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Origin of the Moon

Origin of the Moon. 12 February 2019. Why study the origin of the moon?. How terrestrial planets form: they build up from impacts between smaller objects Moon effects on Earth: tides, change Earth spin Pluto ’ s moons likely formed the same way, from a giant impact on Pluto.

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Origin of the Moon

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  1. Origin of the Moon • 12 February 2019

  2. Why study the origin of the moon? • How terrestrial planets form: they build up from impacts between smaller objects • Moon effects on Earth: tides, change Earth spin • Pluto’s moons likely formed the same way, from a giant impact on Pluto

  3. The Yutu-2 rover has accumulated 120 meters of driving on the lunar surface, surpassing the 114 meters of roving managed by the 2013 Chang’e-3 mission rover Yutu (“Jade Rabbit”) before it became immobilized in its second lunar daytime. The previous lunar night saw the Chang’e-4 lander record a temperature low of -190 degrees Celsius (-310 Fahrenheit), with measurements made possible by a Russian-developed radioisotope thermoelectric generator which also acts as a prototype for future deep-space exploration.

  4. LRO view of Chang’e-4 Lander & Rover

  5. Effects of Moon on Earth: Tides Obliquity stabilized Day and month changes Why study the origin of the moon?

  6. terrestrial planets formation • Disk of gas and dust around Sun • Interparticle collisions: if impact velocities are low enough, we get gravitationally bound aggregates • 10,000 yrs: 10 km-sized bodies • 100,000 yrs: Moon-Mars sized (~2000 km, ~20 “embryos”) • 1 million-10 million yrs: planet-sized “giant impacts” will reduce number of embryos to 4 terrestrial planets

  7. Big Muley

  8. Evidence for giant impacts • Planets spin faster than they orbit • Planets are tilted to orbital revolution

  9. Moon Properties • Name some of the distinguishing properties of the Moon…

  10. Moon Properties • Earth has only 1 Moon • Depleted in Fe and volatiles; • Oxygen isotopes similar to Earth • Moon’s orbit: • is not in Earth’s equatorial plane • Circular • Expanding due to tidal interaction • Moon has very small core

  11. Lunar Far Side

  12. Moon Origin Hypotheses • Co-accretion: Earth and Moon formed together. Like sister • Fission: Earth spun so fast that it split off a Moon-sized chunk. Like daughter • Capture: Earth captured an independently-formed Moon as it passed by. Like wife. • THESE WERE THE 3 HYPOTHESES BEFORE APOLLO! • Giant Impact: Mars-sized body collided with proto-Earth and excavated material eventually coalesced to form Moon

  13. Evaluate the Hypotheses Co-accretion: Moon has little iron, volatiles. Fission: Earth never spun fast enough Capture: too unlikely AFTER APOLLO WE STILL HAD THE SAME THREE POSSIBILITIES

  14. Giant Impact Stages • both differentiated • both formed near 1 AU • Earth close to final size • Mars-sized impactor

  15. Where does Iron go?

  16. Where does Iron go? • Both Fe cores stay with Earth • 1 lunar mass in orbit outside Roche radius • Moon is mostly impactor material

  17. How hot is the Impact? • heat removes volatiles from debris disk

  18. Evolution of the Protolunar disk • Centrally condensed hot disk <a> = 2.5-3REarth • Cooling: condensation/solidification • Collisional spreading of disk • Accretional growth of moonlets • Tidal evolution of moonlets • Collisions between moonlets yield moon

  19. Moon Video • https://www.youtube.com/watch?v=PnhflL7-I3I

  20. the post-impact moon • Impact: Mars-sized body collides with Earth • Debris ejected into Earth orbit • A. heated • B. comes from mantle (no Fe) • C. ~1 lunar mass = ~1% Earth mass = ~10% impactor mass • Debris accumulates to form one large Moon, not multiple small moons… but maybe a second, smaller moon hits it later

  21. ReAccretion & the post-impact moon • Earth spin and Moon orbit locked • Moon orbit expands a few cm/yr • Earth rotation slows: conservation of angular momentum

