1. History & Development of Astronomy  Retrograde motion  The Greek Models  Geocentrism, Epicycles, & the Church  Copernicus  Tycho Brahe  Kepler  Galileo

2. What did ancient civilizations achieve in astronomy? Daily timekeeping Tracking the seasons and calendar Monitoring lunar cycles Monitoring planets and stars Predicting eclipses And more…

3. Days of the week were named for Sun, Moon, and the 5 visible planets.

4. Ancient people of central Africa (6500 B.C.) could predict seasons from the orientation of the crescent moon.

5.  Egyptian obelisk: Shadows tell time of day.

6. England: Stonehenge (completed around 1550 B.C.)

7. Mexico: model of the Templo Mayor

8. New Mexico: Anasazi kiva aligned north–south

9. SW United States: “Sun Dagger” marks summer solstice

10. Scotland: 4,000-year-old stone circle; Moon rises as shown here every 18.6 years.

11. Peru: lines and patterns, some aligned with stars

12. Macchu Pichu, Peru: structures aligned with solstices

13. South Pacific: Polynesians were very skilled in the art of celestial navigation.

14. France: Cave paintings from 18,000 B.C. may suggest knowledge of lunar phases (29 dots).

15. China: earliest known records of supernova explosions (1400 B.C.) Bone or tortoiseshell inscription from the 14th century B.C. "On the Xinwei day the new star dwindled." "On the Jisi day, the 7th day of the month, a big new star appeared in the company of the Ho star."

16. Two Different Early Models…  GEOCENTRIC  Earth is the center of everything  Earth doesn’t spin or move

17. The Geocentric Model as art…

18. Two Different Early Models…  HELIOCENTRIC  The Sun is the center of the solar system  Earth spins (rotates) to create day/night  Earth orbits (revolves) to create the year

19. Geocentric Models made “sense”  GEOCENTRIC: Earth doesn’t move  If we did, we’d feel it!  If we did, we’d lose the moon!  If we did, the stars around us would shift!  THEREFORE:  Sky (& Stars!) rotated around us  Sun & Moon & Planets actually move among key constellations of the Zodiac by design/choice

20. Two Different Early Models…  HELIOCENTRIC: Earth moves about the Sun  So do all of the planets  The Moon goes around us, too  Earth spins to create night and day  THEREFORE:  Sky (& Stars!) just SEEM to rotate around us  Sun & Moon & Planets moved among key constellations of the Zodiac because of OUR motion

21. KEY IDEA: Retrograde motion of the planets  We make the observation that planets – and only the planets – “dance” in front of the stars. How is this observation explained in each model?

22. The Motion of the Planets in the sky over time

23. The Motion of Mars In 2009-2010

24. Retrograde Motion Explanations  Ancient (and geocentric)  The planets move on their own around us  God(s) control their motions  Heaven’s realm – doesn’t concern us!  It just is…

25. Retrograde Motion Explanations  Modern (and heliocentric)  Earth and other planets orbit the sun at different rates  Earth “laps” slower-moving outer planets – and they appear to loop

27. Retrograde Motion Explanations  Modern (and heliocentric)  Earth and other planets orbit the sun at different rates  Inner planets speed between us & sun one way, then seem to reverse along far side

28. Venus’ Different Views  Venus September 2013 – evening sky

29. Venus’ Different Views  Venus September 2013 – evening sky

30. Venus’ Different Views  Venus January 2013 – morning sky

31. Why does modern science trace its roots to the Greeks?  How did the Greeks explain planetary motion?  How did Islamic scientists preserve and extend Greek science? Artist’s reconstruction of the Library of Alexandria

32. Our mathematical and scientific heritage originated with the civilizations of the Middle East.

33. Greeks were the first people known to make models of nature. They tried to explain patterns in nature without resorting to myth or the supernatural. Greek geocentric model (c. 400 B.C.) Why does modern science trace its roots to the Greeks?

