2. ASTR100 (Spring 2008) Introduction to Astronomy The Science of Astronomy Prof. D.C. Richardson Sections 0101-0106

3. How did astronomical observations benefit ancient societies? Keeping track of time and seasons. For practical purposes, including agriculture. For religious and ceremonial purposes. Aid to navigation.

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

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

6. Planets Known in Ancient Times Mercury –difficult to see; always close to Sun in sky Venus –very bright when visible — morning or evening “star” Mars –noticeably red Jupiter –very bright Saturn –moderately bright The “Wanderers”

7. 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…

8. Egyptian obelisk: shadows tell time of day, like a modern-day sundial.

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

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

11. Wyoming: Big Horn Medicine Wheel

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

13. 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 BC) Modern science traces its roots to the Greeks

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

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

16. Explaining Apparent Retrograde Motion Easy for us to explain: occurs when we “lap” another planet (or when Mercury or Venus lap us). But very difficult to explain if you think that Earth is the center of the universe! In fact, ancients considered but rejected the correct explanation…

17. The most sophisticated geocentric model was that of Ptolemy (A.D. 100-170) — the Ptolemaic model: Sufficiently accurate to remain in use for 1,500 years. Ptolemy

18. Copernicus (1473-1543) proposed a Sun-centered model, but still based on perfect circles. Copernicus (1473–1543)

19. Copernicus (1473-1543) proposed a Sun-centered model, but still based on perfect circles. Tycho Brahe (1546-1601) made careful observations but could not detect Earth’s motion.

20. Copernicus (1473-1543) proposed a Sun-centered model, but still based on perfect circles. Tycho Brahe (1546-1601) made careful observations but could not detect Earth’s motion. Kepler used Brahe’s data to show the Copernican model could work, but only if planetary orbits are ellipses, not circles! 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.”

21. Kepler’s First Law: The orbit of each planet around the Sun is an ellipse with the Sun at one focus. Kepler’s three laws of planetary motion

22. Kepler’s Second Law: As a planet moves around its orbit, it sweeps out equal areas in equal times. This means that a planet travels faster when it is nearer to the Sun and slower when it is farther from the Sun.

23. More distant planets orbit the Sun at slower average speeds, obeying the relationship p 2 = a 3 p = orbital period in years a = avg. distance from Sun in AU Kepler’s Third Law

24. Kepler’s 3 rd Law

25. Thought Question An asteroid orbits the Sun at an average distance of a = 4 AU. How long does it take to orbit the Sun? A.4 years. B.8 years. C.16 years. D.64 years. (Hint: remember that p 2 = a 3.)

26. Thought Question An asteroid orbits the Sun at an average distance of a = 4 AU. How long does it take to orbit the Sun? A.4 years. B.8 years. C.16 years. D.64 years. (Hint: remember that p 2 = a 3.)

27. How did Galileo solidify the Copernican revolution? Galileo (1564-1642) overcame major objections to the Copernican view.

28. Using his telescope, Galileo saw: sunspots on Sun (“imperfections”) mountains and valleys on the Moon (proving it is not a perfect sphere)

29. Galileo also saw four moons orbiting Jupiter, proving that not all objects orbit the Earth…

30. … and his observations of phases of Venus proved that it orbits the Sun and not Earth. Ptolemaic ViewCopernican View

31. ASTR100 (Spring 2008) Introduction to Astronomy Newton’s Laws of Motion Prof. D.C. Richardson Sections 0101-0106

32. How do we describe motion? Precise definitions to describe motion: Speed: rate at which object moves. speed = distance/time (units: m/s) Example: speed of 10 m/s. Velocity: speed and direction. Example: 10 m/s due east. Acceleration: any change in velocity. Units: speed/time (m/s 2 ).

33. The Acceleration of Gravity All falling objects accelerate at the same rate (not counting friction of air resistance). On Earth, g ≈ 10 m/s 2 : speed increases 10 m/s with each second of falling.

34. The Acceleration of Gravity (g) Galileo showed that g is the same for all falling objects, regardless of their mass. Apollo 15 demonstration

35. Momentum and Force Momentum = mass × velocity. A net force changes momentum. Often only velocity changes (not mass). The rotational momentum of a spinning or orbiting object is known as angular momentum.

36. Is there a net force? Y/N 1.A car coming to a stop. 2.A bus speeding up. 3.An elevator moving at constant speed. 4.A bicycle going around a curve. 5.A moon orbiting Jupiter. 

37. How is mass different from weight? mass – amount of matter in an object. weight – force that acts upon an object. You are weightless in free-fall!

38. On the Moon… A.My weight is the same, my mass is less. B.My weight is less, my mass is the same. C.My weight is more, my mass is the same. D.My weight is more, my mass is less.

39. On the Moon… A.My weight is the same, my mass is less. B.My weight is less, my mass is the same. C.My weight is more, my mass is the same. D.My weight is more, my mass is less.

40. Why are astronauts weightless in space? There IS gravity in space… Weightlessness is due to a constant state of free-fall…

41. Realized the same physical laws that operate on Earth also operate in the heavens…  one universe. Discovered laws of motion and gravity. Much more: experiments with light; first reflecting telescope; calculus… How did Newton change our view of the Universe? Sir Isaac Newton (1642-1727)