1. 1

2. 2 Phys 181-701 Astronomy

3. 3 May the warp be the white light of morning, May the weft be the red light of evening, May the fringes be the falling of the rain, May the border be the standing rainbow. Thus weave for us a garment of brightness. Song of the Sky Loom (Native American Traditional) Garment of Brightness

4. 4 Intro The Interaction of Matter and Electromagnetic Radiation (Light) Understanding This is an Important Tool of Astronomy Light Interacts with matter in several ways… Reflection Refraction Diffraction Absorption Emission Gravitation!

5. 5 Review Light is a form of Electromagnetic Radiation Radiation may be described as waves Waves are described by their frequency, wavelength, amplitude and speed.

6. 6 Time period of mars

7. 7 Reflection Reflection Nebulae Reflection Light simply scatters off the dust and gas…

8. 8 Refraction Light bends when moving from one substance to another…

9. 9 Diffraction Light bends around obstacles… DiffractionDiffraction

10. 10 Absorption&Emission Absorption and Emission

11. 11 ObservationsObservations

12. 12 Thermal RadiationThermal Radiation Thermal (Blackbody) Radiation Spectra 273 Kelvin = 0 ºC

13. 13 1.Stefan-Boltzmann Law: Hotter objects emit more power per unit area. 2.Wien’s Law: Hotter objects emit light that has a higher average energy. Two Law s Two Laws of Thermal Radiation:

14. 14 Practical Example Change in Brightness Change in Color

15. 15 Calculation ExampleCalculation Example Example: Consider a perfect thermal emitter with a temperature of 15000 K. How much power does it emit per unit area? What is the wavelength of maximum intensity?

16. 16 Putti ng it Toge ther Putting it Together…

17. 17 AnalysisAnalysis

18. 18 DopplerShiftDopplerShift

19. 19 Shifted SpectraShifted Spectra

20. 20 Doppler Effect Formula: Doppler FormulaDoppler Formula

21. 21 Why does the sun shine? Chemical Burning – insufficient radiation Radiative Cooling – only thousands of years Gravitational Contraction – only 25 million years Why does the sun shine?Why does the sun shine?

22. 22 Stars convert energy into matter. E=mc^2E=mc^2

23. 23 600 million tons of H -> 598 million tons of He IN ONE SECOND Proton-Proton ChainProton-Proton Chain

24. 24 Basic Solar Structure

25. 25 The force of gravity inward and the radiation pressure outward balance each other out. Gravitational Equilibrium Radiation PressureRadiation Pressure

26. 26 91.2% Hydrogen – 8.7% Helium 0.1% Heavier Elements Spectroscopy Visible Spectrum Sp ect ros co py

27. 27 LuminosityLuminosity Luminosity The total power output of the sun: 3.8x10 24 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.

28. 28 Sun SpotsSun 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.

29. 29 GranularityGranularity Granularity of the Solar Surface

30. 30 ConvectionConvection

31. 31 A Solar Prominence ProminenceProminence

32. 32 Solar Flare FlareFlare

33. 33 Understanding the sun: simulationssimulations

34. 34 IMPORTANT Light Interacts with Matter Spectrum ( Energy - Temp - Color ) E and A Spectra Radiation Laws Doppler Shift Gravitational Equilibrium

35. 35 Next Time…… STARS, A Mass of A Mass of Incandescent Gas ENDEND