34. Eratosthenes measures the Earth (c. 240 B.C.) Measurements: Syene to Alexandria distance ≈ 5,000 stadia angle = 7°

35. Eratosthenes measures the Earth (c. 240 B.C.) Calculate circumference of Earth: 7/360  (circum. Earth) = 5,000 stadia  circum. Earth = 5,000  360/7 stadia ≈ 250,000 stadia Compare to modern value (≈ 40,100 km): Greek stadium ≈ 1/6 km  250,000 stadia ≈ 42,000 km

36. Underpinnings of the Greek geocentric model: Plato Aristotle How did some Greeks explain planetary motion? Earth at the center of the universe Heavens must be “perfect”—objects move on perfect spheres or in perfect circles.

37. But this made it difficult to explain the apparent retrograde motion of planets… Review: Over a period of 10 weeks, Mars appears to stop, back up, then go forward again.

38. Sun-centered models had been considered Aristarchus Archimedes How did other Greeks explain planetary motion? Philolaus: Sun – the central “fire” at the center of the universe Aristarchus: Earth must be smaller Archimedes: Stars must be MUCH farther away!

39. The most sophisticated geocentric model was that of Ptolemy (A.D. 100–170) — the Ptolemaic model: Ptolemy Sufficiently accurate to remain in use for 1,500 years Arabic translation of Ptolemy’s work named Almagest (“the greatest compilation”)

40. So how does the Ptolemaic model explain retrograde motion? Planets really do go backward in this model.

41. Ptolemaic Retrograde Motion

43. What happened after Ptolemy’s model?  Theologically  Earth at the center of everything “fits” western religious growth in Christianity  Scientifically  Earth rotating and revolving mysteriously through “unseen” forces is hard to prove  Science was unnecessary…

44. The Roman Era

45. The Roman Era … Science should be “practical”

46. The Fall of Rome

47. The Looting of the Library of Alexandria

48. The Dark Ages…..

49. The Dark Ages….. In Europe…

50. Not in the Middle East, China, The Yucatan, Polynesia….

51. The Dark Ages….. In Europe… The Crusades!

52. Greek Records, Preserved, Translated, and advanced by Arabic Empires are brought back to Europe… Including works by Ptolemy, Eratosthenes, Aristarchus, others

53. The Crusades! Greek Records, Preserved, Translated, and advanced by Arabic Empires are brought back to Europe… …and used for navigation charts

54. The Crusades! Greek Records, Preserved, Translated, and advanced by Arabic Empires are brought back to Europe… …and Ptolemy’s model doesn’t quite work – especially for Mercury

55. The Crusades! Greek Records, Preserved, Translated, and advanced by Arabic Empires are brought back to Europe… …and they are copied and kept…

56. The Crusades! Greek Records, Preserved, Translated, and advanced by Arabic Empires are brought back to Europe… …and they are copied and kept… by the Church

58. How did Copernicus, Tycho, and Kepler challenge the Earth-centered idea? Copernicus (1473–1543): Proposed Sun-centered model (“heliocentric”) published 1543. Used model to determine layout of solar system

59. How did Copernicus, Tycho, and Kepler challenge the Earth-centered idea? Copernicus (1473–1543): Sun-centered model Determined layout of solar system (planetary distances in AU). But... Assumed CIRCULAR orbits Model was no more accurate than Ptolemaic model in predicting planetary positions.

61. Brahe compiled most accurate naked eye measurements of planetary positions ever made at the time. Precise to 1/60 th of a degree!

