2. What are atoms? Describe them. Smallest constituents of elements. Contain positive, negative, neutral particles.

3. Rutherford Model All the protons were gathered at the center – a heavy dense positive nucleus, with the electrons scattered around outside.

4. An  particle is a helium nucleus: 2 p+, 2n o.

5. Most  particles went straight through, but the ones that passed closest the Au nucleus were progressively more deflected.

6. The fact that most alpha particles pass straight through the foil suggests: 1. The nucleus is positive 2. The nucleus is negative 3. The atom is mostly empty space. 4. The particles have lots of energy.

7. The fact that some alpha particles were deflected by the foils suggested to Rutherford that: 1. The nucleus is positive 2. The nucleus is negative 3. The atom is mostly empty 4. The particles have lots of energy.

8. Conclusions - Gold foil experiment : atom is mostly empty space dense positively charged nucleus. Electrons move in orbits about the nucleus.

9. Accelerated charges radiate EM energy. Circular motion is acceleration. The e- should lose energy & spiral into the nucleus. That does not happen! Also, how did the positive nucleus stay together? Should repel. Flaws:

10. Bohr Model There are several allowed orbits that an e- can occupy. The orbits are at varying distances from the nucleus. Closest orbit n=1, the ground state. E=0 for e-

11. Bohr Orbits further from the nucleus require the e- to absorb exact amount of E to occupy. If e- in higher orbit, atom said to be excited.

12. Atoms need to absorb E to excite e- to higher orbits. Like climbing a ladder. When e- drops to lower orbit atom gives off E.

13. Evidence for Bohr Mode from Light Spectra Emission -e- emits specific photon E. Absorption- e- absorbs specific photon E.

14. Electric E supplied to gas tubes causes gases to emit light.

15. Emission Spectrum When viewed through a prism or spectroscope, we see only certain of light are emitted by each element. Bright Line Spectra

16. Absorption Continuous spectrum From sunlight

17. Absorption Spectrum When light is passed through cool gasses, each gas absorbs only certain ’s of light. When viewed through a prism, the same ’s that are emitted by each element, are absorbed by each element.

18. Frequencies emitted exactly match the frequencies absorbed.

19. Review How does Rutherford view the atom? How does Bohr view the atom?

20. Rutherford Atom has dense + nucleus Tiny, low mass negative e- orbit in shells. Atom mostly empty space. Evidence: most +alpha particles passing straight through gold foil. Some deflected or repelled straight back.

21. Bohr : Each atomic orbit is associated with a specific E level for e-. It is quantized. Innermost orbit is “ground state” When atom absorbs photon energy e- “jump” to higher E outer orbits. Atom is “excited”. Atom emits photons when e- “fall” to lower inner E orbits. No in between orbits possible, photons absorbed/emitted comes in discrete E amounts.

22. Bohr Model The emission & absorption spectra caused by e- emitting or absorbing photons as they change orbits.

23. How stuff works. How is light produced? 2:15 http://www.youtube.com/watch?v=GCvjo3e m7EQhttp://www.youtube.com/watch?v=GCvjo3e m7EQ

24. The frequencies/colors of the spectral lines correspond to the exact energies (E=hf) that e- emit as they move between atomic orbits.

25. Film: Quantum Mechanics & Atomic Structure 6:20 minutes http://www.youtube.com/watch?v=- YYBCNQnYNM Hwk Concepts: Rd Tx 840 – 847 Do pg 847 #2 – 6 Full Sentences & Mult Choice sheet.

26. Bohr Energy Diagrams

27. Orbital Energy Levels/ Ionization Energy Each orbit is associated with a specific energy which corresponds to the minimum energy needed to totally strip an e- from that orbit. This ionization energy > E needed to jump between orbits. If an atom absorbs E = to the orbit energy it becomes ionized (charged). Orbits are named by quantum number.

28. Ionization Energy: e- stripped from atom if photon with sufficient energy absorbed.

29. When e- is in lower/closer orbits to nucleus. It takes more E to ionize/strip it out of atom.

31. Ex 1: How much energy would be needed to ionize (completely strip) an electron: In the n=1 level of of Hydrogen? in the n = b or level of Mercury? In the n = 2 level of Hydrogen?

32. For e- to jump to higher orbits it must absorb exact  E between orbits.

33. The photon energy absorbed & emitted during transitions between e- orbits:

34. Use diagrams to find  E. E photon = E i - E f Use E pho = hf of the radiation to find frequency associated with photon of known energy.

35. Ex 2: a) How much E is absorbed when a Hydrogen e- jumps directly from the n=1 to n=3 orbit? b) How much E is released when the Hydrogen e- drops from n=3 to n=1? c) When the e- drops back down to the n=1 from n=3 orbit, what f photon is emitted? d) To which type of radiation does that photon correspond? e) How many different photons are possible to be emitted by electron dropping from the n=3 to n=1 level?

36. n =3 to n = 1 E photon = E initial - E final. -13.6 eV - (-1.51 eV)= - 12.1 eV (12.1 eV)(1.6 x 10 -19 J/eV) = 1.936 x 10 -18 J. E = hf.f = E/h f = 1.936 x 10 -18 J/(6.63 x 10 -34 Js) f = 2.92 x 10 15 Hz. Look up.

37. Ex 3: A Mercury Atom has an e- excited from the n=a to the n=e energy level. What is the frequency it will absorb? To which radiation does the frequency correspond? If the e- drops down from the e to the b level, what type of radiation will it emit. 1.61 x 10 15 Hz UV Orange

38. Read Rev Book pg 333 – 334 do pg 334 “try it 1-3” & 338 #17 -19, 22-23, 26-27, & 30, 32 – 34 Write out equations, calculations with units on separate sheet for credit. Hwk check.

