1. Extrasolar Planets
This exoplanet orbiting 51 Pegasi is currently being vaporized by it’s parent star

2. Exoplanet Exploration: A new field in Astronomy
For centuries Astronomers have asked two fundamental questions.
1. Do other worlds exist?
2. Is there life on those other worlds?
Over the last 15 years we have been able to answer “YES” to the first question.
Other worlds are common in the universe
Within the next 15 years we will be able to answer the second question.

3. Extrasolar Planet (Exoplanet) - A planet that orbits a star outside our solar system.
Artists conception of Gliese 581 C - The only terrestrial planet discovered in a stars Habitable Zone (besides Earth). Water on this planet would be in liquid form, like Earth. It is 5 times more massive than Earth and twice the size.

4. As of April, 2009, over 400 Extrasolar Systems have been discovered
As of April, 2009, over 400 Extrasolar Systems have been discovered. But only 8 terrestrial planets have been found
Oceans of lava glow red on the night side of Gliese 876 d. In the distance glow two other planets c and b of Gliese It is 7 times the mass of earth, and has a mean temperature of 642 Kelvin.

5. 287 Extrasolar Systems Discovered so far (April 2008):
6 Terrestrial Planets
182 Gas Giants
77 Hot Jupiters
3 Hot Neptunes (Water Giants)
5 Pulsar Planets

6. Besides planets, Astronomers have also detected:
- 3 Kuiper Belts
- 2 Asteroid Belts
Artists concept of the asteroid belt and planets around the star HD 69830

7. Besides planets, Astronomers have also detected:
- 14 Forming Solar Systems with newly formed planets
Images of planet forming dust disks around stars

8. Properties of Known Extrasolar Systems
Why are most exoplanets gas giants that orbit close to the parent star?
Because our current detection methods are biased toward finding gas giants close to the parent star.
It is difficult to find small terrestrial planets with our current methods.

9. . Planets don't produce any light of their own, except when young.
The challenges of observing extrasolar planets stem from three basic facts:
Planets don't produce any light of their own, except when young.
They are an enormous distance from us.
They are lost in the blinding glare of their parent stars. .
The first planets to be found around nearby stars have never been seen. Instead, astronomers have discovered them indirectly, inferring the existence of an unseen companion through its effects on the star itself.

10. Exoplanet Detectoion Methods:
5 proven methods
- Astrometry & Radial Velocity Method : 235 systems
- Transit Method: 46 systems
- Microlensing Method: 6 systems
- Pulsar Timing Method: 3 systems

11. 1) Astrometric Method
Astrometric Method: Astrometry consists of measuring a star's position in the sky and observing the ways in which its position changes over time.
If the star has a planet, then the gravitational influence of the planet will cause the star to move in a tiny circle.

12. Astrometric Method
Astrometric displacement of the Sun due to Jupiter as at it would be observed from 10 parsecs, or about 33 light-years.

13. Astrometric Method

14. Astrometric Method
Astrometric Method: Pro’s and Con’s
Pro’s:
1 telescope can search many stars at a time
Con’s:
Does not work for far away stars (Can’t see the motion)
Difficult to detect Terrestrial planets (not sensitive enough)
Process is slow (needs to observe multiple orbits)

15. 2) Radial Velocity Method
Doppler Effect Demo
# of frames b.t. strikes

16. Radial Velocity Method
Doppler Effect - The change in frequency of a wave as perceived by an observer moving relative to the wave source.
If a wave source is moving TOWARD an observer, the waves tend to “pile up”, INCREASING the frequency, or pitch.
If a wave source is moving AWAY FROM an observer, the waves tend to “spread out”, DECREASING the frequency, or pitch.