62. Still could not detect stellar parallax Thought Earth must be at center of solar system Recognized that other planets go around Sun. Tycho Brahe (1546–1601)

63. Parallax

64. Parallax results from shift in viewing position If CLOSE to Earth, a star would be seen in different locations (at different angles)

65. Parallax results from shift in viewing position If FAR from Earth, a star would NOT be seen in different locations (at different angles)

66. Hired Johannes Kepler, who used Tycho’s observations to discover actual shape of planetary orbits and motions. Tycho Brahe (1546–1601)

68. Johannes Kepler (1571–1630) Kepler first tried to match Tycho’s observations with circular orbits. An 8 arc-minute discrepancy (about 13% of one degree) led him eventually to ellipses. Developed 3 “laws” of orbits

69. Johannes Kepler (1571–1630) An 8 arc-minute discrepancy (about 13% of one degree) led him eventually to ellipses. 100 meters away! 8 arc-min

70. Johannes Kepler (1571–1630) “If I had believed that we could ignore these eight minutes [of arc], I would have patched up my hypothesis accordingly. But, since it was not permissible to ignore, those eight minutes pointed the road to a complete reformation in astronomy.”

71. An ellipse looks like an elongated circle. What is an ellipse?

72.  Shape  Speed  Time What are Kepler’s three laws of planetary motion?

73. The orbit of each planet around the Sun is an ellipse with the Sun at one focus. Kepler’s First Law: SHAPE

74. As a planet moves around its orbit, it sweeps out equal areas in equal times. Kepler’s Second Law: SPEED

75. This means that a planet travels faster when it is nearer to Sun Kepler’s Second Law: SPEED and slower when it is farther from the Sun.

76. Kepler’s Second Law Simulation at Mastering Astronomy

77. More distant planets orbit the Sun at slower average speeds, obeying the relationship p 2 ~ a 3 p = orbital period (years or days) a = average distance from Sun Kepler’s Third Law: Time

78. Kepler’s Third Law Simulation at Mastering Astronomy

79. Graphical version of Kepler’s Third Law

80. Kepler’s Data Planet Orbit “a” (miles) Period “P” (days) a3a3 P2P2 a3P2a3P2 Mercury 3.596 x 10 7 86.9646.49 x 10 21 77346.009 x 10 18 Venus 6.716 x 10 7 224.7303.3 x 10 21 504906.008 x 10 18 Earth 9.290 x 10 7 365.3801.7 x 10 21 1335006.009 x 10 18 Mars 14.16 x 10 7 687.12836 x 10 21 4721006.008 x 10 18 Jupiter 48.33 x 10 7 4323112900 x 10 21 187800006.012 x 10 18 Saturn 88.61 x 10 7 10760695800 x 10 21 1158000006.011 x 10 18

81. Graphical version of Kepler’s Third Law

84. The Aristotelian Beliefs of Galileo’s Time: Heliocentrism was impossible! 1.Earth was the center of all celestial motions, & everything orbited us. 2.Noncircular orbits are not “perfect” as heavens should be. 3.Earth could not be moving because objects in air would be left behind. 4.If Earth were really orbiting Sun, we’d detect stellar parallax.

85. Galileo’s Telescopic Observations 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

86. 1.The Moon had mountains & craters

87. 2. The Sun had spots

88. 3. Jupiter had four moons in orbit around the planet!

89. Jupiter’s Moons

90. 4. Venus had phases & shape changes

91. 5. Saturn had “ears”

92. 6. The Milky Way had countless stars

93. The Importance of Galileo’s Telescopic Observations 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

94. The Heavens were NOT “perfect” 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

95. The Earth was NOT the only center of motion 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

96. Earth could “keep” its moon if it orbited the Sun 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

97. Venus HAD to orbit the Sun, not Earth 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

98. Galileo’s observations of phases & shape changes of Venus proved that it orbits the Sun and not Earth.

99. Geocentric system: Venus always seen as crescent About the same size Heliocentric system: Venus changes phase Distance varies so SIZE varies too

100. Stars are so far away, we can’t measure parallax even if the Earth moved! 1.The Moon had mountains & craters 2.The Sun had spots 3.Jupiter had moons 4.Venus had phases & shape changes 5.Saturn had “ears” 6.The Milky Way had countless stars

101. Galileo’s observations destroyed Aristotelian beliefs held to be true: 1.Noncircular orbits are not “perfect” as heavens should be. 2.Earth was the center of all celestial motions, & everything orbited us. 3.Earth could not be moving because objects in air would be left behind. 4.If Earth were really orbiting Sun, we’d detect stellar parallax.