39. Film: Quantum Mechanics & Atomic Structure 6:20 http://www.youtube.com/watch?v=- YYBCNQnYNM&annotation_id=annotatio n_990931&feature=iv

40. Equivalence of Mass & Energy

41. Einstein: “EM E, acts like tiny bit of matter, at the smallest scale matter/energy same thing”. E stored in the nucleus of mass obeys Einstein’s equation: E = in J. E = mc 2. m = mass kg c = 3 x 10 8 m/s E can be released when nucleus is transformed.

42. Ex 1: How much energy is produced when 2.5 kg of matter are completely converted to energy? How much energy is that in eV?

43. E = mc 2. =(2.5 kg )(3x10 8 m/s) 2. = 2.25 x 10 17 J in eV (2.25 x 10 17 J)(1 eV / 1.6 x 10 –19 J) = 1.4 x 10 36 eV.

44. Compare that with eV generated by glowing gasses.

45. What is the graph of E vs. m? E m What is the slope?

46. Atomic Mass Units: amu or u Mass of atoms very small so they are measured in amu or u rather than kg. Analogous to J and eV. Since mass is equivalent to energy, 1 u = 931 MeV or 931 x 10 6 eV 931 MeV

47. Ex 2: Calcium has an average mass of 40 u. How much energy in Joules is stored in the nucleus of each atom of Calcium? 40 u x 931 MeV = 37, 240 MeV. u (37, 240 x 10 6 eV) x 1.6 x 10 -19 J = 6 x 10 -9 J. eV.

48. Ex 3: Calculate the mass in kg of one universal mass unit.

49. Convert MeV to Joules. (1 u) x (931 x 10 6 eV/u) x (1.6 x 10 –19 J / eV) = 1.49 x 10 -10 J E = mc 2 so m = E/c 2. (1.49 x 10 10 J) / (3x10 8 m/s) 2 = 1.66 x 10 –27 kg

50. 1 mass unit is close to the mass of a proton or 1 H. (A single hydrogen nucleus)

51. The Atomic Bomb Some of the mass of U is converted to E. The total mass after the reaction is less than the initial mass. Should be “Law of conservation of mass/energy”

52. Summary: EM energy can be thought of as tiny particles (photons) related to f. Matter can be thought of as E stored in nucleus. E in matter E = mc 2. Joules. 1 u = 931 MeV. E in EM radiation/photons E = hf. E measured in eV and J. 1 eV = 1.6 x 10 -19 J.

53. 4. An e- and an anti-electron have the same mass. When they meet they completely annihilate each other. Look up the mass and calculate the energy released from the destruction in joules. E = mc 2. = 2(9.11 x 10 -31 kg)(9 x 10 16 m 2 /s 2 ) =1.64 x 10 -13 J.

54. 5: A Helium nucleus consists of 2 protons & 2 neutrons. How much energy in MeV would be released if it were completely converted? Each nucleon is 1 unit u. 1 u = 931 MeV. 4 x 9.31 x 10 2 MeV/ nucleon. 3724 MeV.

55. Hwk: Pkt Mod Phys Prac 3

56. http://www.youtube.com/watch? v=lPSxIuQLQVI&feature=relate d http://www.youtube.com/watch?v=KWGLS 7Ck1qs&feature=relatedhttp://www.youtube.com/watch?v=KWGLS 7Ck1qs&feature=related Einstein’s Big Idea 51 min historical view. http://www.youtube.com/watch?v=jqiRoKy0Gyo&feature=related

57. Standard Model http://www.particleadventure.org/stan dard-model.html

58. Standard Model: Matter is composed of small subatomic particles called quarks & leptons. Forces also have particles that transfer information through tiny particles. See review book xerox.

59. Quarks compose neutrons & protons.

60. Diagrams Examples

64. Bohr’s model could not explain why e- could occupy only certain orbits. DeBroglie’s hypothesis for the wave nature of matter helped explain how only certain orbits were allowed. Each e- has = h/mv. DeBroglie proposed that each e- is a standing wave.

65. Proposed e- standing waves. Only ’s that fit certain orbits are possible.

66. ’s that don’t fit circumference cannot exist.

67. Heisenberg’s uncertainty principle 1927. It is impossible to be make simultaneous measurements of a particle’s position and momentum with infinite accuracy. When you try to look to see where an e- actually is, you must give it energy. If you give it energy, it moves.

68. Alpha Rays A rays are helium nuclei, (2p + and 2n o ), that are emitted from nucleus. They can be easily stopped by skin or thin sheet of paper. More likely to knock e- from orbits because they lose all their KE at once. Charge = +2e Mass 4 units Energy is KE = ½ mv 2.

69. Beta Rays More penetrating than alpha. Less capable of ionizing because their energy is lost over greater distance. They are fast moving e-. Charge = -e. mass = e. KE = ½ mv 2. v can be sig portion of c. Need a few mm of Al to stop them.

70. Gamma Penetrating power greatest. Can pass thru human body, concrete, and lead. Lowest ionizing power. They are EM waves. No charge. No mass. Energy described by E = hf. Travel with vel of light in vacuum. No maximum stopping range.

71. How could we distinguish the different types of radiation? What could we observe?

76. Hwk rd 450 –462 Core only Do quest pg 451 1-5 p 457 1-4 p 458 1-3 p 462