17. Radial Velocity Method
The Doppler effect works for all kinds of waves, including light.
Instead of the pitch changing, the color changes.
The color change is very slight, and not noticeable to the human eye. However, it can be seen when studying the spectrum. The spectrum appear to be shifted toward the red or blue

18. Blue Shift - Object is approaching Red Shift - Object is receding
Radial Velocity Method
Blue Shift - Object is approaching
Red Shift - Object is receding

19. Radial Velocity Method

20. Radial Velocity Method

21. Radial Velocity Method Radial Velocity Method (Doppler Method) -
This method measures slight changes in a star's velocity as the star and the planet move about their common center of mass.
Astronomers can detect this motion by analyzing the spectrum of starlight due to the Doppler shift in the stars spectrum.
The larger the planet and the closer it is to the host star, the faster the star moves about the center of mass, causing a larger color shift in the spectrum of starlight. That's why many of the first planets discovered are Jupiter-class (300 times as massive as Earth), with orbits very close to their parent stars.

22. Radial Velocity Method
Planet: 55 Cancri E – A Hot Terrestrial Planet

23. Radial Velocity Method
Radial Velocity Method: Pro’s and Con’s
Pro’s:
Can be used on far away stars
Con’s:
Can only observe 1 star at a time (with high tech spectrographs)
Difficult to detect Terrestrial planets (not sensitive enough)
Process is slow (needs to observe multiple orbits)

24. 3) Transit Method
From the vantage point of the Earth, the planet of HD moves across the face of its star once every few days. It is so close that it is being vaporized by the star.

25. Transit Method
Transit Method: If a planet passes directly between a star and an observer's line of sight, it blocks out a tiny portion of the star's light, thus reducing its brightness.
Sensitive instruments can detect this periodic dip in brightness. From the period and depth of the transits, the orbit and size of the planets can be calculated.

26. Transit Method

27. Transit Method

28. Transit Method

29. Properties of Known Extrasolar Systems

30. Transit Method

31. Transit Method: Pro’s and Con’s
Can be used on far away stars
Can detect Terrestrial Planets (Method is sensitive enough)
Can determine atmospheric composition
Con’s:
Can only detect ~1% of all solar systems (angles need to exactly align)
Process is slow (needs to observe multiple orbits)
Also called Photometric Method

32. Gravitational Microlensing Method

33. Gravitational Microlensing Method
If a planet transits EXACTLY through the center of the parent star, gravity from the planet will bend the starlight
Like a lens. The lensed light is magnified, and the star appears to briefly brighten.
Telescopes can watch for the breif brightening of a star to detect a planet.

34. Gravitational Microlensing Method

35. Gravitational Microlensing Method
Pro’s:
Sensitive enough to detect terrestrial planets
Con’s:
The chances of a planet microlensing are very rare.
Extremely sensitive instruments need to be used.

36. Pulsar Timing Method

37. Pulsar Timing Method
Pulsar 1
Pulsar 2
Pulsar 3

38. Pulsar Timing Method
Pulsar- The core of an exploded star that gives off a spinning beam of radiation (like a lighthouse).
From earth, it appears to Pulse radiation at a specific rate.
Pulsar Timing Method: A planets gravitational influence will disrupt the natural Pulse cycle of a pulsar. Astronomers can measure the disrupted pulses to determine the planets size and orbit.

39. Pulsar Timing Method
Pro’s:
Con’s:
Only works for Pulsars (Very rare)
The original planets would be destroyed in the explosion
of the star. The planets they find are formed from the debris after the star exploded. (Some astronomers do not consider these objects to be planets)

40. Properties of Known Extrasolar Systems

41. Future Space Missions:
Kepler Mission – Transit Method

42. Future Space Missions:
Kepler Mission – Transit Method

43. KEPLER MISSION i. Mission Started in April 2009
ii. The Kepler Mission uses the Transit method to search over 10,000 stars.
iii. It will find gas giants as well as Terrestrial planets.
iv. Expected to find:
between 50 to 650 Terrestrial Planets in Earth like orbits,and 900 Hot Gas Giants.

