1. From the Big Bang to Planets a brief history of the Universe Background material – Chapter 1 in text Things I expect you to know, but will not be tested on Intro to some useful physics – Chapters 4 & 5 Things you will be tested on

2. The Hot Big Bang Theory The Universe started from a very hot, dense state around 14 billion years ago and is expanding and cooling down with time.

3. How do we know? 1.Hubble’s law – distant galaxies are all moving away from us, the farther away they are, the faster they are moving 2.The Cosmic microwave background radiation – things that are hot emit light and the universe today is filled with this light emitted when it was much hotter

4. Hubble’s Law Raison bread analogy As dough expands all raisons move away from all other raisons

5. Cosmological Redshift Light, which is an electromagnetic wave, gets stretched as it travels though the expanding space to reach us from far away galaxies. Because red light has longer wavelengths than blue light, we say the light from these galaxies is redshifted, meaning shifted to longer wavelengths.

6. The cosmological redshift

7. Misconception The cosmological redshift is not a Doppler shift. Doppler shifts are caused by the motion through space, cosmological redshifts are caused by the expansion of space. But there is no way to tell the difference from observations

8. 1 st rule to memorize Cosmological redshifts depend on the distance Doppler shifts do not depend on the distance See Chapter 5

9. Discussion If all of the galaxies are today getting farther away from each other, what does this tell you about the galaxies in the past?

10. Hubble time If we know how fast the universe is expanding, we can trace it back to find a time when all the galaxies we see were at the same place. This happened about 14 billion years ago.

11. Discussion What does this tell you about the size of the universe in past?

12. How big is the Universe? Universe – size unknown, may be infinite Observable universe – 14 billion light years in all directions

13. Speed of light and Distances Light travels through space at of fixed speed. 3.00 X 10 8 m/sec We can use this as a unit for measuring distances. A light year is the distance light travels in a year.

14. The Cosmic Horizon If the universe is only 14 billion years old, then the only light that we can see is the light that has had time to reach us. The farthest we can see is therefore 14 billion light years away, anything farther the light has not had enough time to reach us.

15. Cosmic Horizon

16. 1 st Law of Astronomy 201 If you squish something it gets hotter

17. Discussion Can you think of any examples from everyday life of something becoming hot as it is compressed?

18. Diesel vs. gasoline engines Gasoline – air fuel mixture ignited by sparkplug Diesel – air fuel mixture ignited by compression

19. Discussion Diesel engines are about twice as efficient as gasoline engines, so why are the vast majority of cars gasoline cars? Think about how the engines need to be different.

20. What is temperature? Temperature is average random speed of atoms or molecules that make up an object. Higher average random motions = higher temperatures

21. Air molecules at 0 C have an average velocity of about 485 m/s or 1090 miles/hour. Temperature

23. Discussion If temperature is a measure of how fast the atoms are moving, how can we have a cold wind? Shouldn’t all winds by definition be warmer than still air?

24. Why do compressed objects heat up? Consider a super ball bouncing on a table. What happens to the bouncing ball if you drop a book on it?

25. Electrostatic charges Like charges repel (+,+) or (-,-) Opposite charges attract (+,-)

27. Discussion If like charges repel each other, how came the nucleus of an atom can contain more than one positively charged protons? Why don’t all atoms heavy than hydrogen fly apart?

28. Protons and Neutrons You can consider a neutron to be a proton + an electron. A neutron decays into a proton and an electron. A proton smashed together with an electron will turn into a neutron.

29. Elements and isotopes The element is defined by the number of protons in the nucleus. The isotope is defined by the number of protons + neutrons in the nucleus.

32. 1 st Law of astronomy 201 If you squish something, it heats up The opposite is also true, if something expands it cools. Example – a refrigerator

33. Space is very cold, now As the universe expands, it cools. Currently its temperature is 2.73 K or –455 degrees F. But, as we run time back, the universe was much denser and much hotter.

35. Hydrogen The early universe consisted of entirely of a plasma of hydrogen nuclei (protons), neutrons, electrons and photons. More complex nuclei would be busted up by high speed collisions

36. Nucleosynthesis As the universe cooled Proton – neutron collisions produced deuterium deuterium – deuterium collisions produced 3 He deuterium – 3 He collisions produced 4 He.

37. The first 5 minutes At the end of nucleosynthesis the universe consisted of 75% hydrogen and 25% helium with a trace of lithium and beryllium. Also there were left over traces of deuterium and helium-3

38. Neutral atoms After about 380,000 years of expansion the universe cooled to about 3000 K and electrons could remain bound to protons forming the first neutral atoms.

39. Discussion What happens when a cloud of hydrogen and helium contracts because of gravity?

40. Cosmic Microwave Background

43. The early universe contained no life Without carbon, life could not exist in the early Universe. Planets like the Earth could not form without iron, silicon and oxygen.

44. Andromeda Galaxy

50. What are stars? Stars are enormous balls of mostly hydrogen and helium gas.

51. Internal pressure halts gravitational collapse The core of the star gets so hot that hydrogen can fuse into helium. The heat released by this reaction stops the star from contracting.

52. The struggle to avoid collapse When the hydrogen in the core runs out, the star starts to collapse again and becomes even hotter. If the star is massive enough it will become hot enough to fuse helium into carbon.

54. Ring nebula

57. How do the elements got out of the stars? Once enough iron builds up in the core of a massive star, it suddenly collapses. The outer layers of the star “bounce” off the core and are blasted into space in a supernova explosion.

58. Supernovae Supernovae explosions are the most energetic events in the Universe. A single star can outshine 100 billion stars. The explosion of the outer layers is so violent that all the elements heavier than iron can be produced, including many unstable radioactive isotopes.

59. Supernova 1987a

60. The Crab nebula

62. Supernovae can trigger star formation The expanding shock wave of a supernova explosion, can cause a nearby cloud of gas to collapse and form new stars. Thus, its heavy nuclei get incorporated into the next generation of stars.

67. Summary Squishing things makes them hot Temperature is a measure of the average random speed of atoms The universe started out with mostly hydrogen and helium with all other elements were created during supernovae explosions of stars more massive than the Sun