Astro 101 Fall 2013 -- Lecture #2

1. Astro101 Fall 2013 -- Lecture #2

2. Ancient Observers Noticed the “Wandering Stars” (e.g., planets) … They saw that sometimes they had “retrograde” motion. But they thought that Everything orbited the Earth. How could this be? (example) The hash marks show the position of Mars relative to the fixed stars at Five-day intervals

3. The “Geocentric Model” Ancient Greek astronomers knew of Sun, Moon, Mercury, Venus, Mars, Jupiter and Saturn. Aristotle vs. Aristarchus (3rd century B.C.): Aristotle: Sun, Moon, Planets and Stars rotate around fixed Earth. Aristarchus: Used geometry of eclipses to show Sun bigger than Earth (and Moon smaller), so guessed Earth orbits Sun. Also guessed Earth spins on axis once a day => apparent motion of stars. Aristotle: But there's no wind or parallax. Difficulty with Aristotle's "Geocentric" model: "Retrograde motion of the planets".

4. But if you support geocentric model, you must attribute retrograde motion to actual motions of planets, leading to loops called “epicycles”. Ptolemy's geocentric model (A.D. 140)

5. 13 Retrograde Motion – Correct Explanation 12 7 11 5 10 6 4 9 8 3 2 1 13 12 11 10 9 8 7 6 5 4 3 2 1

6. "Heliocentric" Model • Rediscovered by Copernicus in 16th century. • Put Sun at the center of everything. • Much simpler. Almost got rid of retrograde motion. • But orbits circular in his model. In reality, they’re elliptical, so it didn’t fit the data well. • Not generally accepted then. Copernicus 1473-1543

7. Galileo (1564-1642) Built his own telescope in 1609. 400 years ago. Discovered four moons orbiting Jupiter => Earth is not center of all things! Co-discovered sunspots. Deduced Sun rotated on its axis. Discovered phases of Venus, inconsistent with geocentric model.

8. Johannes Kepler • (1571 - 1630) • Born near Stuttgart • Studied philosophy and theology at Tubingen • Developed love for astronomy as a child • Showed high level of mathematical skill • Had a reputation as a skilled astrologer • Wanted to be a minister; became instead a teacher of astronomy and math in Graz, Austria • Became assistant to Tycho Brahe in 1601 • Developed Laws of Planetary Motion

9. Orbits of Planets – Heliocentric Model All orbit in same direction. Most orbit in same plane. Elliptical orbits, but low eccentricity for most, so nearly circular.

10. 13 Retrograde Motion – Correct Explanation 12 7 11 5 10 6 4 9 8 3 2 1 13 12 11 10 9 8 7 6 Earth 5 4 Jupiter (for example) 3 2 1

11. Kepler's First Law The orbits of the planets are elliptical (not circular) with the Sun at one focus of the ellipse. Ellipses eccentricity = (flatness of ellipse) distance between foci major axis length

12. Kepler's Second Law A line connecting the Sun and a planet sweeps out equal areas in equal times. faster slower Translation: planets move faster when closer to the Sun.

13. Kepler's Third Law The square of a planet's orbital period, P, is proportional to the cube of its semi-major axis, a. P2 α a3 (for circular orbits, a=radius). Translation: the larger a planet's orbit, the longer the period.

14. With the scale of the Solar System determined, can rewrite Kepler’s Third Law as: P2 = a3 as long as P is in years and a in AU. So compare Earth and Pluto: Object a (AU) P (Earth years) Earth 1.0 1.0 Pluto 39.53 248.6

15. Newton (1642-1727) Kepler was playing with mathematical shapes and equations and seeing what worked. Newton's work based on experiments of how objects interact. His three laws of motion and law of gravity described how all objects interact with each other.

16. Newton's Correction to Kepler's First Law The orbit of a planet around the Sun has the common center of mass (instead of the Sun) at one focus.

17. Timelines of the Big Names Galileo 1564-1642 Copernicus Newton Brahe 1473-1543 1473-1543 1546-1601 1642-1727 Kepler 1571-1630

18. At this time, actual distances of planets from Sun were unknown, but were later measured. One technique uses parallax. “Earth-baseline parallax” uses telescopes on either side of Earth to measure planet distances.

19. The Celestial Sphere An ancient concept, as if all objects at same distance. But to find things on sky, don't need to know their distance, so still useful today. Features: - Does not rotate with Earth - Poles, Equator - Coordinate System

20. Celestial Coordinates: Right Ascension – parallel to lines of longitude, i.e., run from North to South -- in units of Hours, Minutes, Seconds -- why? Correspondence with sidereal rotation of the sky in 23 hr 56 min solar time Declination – parallel to lines of latitude, i.e., parallel to Equator

21. Lines of R.A. (Right Ascension) N Celestial Pole Lines of Decl. (Declination) + = Northern hemisphere - = Southern hemisphere N Pole Equator S Pole Earth A typical celestial coordinate would look like this: 21h 34m 13.3 sec +28.6 deg. Earth sphere “projected” outwards to the sky, except, it doesn’t rotate with the Earth S Celestial Pole

22. The Year Inclined view of the Earth’s orbit The Earth revolves around the Sun in 365.256 days (“sidereal year”).

24. The "Solar Day" and the "Sidereal Day" Solar Day How long it takes for the Sun to return to the same position in the sky (24 hours). Sidereal Day How long it takes for the Earth to rotate 360o on its axis. These are not the same!

