1. Solar System Formation

2. Review Question
What causes the Doppler shift of light?

3. Review Question
How does a glass lens bend the path of light?

4. Review Question
Why are all large astronomical telescopes built today reflectors and not refractors?

5. Review Question
What is the primary reason astronomers build large ground based telescopes?

6. Review Question
Why do astronomers wish to put telescopes in Earth orbit?

7. Age of the Solar System
The oldest rocks found on Earth are about 4.55 billion years old, not native but meteorites which fall from space.
The oldest Earth rocks are 3.85 billion years old.

8. Radioactive dating
Unstable parent isotopes decay at a constant rate to stable daughter isotopes. By measuring how much of the parent isotope is still present,
and how much of the daughter isotope there is, we can calculate the age of the rock.

9. Rubidium 187 Strontium 87 48800 Uranium 238 Lead 206 4470
parent
daughter
½ life (millions of years)
Rubidium 187
Strontium 87
48800
Uranium 238
Lead 206
4470
Plutonium 244
Thorium 232 83
Iodine 129
Xenon 129 16
Manganese 53
Chromium 53
3.7
Aluminum 26
Magnesium 26
0.72

10. Discussion
The age of a rock given by radiometric dating is the time since the rock last solidified.
What happens to the lighter daughter elements when the rock is in a molten or gaseous phase?

11. Formation of the Solar System
The nebular hypothesis
The Sun and planets formed from the gravitational collapse of a single, spherical, slowly rotating cloud of cold interstellar gas and dust.

12. Discussion
Why does the gas cloud need to be cold?

13. Consequence Planet formation is a natural outcome of star formation.
Planetary systems should be common.

14. Dynamics of the Planets
The planets revolve counterclockwise around the Sun as viewed from above the Sun’s north pole, the same direction that the Sun rotates on its axis.

16. Discussion
Why can’t the all the planets just orbit in any arbitrary direction? Why should they all go around the Sun in the same way?

17. 2. The major planets have orbital planes that are only slightly inclined with the plane of the equator of the Sun’s rotation, i.e. the orbits are coplanar.

18. Orbital inclination

19. Orbital Inclination Mercury 7.004 Venus 3.394 Earth Mars 1.85 Jupiter
Mars
1.85
Jupiter
1.308
Saturn
2.488
Uranus
0.774
Neptune
1.774

20. Discussion
What does this mean for the paths of the planets through the sky?

21. Discussion If the solar nebula started as a spherical cloud
why do all the planets lie in a plane above the Sun’s equator. Shouldn’t they be spherically distributed about the Sun?

22. Gravity can collapse a rotating cloud only along the axis of rotation.

23. Discussion
What two changes take place as the solar nebula collapses due to gravity?

27. Orion nebula HST

28. 3. The planets move in elliptical orbits that are very nearly circular.

29. Eccentricities Mercury 0.206 Venus .007 Earth .017 Mars .093 Jupiter
.048
Saturn
.056
Uranus
.046
Neptune
.010

30. Discussion Why are all the orbits nearly circular? What
happens to planets that formed with
highly eccentric (very elliptical) orbits?

32. 4. The planets rotate counterclockwise as viewed from above the north pole, the same direction as they revolve, except for Venus and Uranus.

33. Rotation of the Planets
Period (days)
Axis tilt
Mercury
58.6
0.0
Venus
-243.0
177.4
Earth
0.997
23.5
Mars
1.026
25.2
Jupiter
0.41
3.1
Saturn
0.43
26.7
Uranus
-0.72
97.9
Neptune
0.67
29.0

34. Discussion
Why do you think the planets rotate in the same direction and why is this direction in the same sense as the planets orbit the Sun?

35. Discussion
Unlike all the other planets Venus rotates backward. How would the diurnal and yearly motion of the Sun differ on Venus than on the Earth?

36. Discussion
Is the solar day longer or shorter than the sidereal day on Venus?

37. Discussion
Which planet will have the most extreme seasons?

38. 5. The Planets’ orbital distance from the Sun follows a regular spacing.
Titius-Bode rule
Write down 0, 3, 6, 12, … each number, after the first, being double the previous value. Add 4 to each and divide by 10.

39. Titius-Bode Rule and Distance
Distance AU
T-B distance AU
Mercury
0.39
0.4
Venus
.72
0.7
Earth
1.0
Mars
1.52
1.6
(Ceres)
2.77
2.8
Jupiter
5.2
Saturn
9.54
10.0
Uranus
19.18
19.6
Neptune
30.06
38.8

40. A packed Solar System?
The solar system may be as densely packed as possible. There do not appear to be any orbits stable over the lifetime of the solar system between the current planets.

