1. Introducing the Moon! A primer on lunar formation and evolution Lillian R. Ostrach 5 June 2012 A17 Se T LROC WAC, RGB = 689, 415, 320 nm [NASA/GSFC/ASU] 1

2. Earth Moon System Formation of Moon may have resulted in Earth’s axial tilt of 23.5° Moon stabilizes Earth’s axial tilt and thus stabilizes climate (Mars’ tilt varies 0-60°) Moon may have enhanced early melting and differentiation of Earth (much closer) Raises tides in oceans – influence on life? Lunar recession is lengthening our day over time Moon has influenced mythology, religion, arts (music, painting, writing) Earth 12,756 km Moon 3476 km 2

3. The Moon Day 27.3 Earth Days “Year” 27.3 Earth Days Near Side Far Side Dark Side Diameter ~1/4 Earth’s Gravity 1/6 Earth’s Moon’s mass 1% that of the Earth’s Earth to Moon 384,400 km (230,640 miles) Axis tilted ~1.5° Surface equivalent to area of Africa Earth 12,756 km Moon 3476 km And we’ve been there in person 9 times, 6 times on the surface! 3

4. Origin of the Moon: Classic Theories Co-accretion –Earth and Moon formed together from the nebula Capture –Moon formed elsewhere, then captured by Earth’s gravity Fission –Earth rotation so fast that a portion of Earth was thrown off Untestable hypotheses until lunar samples were returned 4

5. What do We Know? Angular momentum of Earth-Moon system very high –Moon’s orbit is not in the Earth’s plane of rotation –Moon’s spin axis differs grossly than the Earth’s Bulk composition –3.3 g/cc vs 5.5 g/cc (compressed) –Moon must be depleted in Fe –O isotopes between Earth Moon identical –Moon extremely depleted in volatiles Not completely, Mn What about CO and CO 2 ? –Moon enriched in refractory* elements, or is it? 5 *refractory elements = vaporizes or condenses at high temperatures; ex: Ca, Al, Ti

6. Testing the Models Post Apollo Moon: low density, O isotopes identical to Earth, depleted in volatiles, depleted in some siderophiles (Ni, Co), high angular momentum So how did the Moon form? 6

7. Giant Impact 7

8. Giant Impact Hypothesis Moon formed as Mars sized bolide hit proto-Earth Core of bolide became part of Earth, depleting proto-Moon of metallic iron Mantle and crust of bolide and part of Earth’s crust vaporized and went into orbit around Earth (lighter elements, volatiles boiled off into space) Consistent with Moon’s orbital configuration What about O isotopes? Bolide needed to form in nearly same orbit Density (5.5 vs. 3.3 g/cc) 8

9. Problem Solved? Giant Impact hypothesis has been around for >35 years…We need more samples! Moon does/did have some volatiles (vesicles, pyroclastic materials) Identical O isotopes (same place in Solar System) Small metallic core of Moon explained How well do samples represent the whole Moon? –Six Apollo locations all on central nearside (381.7 kg), three robotic Soviet locations (321 g) also nearside What about refractory elements? How well do we know the Moon? What do we need to do? Can we learn about Earth from further study of the Moon? 9

10. Breaking news! Titanium Isotopes Identicial for Earth and Moon! Titanium isotopes vary in other samples From impact hypothesis, would not expect isotopic ratios to be the same…equilibration? Models estimate 100 – 1000 years for lunar formation after impact New results do not disprove impact hypothesis! Another tool for continued testing of lunar formation by giant impact http://www.psrd.hawaii.edu/May12/Ti-isotopes-EarthMoon.html 10

11. How well do we know the Moon’s bulk composition? Not all that well! Recent papers giving very different results in terms of bulk lunar Al 2 O 3 (Longhi, 2006; Taylor et al, 2006) Longhi: Moon is not refractory enriched Taylor et al: The Moon is refractory enriched Both valid results from very different assumptions http://www.psrd.hawaii.edu/April07/Moon2Views.html Range of bulk lunar Al 2 O 3 found in various studies (diagram from J. Taylor). 11