102. Moons of Jupiter clearly orbited Jupiter, not Earth Venus’ Phases and size changes showed it orbited the Sun, not Earth. NOTE! He didn’t see proof of EARTH orbiting the sun Overcoming the first objection (Earth at center of solar system):

103. Galileo’s experiments showed that objects in air would stay with a moving Earth. Overcoming the second objection (nature of motion): Aristotle thought that all objects naturally come to rest. Galileo showed that objects will stay in motion unless a force acts to slow them down (Newton’s first law of motion). The planets COULD move about the Sun and not stop!

104. Overcoming the third objection (heavenly perfection): Using his telescope, Galileo saw: —Sunspots on Sun (“imperfections”) —Mountains and valleys on the Moon (proving it is not a perfect sphere) —“Ears” of Saturn

105. Tycho thought lack of parallax seemed to rule out an orbiting Earth. Galileo showed stars must be much farther than Tycho thought—in part by using his telescope to see that the Milky Way is countless individual stars. If stars were much farther away, then lack of detectable parallax was no longer so troubling. Overcoming the fourth objection (parallax):

106. Galileo Galilei In 1633 the Catholic Church ordered Galileo to recant his claim that Earth orbits the Sun. His book on the subject was removed from the Church’s index of banned books in 1824. Galileo was formally vindicated by the Church in 1992.

109. Summary of Key Ideas

110. The Scientific Method Make Observations Research/Consider Prior Theories Analyze Results

111. The Scientific Method Make Observations Research/Consider Prior Theories Analyze Results If pre-existing theories explain observation, propose new observations & experiments to extend theories.

112. The Scientific Method Make Observations Research/Consider Prior Theories Analyze Results If pre-existing theories explain observation, propose new observations//experiments to extend theories. If NO pre-existing theories explain observation, modify or develop new theory

113. The Scientific Method Make Observations Research/Consider Prior Theories Analyze Results If pre-existing theories explain observation, propose new observations//experiments to extend theories. If NO pre-existing theories explain observation, modify or develop new theory Make predictions from new/modified theory Do the Experiment! Analyze Results Submit for Peer Review & Publish

114. WHAT DID YOU THINK?  What makes a theory scientific?  A theory is an idea or set of ideas proposed to explain something about the natural world. A theory is scientific if it makes predictions that can be objectively tested and potentially disproved.

115. WHAT DID YOU THINK?  What is the shape of Earth’s orbit around the Sun?  All planets have elliptical orbits around the Sun.

116. WHAT DID YOU THINK?  Do the planets orbit the Sun at constant speeds?  No. The closer a planet is to the Sun in its elliptical orbit, the faster it is moving. The planet moves fastest at perihelion and slowest at aphelion.

117. WHAT DID YOU THINK?  Do all of the planets orbit the Sun at the same speed?  No. A planet’s speed depends on its average distance from the Sun. The closest planet moves fastest, the most distant planet moves slowest.

118. WHAT DID YOU THINK?  How much force does it take to keep an object moving in a straight line at a constant speed?  Unless an object is subject to an outside force, like friction, it takes no force at all to keep it moving in a straight line at a constant speed.

119. WHAT DID YOU THINK?  How does an object’s mass differ when measured on Earth and on the Moon?  Assuming the object doesn’t shed or collect pieces, its mass remains constant whether on Earth or on the Moon. Its weight, however, is less on the Moon.

120. WHAT DID YOU THINK?  Do astronauts orbiting the Earth feel the force of gravity from our planet?  Yes. They are continually pulled earthward by gravity, but they continually miss it because of their motion around it. Because they are continually in free-fall, they feel weightless.