1. Quiz 1 Each quiz sheet has a different 5-digit symmetric number which must be filled in (as shown on the transparency, but NOT the same one!!!!!) Please hand in both the exam and the answer sheets with your name on both Question/answer sheets will be handed back on Wednesday after class Please remain seated until we begin collecting (20-25 minutes after start) Class after quiz

3. Why is the sky blue ? The atmosphere scatters the blue light more than red light

4. Light and Matter Light is electromagnetic energy, due to interaction of electrical charges Matter is made of atoms – equal number of positive and negative particles An atom is the smallest particle of an element; natural element H to U Atom  Nucleus (protons + neutrons), with ‘orbiting’ electrons No. of protons in nucleus = Atomic Number Science of light  Spectroscopy

5. Radiation and Spectroscopy Light is electromagnetic energy Propagates as both particles and waves Photons – particles of light Wavelength = Velocity / Frequency

6. Light is electromagnetic wave; Does not require a medium to propagate, unlike water or sound Wavelength is the distance between successive crests or troughs

7. Wavelength ( ) Speed (c) Frequency (f) (# waves/second) Speed = wavelength x frequency  c =  f Frequency ‘f’ is the number of waves passing a point per second WAVES: Frequency, Wavelength, Speed

8. Units of wavelength and frequency Frequency is the number of cycles per second Since speed of light is constant, higher the frequency the shorter the wavelength and vice- versa Wavelengths are measured in Angstroms: 1A = 1/100,000,000 cm = 1/10 nanometer (nm) The higher the frequency the more energetic the wave Wavelength (or frequency) defines radiation or color

9. Spectrum Prism White Light Prisms disperse light into its component colors: Red-Violet

10. Visible Light Forms a narrow band within the electromagnetic spectrum ranging from gamma rays to radio waves Human eye is most sensitive to which color? Yellow. Why?

11. Light: Electromagnetic Spectrum From Gamma Rays to Radio Waves Gamma rays are the most energetic (highest frequency, shortest wavelength), Radio waves are the least energetic. Gamma X-Ray UV Visible

12. Decreasing Wavelength OR Increasing Frequency

13. Visible light spectrum: Each color is defined by its wavelength, frequency or energy Red - Blue  7000 - 4000 Angstroms ( 1 nm = 10 A, 1 A = 10 -8 cm) Blue light is more energetic than red light Light also behaves like ‘particles’ called photons Photon energy, frequency, wavelength: E = h f = hc/ Planck’s Law (‘h’ is a number known as Planck’s constant)

14. Matter and Particles of Light: Quantum Theory Light (energy) and matter in motion behave both as waves and particles Wave-Particle Duality - Quantum Theory Particles of light are called photons: E = hf = hc/ Photons of a specific wavelength may be absorbed or emitted by atoms in matter Matter is made of different natural elements: lightest Hydrogen (1 proton), heaviest Uranium (92 protons) Smallest particle of an element is atom, made up of a nucleus (protons and neutrons), and orbiting electrons Electrons and protons attract as opposite electrical charges, NOT gravitationally like planets and Sun

16. The Hydrogen Atom Electron orbits Discrete energies

17. Absorption of light (energy) photon by H-atom

18. Emission of light photon by H-atom photon energy  color

21. Series of spectral lines of Hydrogen

22. Wavelengths of series of lines from Hydrogen

23. SPECTRAL SIGNATURE OF ELEMENTS

24. Continuous, Absorption, and Emission Spectra

25. Brightness and Temperature Brightness is related to the total energy emitted, or the luminosity of an object The energy emitted is related to the temperature of the object B =  T 4  is a constant) Stefan-Boltzmann Law

26. Color Indicates Temperature and Energy of the Source Objects generally emit radiation at all wavelengths, but mostly at one peak Wavelength depending on their temperature (e.g. blue – hot, red – cool) Surface T (Sun) = 5600 K “ (Mercury) = 800 K Blackbody: Perfect absorber and emitter Of radiation at a given Temperature T

27. TEMPERATURE SCALES Room Temp = 300 K = 27 C = 81 F Astronomers usually use the Kelvin Scale K = C + 273 C = (F - 32) x 5/9 ~ (F - 30) / 2 F = (C x 9/5) + 32 ~ C x 2 + 30

28. The Doppler Effect Why does the “pitch” of a police siren differ when, say, a police car is approaching you, or when you are running away from the police (not recommended) ? The frequency (the number of sound waves per second) is higher when approaching, and smaller when receding from the source

29. Doppler Effect in Sound High Pitch (short waves) Low Pitch (long waves)

30. d=1 d=2 d=3 B=1 B=1/9 B=1/4 Brightness decreases inversely as the square of the distance

31. The Doppler Effect Velocity c = frequency (f) x wavelength ( 

32. Doppler Shift of Wavelengths What about the wavelength? What about light? Shorter wavelength  Blue-shift, Longer wavelength  Red-shift We can determine the velocity of astronomical objects, moving away or towards the Earth, by measuring the wavelength of light from the object Observed red-shift of galaxies all over the sky shows that galaxies are moving away from one another  the Universe is expanding (Hubble’s Law)

33. Hubble Diagram: Distribution of Galaxies

34. Hubble’s Law: v = H o d Velocity increases with distance

35. Expanding Universe Hubble’s law  Universe is expanding Universe had a beginning ! How long ago? Age of the universe: 1/H o (units of time) Big Bang !! How does one determine distances? Redshift

36. Cosmic Microwave Background (CMB): Universal and Uniform Radiation

37. CMB Properties The entire universe is filled with extremely uniform radiation CMB radiation corresponds to a fixed temperature of 2.73 K (-270.3 o C or -428.9 o F) Blackbody: uniform temperature oven CMB radiation is also isotropic  same in all directions But with extremely slight variations immediately following the Big Bang due to matter

38. Distribution of Matter in Galaxy Stars rotate about the center of galaxy Velocity determined by gravity: mass M c and distance R c from the center KE = PE ½ m star v 2 = G M c m star / R c Velocity v should decrease with radius R c Surprise !

39. Evidence of Dark Matter: Rotation Curves of Galaxies

40. Dark Matter Halo Rotation curves are flat out to distances beyond observable galaxies Ergo: Galaxies have “dark matter” haloes What is dark matter?