41. 6. Most satellites revolve in the same direction as their parent planet’s rotation and lie close to their parent planet’s equatorial plane
An exception is Neptune’s Triton

42. Discussion
How would you explain this observation with our formation theory of the Solar System?

43. 7. The Sun contains 99. 8% of the solar systems mass but only 0
7. The Sun contains 99.8% of the solar systems mass but only 0.5% of the angular momentum

44. Discussion
If the Sun formed from a single spherical rotating cloud, wouldn’t you expect that all the pieces would have the same angular momentum as the original cloud? How must the solar system have changed since the time of its formation that this is no longer the case?

45. Discussion
Either the Sun’s rotation rate has slowed over time, or the planet’s have been spun up in the orbits. How could we decide between these two possibilities?

46. The Sun rotates once every 27 days, but should rotate once in about 2 hours if angular momentum were distributed evenly.
This two hour rotation rate is common among other young solar mass stars elsewhere in the galaxy as well as higher mass stars.

47. Slowing the Sun’s rotation
Magnetic breaking – The Sun’s magnetic field might interact with the early solar nebula to slow the Sun’s rotation.
Strong solar winds early in the history of the Sun might have carried the extra angular momentum away.

48. 8. Long period comets come from all directions and orbital inclinations in contrast to the coplanar orbits of the planets.

49. Discussion
If the long period comets can have any inclination, what does this tell you about their distribution around the Sun?

50. 2 types of planets
Terrestrial planets – iron-nickel cores and silicate mantles
Jovian planets – silicate/hydrogen compound (methane, ammonia, water) cores and mostly H and He mantles

51. Terrestrial & Jovian planets

52. Density Mass of the planet divided by the volume of the planet.
Higher density implies a larger percentage of high density materials, such as iron and nickel, lower density implies more silicates.

53. Mean density of planets
Neptune 1.6 g/cm3
Sun g/cm3
Jupiter g/cm3
Uranus g/cm3
Saturn g/cm3
Earth g/cm3
Mercury 5.4 g/cm3
Venus g/cm3
Mars g/cm3
Moon g/cm3

54. 9. Most solid planetary surfaces are heavily cratered

56. Meteor Crater (1.2 km)

57. Arizona from the Shuttle

58. 10. All the Jovian planets have rings and a large number of moons

59. 11. All the Jovian planets have a core of icy/rocky material with between times the mass of the Earth

60. 12. All planets are enriched with heavier elements in comparison with the solar abundances

61. The Planetesimal Hypothesis
Fluffy dust grains condensing out of the solar nebula stick together as a result of low-speed collisions, building up to small bodies called planetesimals.

64. Protoplanets
As the protoplanets grow by accretion of planetesimals, their gravity increases spurring more accretion.

65. Simulation

67. Solar nebula composition
We expect that the solar nebula from which the Sun formed, had the same composition as the current solar surface.
98% hydrogen and helium
1.4% hydrogen compounds – CH4, NH3, H2O
0.4% silicate rocks
0.2% metals

68. Discussion If the planets and Sun all formed from the
same nebula, why don’t all the planets and the
Sun of the same chemical composition?
The outer planets have about the same
composition as the Sun but the terrestrial
planets do not. Why?

71. Discussion
Can the Earth hold hydrogen and helium gas in its atmosphere? How do you know?

72. Discussion
Do you think any of the other terrestrial planets hold hydrogen and helium gas?

73. Discussion
Why do you think the cores of all the Jovian planets have a mass about 10 times the mass of the Earth?

74. Jovian Planets
Once at protoplanet reaches a mass of about 10 times that of the Earth, it can capture large amounts of gas directly from the solar nebular, becoming a Jovian planet.

75. Discussion
Why do you think Uranus and Neptune didn’t get as big as Jupiter and Saturn?

76. Doppler method for extra solar planet detection

77. Discussion
What planet characteristics (mass and distance from the star) will be easiest to find with the Doppler method? Explain your reasoning.

78. Extra Solar planets
Many extra-solar planets are Jupiter-like planets which lie very close to their star.

79. Planetary Migration
Most likely these hot Jupiters formed beyond the frost-line, but due to close encounters with other protoplanets lost orbital speed and spiraled in toward the star.