25. One solar day later, the Earth has rotated slightly more than 360o . A solar day is longer than a sidereal day by 3.9 minutes (24 hours vs. 23 hours 56 minutes 4.091 seconds).

26. Scorpius Orion The Year Inclined view of the Earth’s orbit The Earth revolves around the Sun in 365.256 days (“sidereal year”). But the year we use is 365.242 days (“tropical year”). Why?

27. Precession The Earth has a bulge. The Moon "pulls down" on the side of the bulge closest to it, causing the Earth to wobble on its axis (how do we know this?) Vega * * Polaris Spin axis Precession animation Precession Period 26,000 years!

28. Scorpius Scorpius Orion Orion Now Night Day Day Night Summer: July Winter: January 13,000 years from now Night Night Day Day Winter: July or January? Summer: January or July? We choose to keep July a summer month, but then in 13,000 years, summer occurs on other side of orbit!

29. The Motion of the Moon The Moon has a cycle of "phases", which lasts about 29 days. Half of the Moon's surface is lit by the Sun. During this cycle, we see different fractions of the sunlit side. Which way is the Sun in each case?

31. Q: What is a “Blue Moon” ? A: The second Full Moon occuring within a single calendar month. Occur, on average, once every 2.7 years. Some American Full Moons September: Harvest Moon (Colonial American) October: Corn Ripe Moon (Taos) November: Sassafras Moon (Choctaw) December: Big Freezing Moon (Cheyenne) … there are many others (names for every month) …

32. Cycle of phases slightly longer than time it takes Moon to do a complete orbit around Earth. Orbit time or "sidereal month" Cycle of phases or "synodic month" 27.3 days 29.5 days

33. Eclipses Lunar Eclipse When the Earth passes directly between the Sun and the Moon. Sun Earth Moon Solar Eclipse When the Moon passes directly between the Sun and the Earth. Earth Moon Sun

34. Solar Eclipses Diamond ring effect - just before or after total Total Partial Annular - why do these occur?

35. LunarEclipse

36. Why don't we get eclipses every month? How can there be both total and annular eclipses?

37. Moon's orbit tilted compared to Earth-Sun orbital plane: Sun Moon Earth 5.2o Side view Moon's orbit slightly elliptical: Moon Distance varies by ~12% Earth Top view, exaggerated ellipse

38. Types of Solar Eclipses Explained

41. Certain seasons are favorable for eclipses. Solar “eclipse season” lasts about 38 days. Likely to get at least a partial eclipse somewhere. It's worse than this! The plane of the Moon's orbit precesses, so that the eclipse season occurs about 20 days earlier each year. Next total solar eclipse in N. America = August 2017

42. Rocket Science 101

43. Rocket Science 101 • The same laws that govern the motion of the planets around the sun (Kepler’s Laws) also govern: • -- Motion of satellites (“moons”) around planets • -- Motion of artificial satellites and spacecraft around the Earth • -- Motion of spacecraft on their way through the Solar System • What are the differences? • -- The body creating the gravity that governs the orbit (the “central • body”) is not necessarily the same • -- This determines the period of each orbit (time for orbit) • -- Orbits may be highly elliptical, or inclined • -- This also affects the period • -- The velocity (“speed”) of something moving in an elliptical orbit will be different than the velocity of something moving in a circular orbit at the same distance from the central body

44. Example Central Body could be Earth, Sun, Jupiter, … Circular Orbit 2 Circular Orbit 1 Central Body P2 P1 Elliptical Orbit 3 Orbits 1 and 2 are circular, so the velocity of the satellite/moon/spacecraft is the same everywhere in each orbit, BUT  Because the orbits have different radii (sizes = distances from the body), the velocities in the two orbits are not the same ! Velocity at P1 for Orbit 1 and Orbit 3 are also NOT the same (because they aren’t the same orbit!)

45. Some terminology “Apo” – Point of furthest distance = slowest speed in the orbit “peri” – Point of closest approach = fastest speed in the orbit Central Body x x Elliptical Orbit 3 Central body = Earth (satellites, Moon), we say “Perigee” and “Apogee” Central body = Sun (planets, comets, asteroids, interplanetary spacecraft) we say “Perihelion” and “Aphelion”

46. We can use Kepler to our advantage … How to get from Orbit 1 to Orbit 2: Circular Orbit 2 Burn 1 = Add velocity so that the moving object has the proper velocity for the”transfer” orbit It moves in the ellipse Out to point 2, then Burn 2 = Add velocity so that the moving object has the proper velocity for Orbit 2 All of these velocities can be calculated from Kepler’s Laws Elliptical (“transfer”) Orbit 3 Burn 2 Burn 1 Circular Orbit 1

47. You can see satellites sometimes… http://www.heavens-above.com

48. ISS Pass 20 Oct 2011 Albuquerque Sky Path