12. Se T C FS Mv M A 12

13. Highlands (Terrae) Heavily cratered, thus overturned and mixed to 1 km or more Ancient ‘flotation’ crust Magma Ocean (Eu) –Anorthite floated –Olivines, pyroxenes sunk Anorthosites old as 4.5 Ga Mg-Suite Highlands Rocks until 4.3 Ga (ANT) –Anorthosite: Anorthite (An) –Troctolite: An + Olivine+ Pyroxene –Norite: An + Pyroxene KREEPy highlands rocks 4.35 Ga - end of primary crust formation KREEPy basalt 3.85 Ga (Ap 15 samples of Apennine Bench Formation) Does the bulk crust composition give insight to bulk lunar composition? KREEP = dregs of magma ocean 13

14. Lunar samples: Apollo 15 Genesis Rock, coarsely crystalline anorthosite dated at 4.1 derived locally (not 4.4 Ga, but probably formed at that time) Apollo 15 “Genesis Rock”, #15415 Time to do SCIENCE on the Moon! 14

15. Volcanic Plains Mare Basalts (Dark Areas) Formed after crust (bright areas) and most big impacts Erupted in vast quantities as a very fluid magma Flooded pre-existing topographic lows (craters) forming smooth plains Cover about 16% of lunar surface Very similar to basalts on the Earth (Deccan traps in India 65 Ma), watch basaltic rocks forming in Hawaii and Iceland Ages range from 3.1 to 3.8 Ga, some small fragments as old as 4.3 Ga Basaltic eruption in Hawaii, mixed pyroclastic and effusive 15

16. Mare Samples Mare basalt samples 3.1 to 3.8 Ga (but perhaps some much younger, 1-2 Ga???) 100s to >4000 m thick Nearly devoid of H 2 O, very depleted in other volatiles Some >10 wt % TiO 2 – Ti and O “resources” Refractory inventory (where is the Al? Lots of Ti) Complex mantle! Apollo 11 Basalt How do the mare fit into magma ocean story? (just wait a bit…) 16

17. Volcanic Beads Emplaced in explosive eruptions - fire fountains Many varieties, giving distinctive colors, some glasses, some crystalline Volcanic beads - important for volatile history (some do/did exist!); probably CO 2 CO main gases, traces of Zn, S, Pb...small amounts H 2 O Ap 15 green glass, Ap 17 orange glass... Shorty Crater Apollo 17 17

18. Lunar Mineralogy – The Basics Minerals are keys to understanding lunar rocks - compositions and atomic structures reflect formation conditions Lunar minerals are (essentially) anhydrous – ~ no water, no hydroxyl, no H!* Lunar minerals mostly formed at low pressure Lunar minerals formed under low oxygen fugacity (i.e., reducing conditions) Iron present as Fe 2+ or Fe 0 Ti present as Ti 4+ or Ti 3+ Cr present as Cr 3+ or Cr 2+ Terrestrial volcanics Lunar Basalts Slide courtesy of Brad Jolliff 18

19. Primary silicate minerals – just 3! Olivine (Mg,Fe) 2 SiO 4 (ss) forsteriteMg 2 SiO 4 fayaliteFe 2 SiO 4 Pyroxene (Mg,Fe,Ca) 2 SiO 6 (lmt’d ss) orthopyroxene(Mg,Fe) 2 Si 2 O 6 (enstatite, ferrosilite) clinopyroxene(Ca,Mg,Fe) 2 Si 2 O 6 (pigeonite, augite) Plagioclase NaAlSi 3 O 8 - CaAl 2 Si 2 O 8 (ss) anorthiteCaSi 2 Al 2 O 8 bytownite(Ca 1-x,Na x )Al 2-x Si 2+x O 8 Slide courtesy of Brad Jolliff 19

