1. Brief
Summary

2. Three outstanding issues:
Outer Jovian planets may not have had enough time to formed in their current locations
Rocks returned by astronauts from the heavily cratered lunar highlands are ~ 3.9 million yrs old – younger than solar system
There were no icy planetesimals in the inner solar system. Where did the Earth’s water come from?

3. Solution? Late Heavy Bombardment (LHB)
All Jovians planets formed in orbits closer to that of Jupiter
Orbital resonances between Jupiter and Saturn caused outer Jovians to move suddenly to larger orbits
Uranus and Neptune interacted with Kuiper Belt objects, scattering large numbers of them into the inner solar system
This lead to heavy bombardment & delivery of ices to Terrestrial planets.

4. The oldest biological markers known to scientists date precisely to the end of the LHB.

5. WE NOW UNDERSTAND HOW THE LOCATIONS AVAILABLE FOR LIFE WERE FORMED.
NOW, WHAT ARE THE REQUIREMENTS FOR LIFE?

6. Life depends critically on environment
Life depends critically on environment. We will examine how life-friendly environments can form in the universe.
Fundamentals:
Temperature Liquids (particularly H2O) Sources of Energy Chemical environment Radiation environment

7. interiors surfaces atmospheres
What determines the environments of terrestrial-like planets? A look at: (much of what follows also applies to Jovian planets & moons)
interiors surfaces atmospheres

8. Terrestrial planets are mostly made of rocky materials (with some metals) that can deform and flow.
Likewise, the larger moons of the Jovian planets are made largely of icy materials (with some rocks and metals) that can deform and flow.
The ability to deform and flow has many consequences.

9. Weight of mountain is determined by its mass & the strength of the gravitational acceleration,
Fg = mg
If this force exceeds the ability of the underlying rock/ice to support it, the mountain will sink into the crust.
weight of mountain
The ability to deform and flow leads every object with diameters greater than a few hundred km to become spherical under the influence of gravity.

10. The ability to deform and flow also created structure in the interiors of planets

11. Early in their existence, the Terrestrial planets and the large moons had an extended period when they were mostly molten.
The heating that led to this condition was caused by impacts, where the kinetic energy of the impacting material was converted to thermal energy.
Today, the interiors of planets are heated mainly by radioactive decay.

12. Differentiation – the process by which gravity separates materials according to their densities
Denser materials sink, less dense material “float” towards top

13. This created density layers: core, mantle, crust
DIFFERENTIATION: During the time when interiors were molten, denser material sank towards the center of a planet/moon while less dense material “floated” towards top.
This created density layers: core, mantle, crust

14. Earth (solid inner, molten outer core)
Terrestrial planets have metallic cores (which may or may not be molten) & rocky mantles
Earth (solid inner, molten outer core)
Mercury (solid core)
Earth’s interior structure

15. Differentiated Jovian moons have rocky cores & icy mantlesIo
Europa
Ganymeade
Callisto

16. Interior structure of the Terrestrial planets:

17. The Lithosphere…
Layer of rigid rock (crust plus upper mantle) that floats on softer (mantle) rock below
While interior rock is mostly solid, at high pressures stresses can cause rock to deform and flow (think of silly putty)
This is why we have spherical planets/moons

18. Larger planets take longer to cool, and thus:
The interiors of the terrestrial planets slowly cool as their heat escapes.
Interior cooling gradually makes the lithosphere thicker and moves molten rocks deeper.
Larger planets take longer to cool, and thus:
1) retain molten cores longer
2) have thinner (weaker) lithospheres

19. Geological activity is driven by the thermal energy of the interior of the planet/moon
The stronger (thicker) the lithosphere, the less geological activity the planet exhibits.
Planets with cooler interiors have thicker lithospheres!

20. Earth has lots of geological activity today, as does Venus
Earth has lots of geological activity today, as does Venus. Mars, Mercury and the Moon have little to no geological activity (today)
This has important repercussions for life:
Outgassing: produces atmosphere
Magnetic fields (need molten cores): protect planet surface from high energy particles from a stellar wind.

21. Larger planets stay hot longer.
Earth and Venus (larger) have continued to cool over the lifetime of the solar system  thin lithosphere, lots of geological activity
Mercury, Mars and Moon (smaller) have cooled earlier  thicker lithospheres, little to no geological activity

22. Initially, accretion provided the dominant source of heating.
Very early in a terrestrial planet’s life, it is largely molten (differentiation takes place).
Today, the high temperatures inside the planets are due to residual heat of formation and radioactive decay heating.

23. Stresses in the lithosphere lead to “geological activity” (e. g
Stresses in the lithosphere lead to “geological activity” (e.g., volcanoes, mountains, earthquakes, rifts, …) and, through outgassing, leads to the formation and maintenance of atmospheres.
Cooling of planetary interiors (energy transported from the planetary interior to the surface) creates these stresses
Convection is the main cooling process for planets with warm interiors.

24. Convection - the transfer of thermal energy in which hot material expands and rises while cooler material contracts and falls (e.g., boiling water).

25. Convection is the main cooling process for planets with warm interiors.

27. Side effect of hot interiors - global planetary magnetic fields
Requirements:
Interior region of electrically conducting fluid (e.g., molten iron, salty water)
Convection in this fluid layer
“rapid” rotation of planet/moon

28. Earth fits requirements
Venus rotates too slowly
Mercury, Mars & the Moon lack molten metallic cores
Sun has strong field

29. Planetary Surfaces 4 major processes affect planetary surfaces:
Impact cratering – from collisions with asteroids and comets
Volcanism – eruption of molten rocks
Tectonics – disruption of a planet's surface by internal stresses
Erosion – wearing down or building up geological feature by wind, water, ice, etc.

30. Impact Cratering: The most common geological process shaping the surfaces of rigid objects in the solar system (Terrestrial planets, moon, asteroids)

31. Volcanism
Volcanoes help erase impact craters

32. Volcanic outgassing: source of atmospheres and a source of water

33. Erosion: the breakdown and transport of rocks and soil by an atmosphere.
Wind, rain, rivers, glaciers contribute to erosion.
Erosion can build new formations: sand dunes, river deltas, deep valleys).
Erosion is significant only on planets with substantial atmospheres.

34. Tectonics: refers to the action of internal forces and stresses on the lithosphere to create surface features.
Tectonics can only occur on planets or moons with convection in the mantle
Earth & Venus
Jupiter’s moons Europa & Ganymede?

35. Tectonics…
raises mountains
creates huge valleys (rifts) and cliffs
creates new crust
moves large segments of the lithosphere (plate tectonics)

37. Portion of Valles Marineris on Mars – created by tectonic stresses

38. Tectonic plates

40. divergent plate boundary (plates move away from each other).
Atlantic Ocean
Great Rift Valley in Africa
Valles Marineris (Mars)

41. Portion of Valles Marineris on Mars – created by tectonic stresses

42. convergent plate boundary with subduction : plates move towards each other & one slides beneath the other.
Nazca plate being subducted under the South American plate to form the Andes Mountain Chain.
Island arc system

43. convergent plate boundary without subduction : plates move towards each other and compress.
Formation of Himalayas.

44. Plates sliding past each other: earthquakes, valleys, mountain building

45. Half of the world’s volcanoes surround the Pacific plate
Tectonic plates