44. SIM PlanetQuest Mission
Expected Start -2012
Will use astrometric method
will search the nearest 250 stars.
Expected to find terrestrial and gas planets

45. Darwin and TFP TFP = Terrestrial Planet finder Expected start: 2015
Will directly image terrestrial planets using IR (take actual pictures!)

46. Darwin and TFP Expects to find:
Signs of life in the atmospheres in order to determine if the planet is habitable
If a Terrestrial planet has CO2, H2O, O3 (Ozone) it will be habitable.

47. Protoplanetary Disks

48. Exit Slip
List the 5 types of detection methods used to discover extra solar planets
Describe how we use either the transit method or the doppler effect to discover exoplanets
What is the current mission to find exoplanets, what type of method does it use, and what does it expect to find.

49. Protoplanetary Disks around Beta Pictoris

50. Basic Definitions
Protoplanetary Disk -rotating disk of dense gas surrounding a young newly formed star,
Protostar -a cloud of hot, dense gas and dust that is gravitationally collapsing to form a star
Protoplanets -are moon-sized planets, or larger embryos within protoplanetary discs

51. T-Tauri Star -young star that is just beginning nuclear fusion and produces strong outflows of particles (winds)
Solar Nebula -The disk of gas and dust that surrounded the sun when it was forming.
Jovian Planet – Gas planet

52. Planetary Formation:
                                                                                                                                                   

53. Location of star formation:
Solar System Formation
Solar Systems naturally form around stars
Therefore, solar systems form where star formation is Prevalent.
Location of star formation:

54. Solar System Formation
M100 spiral galaxy
A map of our Galaxy

56. M16 : Eagle Nebula

57. Solar System Formation

58. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
Gravity causes the solar nebula to contract and flatten into a spinning disk, a protoplanetary disk. The large blob in the center will become the Star.

59. Orion Nebula

60. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
2. Most of the mass goes toward the center, forming a Protostar. In the Protoplanetary Disk gravity causes dust grains to collide, stick together, and grow into moon-sized protoplanets.

61. Protoplanetary Disks

62. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
3. Strong winds from the still-forming Star expel the gas.
Planetesimals continue to collide and grow. Over the course of a hundred million years or so, protoplanets collide forming a few large planets that travel in roughly circular orbits.

63. Solar System Formation

64. Solar System Formation

65. Solar System Formation

66. Protoplanetary Disks

67. Protoplanetary Disks

68. Protoplanetary Disks

70. Protoplanetary Disks

71. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
4. When Fusion takes hold in the protostar, it becomes a star. This infant star is called a T-Tauri Star. Solar wind from the T-Tauri star blows the remaining gas and dust away. The Star and a few planets remain.
Remaining debris, such as Asteroids and Comets in unstable orbits will Eventually collide into the planets or star.

72. T-Tauri Stars with Disks

74. Solar System Formation

75. Solar System Formation

76. Solar System Formation

77. Solar System Formation

78. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
5. Remaining debris, such as Asteroids and Comets in unstable orbits will Eventually collide into the planets or star.
These collisions account for the “quirks” found with some of the planets:

79. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
Remaining debris, such as Asteroids and Comets in unstable orbits will Eventually collide into the planets or star.
These collisions account for the “quirks” found with some of the planets:
Earth has a moon
Venus Rotates Backwards
Mercury has a large Iron core
Uranus rotates on its side

80. Solar System Formation

81. Solar System Formation Steps in Planet formation:
Problems with our current model:
Observations show our model is probably correct, but it needs slight modifications.
Example:
When our solar system is run through a simulation,
Uranus and Neptune do not form.

82. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
Other Info:
Gas giants cannot form within 4 A.U. of a sun like star. It is too hot for the H and He gas to condense.
Therefore, the gas giants we find close to a star MUST have been knocked inward from the outer solar system.

83. Steps in Planet formation:
Solar System Formation
Steps in Planet formation:
Other Info:
If the original solar nebula spins too fast. The nucleus will break apart and form multiple stars.