1. Earth-rise on Moon

2. The Moon

3. A12 A14 A15 A17 A11 A16 L24 L20 L16 Apollo and Luna Landing Sites

4. Lunar Surface – Sandy and Rocky

5. The Moon: Some Factoids Lunar exploration: Luna series (USSR), Surveyor (US) unmanned missions Apollo manned missions explored geology Density = 3.34 g/cc ; composition? D (Earth, Mercury,Venus) = 5.52, 5.43, 5.24 g/cc  Composition? Basic surface and interior similar to rocky part of the Earth (little or no metallic core or magnetic field)

6. Highlands and Marias Highlands were heavily cratered during the early history, from formation to about 4 billion years ago Marias (dried up lava oceans) formed later, about 3 billion years ago

7. Cratered Highlands and Marias Highlands are much older than marias. Why?

8. Evolution of highlands and maria

9. Craters and chronology (age) Highlands are highly cratered regions that must be older than smoother regions of surface since most cratering activity was at the time of the formation of the solar system Marias are much younger, and evolved later at places where large crater impact basins were formed and filled with lava from the interior

10. Atmospheres and Surfaces Lack of atmosphere - results in extreme temperatures - exposes surface to meteoroid impact  craters - lack of current geological activity and evolution (ceased long time ago) Moon and Mercury lack atmosphere (too small and too close to the Sun) Both have similar surface geology  craters and marias

11. Formation of a lunar sea: Impact of meteoroid  Impact Basin  Filled with Lava  Maria

12. A Mare

13. Maria – Lightly cratered smooth surface

14. Lava River

15. Lunar Geology

16. Formation of Moon No generally accepted theory: three scenarios - Accretion - Fission (breakup) - Capture Possibly a combination

17. Formation of Moon

18. Earth Tides on Moon Tidal forces due to the Earth forced the Moon to rotate at the same rate as Its revolution; therefore it keeps the same face towards the Earth

19. Another view of Moon ? And, Mercury !

20. Cratered highlands of Mercury

22. Mercury – Basic Statistics Mass ~ 1/20 Earth’s Diameter ~ 1/3 “ Density ~ 5.5 g/cc Year ~ 88 Earth days Day ~ 59 “ 0.4 AU from the Sun Surface T: Day  700 F, Night  -300F

23. Mariner Fly-By’s Several orbital reconnaissance satellites, but no space probes landed yet

24. Mariner Fly-By Picture Mosaic

25. Best Mercury Sighting at Maximum Western Elongation Eccentric orbit implies different maximum angles

26. Greatest Elongations of Mercury Optimum Mercury Sighting at Maximum Elongation, and/or just after sunset or before sunrise NOT easily seen, like Venus as “evening star”: Mercury is too small, too close to the Sun, and lacks atmosphere and hence has small albedo

28. Mercury – Basic Features Metal ball (mostly iron) surrounded by heavily cratered rocky crust like Moon But weak magnetic field, why? No molten, moving core! Only refractory elements; volatile elements evaporated Geology like the Moon, e.g. Caloris basin resembles lunar maria – large crater impact basin flooded later with lava No Plate Tectonics, why?

29. Interiors of Earth and Mercury

30. Dopper Radar measurement of rotation speed of Mercury

31. Aracebo Radio Telescope(Puerto Rico)

32. A “Day” on Mercury A year is the period of revolution (orbit) around the Sun Two kinds of “day” on a planet: Sidereal and Solar Sidereal day is the actual period of rotation on its axis (viewed with respect to the stars, not the Sun) Solar day is the period of rotation with respect to the Sun On the earth: solar day = 24 hrs, longer than sidereal day by 4 mins. Mercury’s sidereal day is 2/3 of a Mercury year

33. Rotation and Revolution of Mercury: Day and Year Rotation period ~ 2/3 revolution period A solar day is twice as long as a year !! Solar Day (176 d) = 2 x Sidereal year (88 d) Wait two years to see the sun in the same place in the sky (on the earth it is just 1 solar day, or 1 sidereal day + 4 mins) What’s going on?

34. Rotation and Revolution of Mercury Strong Tides due to Sun Periods of Mercury A solar day on Mercury is twice as long as the sidereal year Like the Moon Moon’s rotation period equals orbital period: see only one side or face of Moon

35. Hot Poles on the Equator ! Perihelion of Mercury is 1.5 times closer than aphelion Mercury receives 2.25 times more solar energy at perihelion than at aphelion Two extremities of the equator pointing towards the sun constitute two hot ‘thermal’ poles Largest variation in temperature between day/night, but maximum temperature ~700 F is still less hot than Venus (> 800 F)