20. FeOMgO TiO 2 MgTi 2 O 5 MgTiO 3 Mg 2 TiO 4 FeTi 2 O 5 FeTiO 3 Fe 2 TiO 4 Armalcolite  In rocks w/ilmenite and armalcolite, armalcolite appears to have crystallized early, then reacted to form ilmenite  Textures indicate ulvöspinel also reacts (subsolidus reduction) to form ilmenite. Rutile: TiO 2 Tetrag. Armalcolite: (Fe,Mg)Ti 2 O 5 Orthorh. Ilmenite: FeTiO 3 Hexag. Ulvöspinel: Fe 2 TiO 4 Isom. (10 vol.% of some basalts; also contain Cr, Al, Mn, V) Main Ti-bearing Oxides on the Moon Slide courtesy of Brad Jolliff 20

21. KREEP and late-stage lunar minerals Potassium (K), Rare Earth Elements (REE), and Phosphorous (P) Elements that are excluded from the major rock-forming minerals Late-stage assemblages - rich in phosphates and K-feldspar (indicators!) Also elements such as Ba, Rb, Cs, Zr, Hf, Nb, Ta, U, and Th Formed as residue of low-pressure magma crystallization (last stuff) Incompatible elements: Cations are large and/or highly charged, don’t fit well into crystallographic sites occupied by Fe, Mg, and Ca – cause distortion if allowed Slide courtesy of Brad Jolliff 21

22. Quick Peek: Lunar Differentiation & Magma Ocean Eu Anomaly (REE see periodic table) Eu: Same size and charge as Ca so it substitutes easily in anorthite (feldspar) Early lunar crust enriched in Eu, later basalts deficient Bottom Line: Came from same source - MAGMA OCEAN We can ‘see’ that basalts are younger 22

23. Apollo 11 Soil Landing site in lunar maria (where?) Diverse components ­ Dark: Basalt (volcanic) ­ Light: Plagioclase-rich ­ Breccias (mixed rocks) ­ Glasses: Volcanic Impact How did the anorthosite get there? Fig. 1, Wood et al., 1970 23

24. Explaining Anorthosite Grains at Apollo 11 Wood et al., 1970 24

25. Magma Ocean Theory: The Basics As magma ocean cools, anorthosite floats, olivine, ilmenite, and pyroxene sink Early crust enriched in Ca and Al, depleted in Fe and Mg Secondary crust formation in terms of intrusions and extrusions of denser Fe and Mg rich magmas Is the magma ocean, flotation crust, dense minerals sinking, etc., a done deal? http://www.psrd.hawaii.edu/ Magma ocean, magma seas, or something else? 25

26. Formation of the Earliest Crust, 1 Fig. 2.5c, Lunar Sourcebook 26

27. Formation of the Earliest Crust Slide courtesy of Brad Jolliff What is going on? 1) Large-scale convection of MO? *overturn!* at least locally (Fe/Ti-rich mins, KREEPy stuff) 2) Partial melting near base of “crust”  intrusions 3) KREEPy pockets near base of “crust”, mixed with intrusions 27

28. Time to Solidify an Ocean of Magma 72215: impact melt breccia; high incompatibles – late-stage crystallization A single zircon in 72215 shows a range of ages: oldest cluster dated at 4.417 Ga Suggests that MO significantly crystallized by this time 28 http://www.psrd.hawaii.edu/Mar09/magmaOceanSolidification.html

29. (Some) Problems with the Magma Ocean Hypothesis Problem: energy source to melt Moon, create global magma ocean Solution: rapid accretion (giant impact); otherwise – no realistic clue Problem: “layer cake” cumulate pile indicates that mare basalt types are related to depth (but exps show deep source >300 km); similarity in Mg# among VLT- low-high Ti-basalts Solution: large-scale (global?) overturn resulting from gravitational instabilities in the cumulate pile (more dense rocks overlying less dense)  “well-stirred” LMO with mixing (heterogeneous mantle!) Problem: overlapping ages of FAN and Mg-suite rocks AND different trace elemental abundances Solution: LMO probably mostly crystallized when Mg-suite rocks formed but last pockets of FAN melt still present; the two rocks not simply related/from the same parent magma 29

30. Fig. 2.5e, Lunar Sourcebook, after Walker, 1983 30

31. Fig. 12, 13 from Jolliff et al., 2000 31

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