1. Announcements Reading Assignment posted for Lecture 1-3 + planetarium Please turn off all electronic devices Please sign attendance sheet

2. What is one piece of evidence that the Earth is round? a)North Star always same height above horizon b)Constellations always have the same orientation c)Shadow of Earth on Moon during lunar eclipse is rabbit-shaped d)Everyone on Earth sees same constellations e)North Star not always visible

3. Lecture 3: Greek Cosmology Astronomy 1143 – Spring 2014

4. Key Ideas: Greeks -- geocentric (Earth-centered) Universe Parallax – apparent shift in position of object viewed from different locations Geometric measure of distance Measuring the Moon’s Diameter Angular Diameter and Distance Needed Size of Moon & Sun relative to Earth measured – depth in heavens seen

5. Key Ideas: Evidence for Geocentric Universe High speeds not needed for Earth Stars do not change appearance over course of year No parallaxes seen for stars Ptolemy’s geocentric model Complicated by need to explain observations Retrograde motion explained by epicycles Model matched observations and made predictions – did it represent reality?

6. Describing the Sky We do not “see” a 3-dimensional night sky We can describe brightnesses and colors and motions Stars appear as single points of light Planets are close to points of light (at least to the naked eye) Sun and Moon appear as actual extended objects Describe separation of stars on the sky and the apparent size of objects by angular distance and angular size

7. Angular Size

8. Angular Distance & Size

9. Angular Size Changes with Distance The angular size of a dime and quarter can be the same, even though their physical sizes are different

10. Measuring big distances Measuring distances and physical sizes in astronomy is very difficult Obvious methods such as meter sticks are out (there’s that whole lack of oxygen thing) We don’t usually have reference objects here on Earth to help us out Answer: Use geometry

11. The Moon’s Size and Distance The first step to understanding the nature of the Moon is to measure how big it is and how far away it is. Measuring these quantities requires geometry. We again want to measure distances/sizes that are very, very big

12. Measuring the Size of the Moon The further away an object is, the smaller its apparent angular size. If two objects have the same angular size, the more distant object has a larger radius. We must know the distance to calculate the actual physical size of an object by geometry. True for things on Earth and in the sky

13. Geometry, Distance and Size Say you wanted to measure the height of this: a

14. The height of Mount Everest The height of Mount Everest (aka Chomoloangma or Sagarmatha) was very difficult to determine because its distance from surveyors was poorly known. Named after Sir George Everest, the surveyor-general of India 1808: Great Trigonometric Survey of India began 1852: Mt. Everest identified as the highest peak by Radhanath Sikdar

15. Definition of Parallax Parallax is the apparent shift in the position of an object when it is viewed at different positions The size of the shift depends on Distance to the object Distance between viewing points If you measure the angular size of the shift and the distance between the observation points, you can calculate the distance

16. Method of Trigonometric Parallaxes Distant Stars p Earth Foreground Object p = parallax angle

17. Parallax decreases with distance Closer objects have larger parallaxes: Distant objects have smaller parallaxes:

18. Lunar Parallax

19. Right Triangles opposite hypotenuse adjacent A

20. Right Triangles opposite hypotenuse adjacent A If you have a right triangle, the length of one side and the angle, you can get the length of the other side

21. Measuring the Moon’s Size Unlike parallax, we can do this from one place Step 1: Measure the angular size of an object on the sky and divide by 2 a You

22. Measuring the Moon’s Size Unlike parallax, we can do this from one place Step 1: Measure the angular size of an object on the sky and divide by 2 a/2 You R distance If we know a and distance, we can get R

23. Measuring the Moon’s Size Step 2: Use the definition of a tangent a/2 You R distance

24. Measuring the Moon’s Size Step 3: Put numbers into your calculator Distance of Moon: 384,400 km Angular size of Moon: 31’ (arcminutes) about ¼ of the Earth’s radius

25. Mean Distance: 384,400 km (~60 R Earth ) Perigee (nearest): 363,300 km Moon Appears ~11% larger at Perigee Apogee (farthest): 405,500 km

26. Moon at PerigeeMoon at Apogee

27. How does the Sun compare to the Earth and Moon? Measuring the parallax of the Sun is much more difficult Measurement of the Earth-Sun distance relies on more indirect methods However, a few facts about the relation between the Earth, Moon and Sun can be figured out from observations that ancient cultures could make

28. What can we learn from solar eclipses? The Sun is more distant than the Moon The Sun has the same angular size as the Moon Therefore, the Sun has a bigger radius than the Moon

29. Sun vs. Earth Greek astronomers calculated the size of the Sun as well as the Earth & Moon Aristarchus, using the angle between Earth-Moon- Sun at quarter moon (see EC problem), argued that the Sun was ~5 times larger than Earth Ptolemy, using other geometric arguments, found a similar value Aristarchus argued that the larger Sun should be stationary rather than the smaller Earth Ptolemy (and vast majority of other astronomer) thought that the Earth did not move. Why not?

30. Greek Cosmology Greek thinkers sought to: Explain observations with a model of the solar system Apply model to observations of Sun, Moon, planets & stars Scientific Method in operation! Geocentric Hypothesis Earth is at the center of the Universe, and everything orbits around the Earth

31. Aristotle-Greek, 384-322 BCE Hypothesized a geocentric system (Earth at the center) Hypothesis: The Earth is at the center of the Universe, and the planets orbit around the Earth

32. Claudius Ptolemais (Ptolemy - c. 150 CE) Great Astronomer & Geographer of the late classical age. Wrote the Mathematical Syntaxis Compilation of Mathematical & Astronomical knowledge of the time. Known to us as the Arabic “Al Magest” Argued for the geocentric model based on observational evidence.

33. Scientific Arguments For thousands of years, the consensus (but not the only view) was that the Universe was geocentric This was not because no one was making observations or testing hypotheses in a scientific manner Ancient astronomers discussed several reasons why observations were in agreement with a geocentric model Basic problems: did not conceive of the true distances to stars & incomplete knowledge of physics

34. The Need for Speed A major conceptual barrier was the enormous speed. Rotation at the Equator: Circumference of Earth: 40,000 km Time for One Rotation: 24 hours Speed = Distance  Time = 40,000 km  24 hr = 1670 km/hr

35. Ptolemy’s argument: you always see half the sky, so the Earth has to be at the center & very small compared to the size of the heavens

36. In addition, stars always have the same brightness. Earth not getting closer or farther away.

37. Lack of Stellar Parallaxes June Distant Stars Foreground Star December

38. Simple Geocentric Model of Universe However, model does not explain all observations Variable speed of Sun and Moon across the sky – different angular distances covered night to night RETROGRADE MOTION

39. Mars Retrograde Motion August 2003 Photo by Turkish amateur astronomer Tunç Tezel

40. Earth Epicycle

41. Ptolemy’s Solar System

42. The Ultimate Geocentric System Ptolemy’s Universe Geocentric Sun larger than Earth larger than Moon Heavens have depth and are distant from Earth Ptolemy’s final geocentric system was quite complex: 40 epicycles & deferents required. Equants & eccentrics for all planets, the Moon, & the Sun It agreed with the available observations and predicted the motions of the planets, Sun, and Moon. It was to prevail virtually unchallenged for nearly 1500 years.