granularity of the Solar Surface

14. Convection

15. Prominence A SolarProminence

16. Flare Solar Flare

17. simulations Understanding the sun:

18. End NEXT TIME: Measuring the Stars

19. “Perhaps the greatest anomaly in this situation is the incredibly weak scientific case for the whole scenario of cosmic evolution. There can be no "experiments" or "observations" of stars evolving, in the very nature of the case, so it cannot be scientific, though it may be naturalistic - all based on mathematical manipulations, computer simulations, and atheistic or pantheistic philosophies.” -Henry Morris in Creation by Inflation and Quantum FluctuationBack to Genesis 129a, August 1999. Quotes • “I believe that a scientist looking at nonscientific problems is just as dumb as the next guy.” • -Richard Feynman, 1968 “I believe that a theologist looking at nontheological problems is the next guy” -Professor Scheidly, Just Now

20. Readings Readings: ASTRONOMY TODAY Chapter 17, 20, and 21

21. General Solar Properties Nearest Neighbors

22. Proxima Proxima Centauri

23. Stellar Parallax Proxima Centauri: Stellar parallax = 0.76” Distance = 1/0.76 = 1.3 pc Distance = 270,000 AU Distance = 4.3 ly

24. Proper motions Proper Motions of Stars…

25. Apparent Brightness Apparent Brightness  Luminous Intensity/Distance2

26. Apparent Magnitude A change in apparent magnitude by 5 corresponds to an increase in apparent brightness by a factor of 100. The log scale allows us to express large differences in a compact way.

27. Spectral Classification

28. Characteristics

29. Stellar Radii Estimating Stellar Radii…

30. HR Hertzsprung-Russell Diagram…

31. HR

32. HR

33. HR M55

36. Move foreward