1. Lecture Outline Chapter 10: Other Planetary Systems: The New Science of Distant Worlds

2. BETA Pictoris – the first hint at Stars with Planetary Disks?

4. Detecting Planets around OTHER stars! KEPLER COROT WASP

5. Why are extrasolar planets difficult to detect? Sun-like stars are about a billion times brighter than any light reflected from its planets. Planets are close to their stars, relative to distance from us to the star. –Like being in San Francisco & trying to see a pinhead 15 meters from a grapefruit in Washington, D.C.

6. So given how bright stars are, how CAN we detect planets around other stars?

7. Planet Detection IndirectIndirect: Measurements of stellar properties revealing the effects of orbiting planets DirectplanetsDirect: Pictures or spectra of the planets themselves

8. Indirect Detection through Gravitation Sun & Jupiter orbit around their common center of mass. Sun wobbles around center of mass with same period as Jupiter.

9. Gravitational Tugs Sun's motion around solar system's center of mass depends on tugs from all planets. Astronomers around other stars measuring this motion could determine masses and orbits of all planets! © 2015 Pearson Education, Inc.

10. Astrometric Technique We can detect planets by measuring change in star's position on sky. However, tiny motions are very difficult to measure (~ 0.001 arcsecond). © 2015 Pearson Education, Inc.

11. Doppler Technique Measuring a star's Doppler shift can tell us its motion toward & away from us. Current techniques can measure motions as small as 1 m/s (walking speed!). © 2015 Pearson Education, Inc.

12. 1st Extrasolar Planet Detected The planet around 51 Pegasi has a mass similar to Jupiter’s, despite its small orbital distance.

13. First Extrasolar Planet Doppler shifts of the star 51 Pegasi indirectly revealed a planet with 4-day orbital period. Short period means that planet has small orbit. This was the first extrasolar planet to be discovered around a Sun-like star (1995). © 2015 Pearson Education, Inc.

14. Transits and Eclipses A transit is when a planet crosses in front of a star. Reduces star's apparent brightness & tells radius. Sometimes an eclipse – the planet passing behind the star, can also be detected © 2015 Pearson Education, Inc.

15. Kepler NASA's Kepler mission launched in 2008 to begin looking for transiting planets. Designed to measure 0.008% decline in brightness when an Earth-mass planet eclipses a Sun-like star. © 2015 Pearson Education, Inc.

16. Other Planet-Hunting Strategies Gravitational Lensing: Mass bends light in a special way when a star with planets passes in front of another star.

17. Other Planet-Hunting Strategies Features in Dust Disks: Gaps, waves, or ripples in disks of dusty gas around stars can indicate presence of planets.

18. Inferring planets that aren’t seen!

19. Direct Detection Special techniques for concentrating or eliminating bright starlight are enabling the direct detection of planets.

20. Direct Detection

21. What properties of extrasolar planets can we measure?

22. Measurable Properties Orbital period, distance, and shape Planet mass, size, & density Atmospheric properties

23. Planet Mass and Orbit Tilt We cannot measure an exact mass for a planet without knowing tilt of its orbit, because Doppler shift tells us only velocity toward/away from us. Doppler data give us lower limits on masses.

24. Calculating density Using mass, determined using Doppler technique, & size, determined using transit technique, density can be calculated.

25. How do extrasolar planets compare with planets in our solar system?

26. Orbits of Extrasolar Planets Most of the detected planets have orbits smaller than Jupiter's. Planets at greater distances are harder to detect with the current techniques. Orbits of some extrasolar planets are much more elongated (have a greater eccentricity) than those in our solar system.

27. Orbits and sizes of extrasolar planets from Kepler

28. Results from Kepler indicate that planets are common, and small planets greatly outnumber large planets!

29. Masses and sizes of extrasolar planets © 2015 Pearson Education, Inc.

30. Surprising Characteristics Some extrasolar planets have highly elliptical orbits. Planets show huge diversity in size and density. Some massive planets, called hot Jupiters, orbit very close to their stars. © 2015 Pearson Education, Inc.

31. Do we need to modify our theory of solar system formation?

33. Revisiting the Nebular Theory The nebular theory predicts that massive Jupiter-like planets should not form inside the frost line (at << 5 AU). The discovery of hot Jupiters has forced reexamination of nebular theory. Planetary migration or gravitational encounters may explain hot Jupiters.

34. Planetary Migration A young planet’s motion can create waves in a planet- forming disk. Models show that matter in these waves can tug on a planet, causing its orbit to migrate inward.

35. Hot Jupiters

36. Gravitational Encounters Close gravitational encounters between two massive planets can eject one planet while flinging the other into a highly elliptical orbit. Multiple close encounters with smaller planetesimals can also cause inward migration.

37. Modifying the Nebular Theory Observations of extrasolar planets have shown that the nebular theory was incomplete. Effects like planet migration and gravitational encounters might be more important than previously thought.

38. Planetary Types There seem to be a much greater variety of planet types than we find in our solar system. This includes gas giants with very different densities and water worlds.

39. Thought Question What happens in a gravitational encounter that allows a planet's orbit to move inward? A.It transfers energy and angular momentum to another object. B.The gravity of the other object forces the planet to move inward. C.It gains mass from the other object, causing its gravitational pull to become stronger.

40. Thought Question What happens in a gravitational encounter that allows a planet's orbit to move inward? A.It transfers energy and angular momentum to another object. B.The gravity of the other object forces the planet to move inward. C.It gains mass from the other object, causing its gravitational pull to become stronger.

41. Are planetary systems like ours common?

42. What have we learned? Do we need to modify our theory of solar system formation? –Original nebular theory cannot account for the existence of hot Jupiters. –Planetary migration or gravitational encounters may explain how Jupiter-like planets moved inward. Are planetary systems like ours common? –The answer is coming soon…

43. The Process of Science Observation: TMR-1 “detected” in 1998

44. The Process of Science Observation: TMR-1 “detected” in 1998 planetHypothesis: It is a planet, connected by a disk to a double (binary star)

45. The Process of Science Observation: TMR-1 “detected” in 1998 planet ?Hypothesis: It is a planet ? Critical Tests: Spectra

46. The Process of Science Observation: TMR-1 “detected” in 1998 planet ?Hypothesis: It is a planet ? Critical Tests: Spectra Result: A background star!

47. The Process of Science

48. How do extrasolar planets compare with our solar system?

49. Orbits of Extrasolar Planets Most of the detected planets have orbits smaller than Jupiter’s. Planets at greater distances are harder to detect with the Doppler technique.

51. Orbits of Extrasolar Planets Most of the detected planets have greater mass than Jupiter. Planets with smaller masses are harder to detect with the Doppler technique.

52. Planets: Common or Rare? One in ten stars examined so far have turned out to have planets. The others may still have smaller (Earth-sized) planets that cannot be detected using current techniques.

53. Surprising Characteristics Some extrasolar planets have highly elliptical orbits. Some massive planets orbit very close to their stars: “Hot Jupiters.” –See “SuperWASP”SuperWASP