  22. The giant-impact hypothesis, sometimes called the Big Splash, or the Theia Impact suggests that the Moon formed out of the debris left over from a collision between Earth and an astronomical body the size of Mars, approximately 4.5 billion years ago; about 20 to 100 million years after the solar system coalesced.The colliding body is sometimes called Theia, from the name of the mythical Greek Titan who was the mother of Selene, the goddess of the Moon.[Analysis of lunar rocks, published in a 2016 report, suggests that the impact may have been a direct hit, causing a thorough mixing of both parent bodies

  23. The newly formed Moon orbited at about one-tenth the distance that it does today, and spiraled outward because of tidal friction transferring angular momentum from the rotations of both bodies to the Moon's orbital motion. Along the way, the Moon's rotation became tidally locked to Earth, so that one side of the Moon continually faces toward Earth. Also, the Moon would have collided with and incorporated any small pre-existing satellites of Earth, which would have shared the Earth's composition, including isotopic abundances. The geology of the Moon has since been more independent of the Earth. Although this hypothesis explains many aspects of the Earth–Moon system, there are still a few unresolved problems, such as the Moon's volatile elements not being as depleted as expected from such an energetic impact.

  24. Computer simulations show a need for a glancing blow, which causes a portion of the collider to form a long arm of material that then shears off. The asymmetrical shape of the Earth following the collision then causes this material to settle into an orbit around the main mass. The energy involved in this collision is impressive: possibly trillions of tons of material would have been vaporized and melted. In parts of the Earth, the temperature would have risen to 10,000 °C (18,000 °F). The Moon's relatively small iron core is explained by Theia's core accreting into that of Earth. The lack of volatiles in the lunar samples is also explained in part by the energy of the collision. The energy liberated during the re-accretion of material in orbit around Earth would have been sufficient to melt a large portion of the Moon, leading to the generation of a magma ocean.

  25. ReAccretion & the post-impact moon • In the past, which is a possible state of the Earth/Moon system? • A. Moon orbits closer in, Earth’s day is 18 hours • B. Moon orbits farther away, Earth’s day is 36 hours • C. Moon orbits closer in, Earth day is same as now • D. Same conditions as today

  26. ReAccretion & the post-impact moon • In the past, which is a possible state of the Earth/Moon system? • A. Moon orbits closer in, Earth’s day is 18 hours • B. Moon orbits farther away, Earth’s day is 36 hours • C. Moon orbits closer in, Earth day is same as now • D. Same conditions as today

  27. The giant-impact hypothesis is currently the favored scientific hypothesis for the formation of the Moon. Supporting evidence includes: • Earth's spin and the Moon's orbit have similar orientations. • Moon samples indicate that the Moon’s surface was once molten.  • The Moon has a relatively small iron core. • The Moon has a lower density than Earth. • Evidence exists of similar collisions in other star systems. • Giant collisions are consistent with the leading theories of the formation of Solar Systems. • The stable-isotope ratios of lunar and terrestrial rock are identical, implying a common origin

  28. Summary • Apollo mission had the scientific objective to discover the origin of the Moon • It did not, but Apollo results were key in developing later models • The Moon is not the sister, daughter or wife of Earth • Instead, it was created form a giant collision: the Big Splash, when Earth was struck by a Mars-sized object

  29. Kepler-107 is about 1,714 light years away, in the direction to our constellation Cygnus. The study focuses on the two innermost planets orbiting Kepler-107 (out of four known to exist). They are similar to each other in terms of both radii  and orbital periods – their sizes are 1.536 and 1.597 Earth-radii, respectively, with an uncertainty of only about 0.2 percent. Their years  are 3.18 and 4.90 days, respectively.  When it comes to their densities, however, these two exoworlds are quite different – 5.3 and 12.65 grams per cubic centimeter, respectively. Earth’s density is 5.5 grams per cubic centimeter, for comparison, while water is only 1 gram per cubic centimeter. So – although their sizes and orbits are similar – one of these worlds is much, much denser than the other.

  30. Colliding exoplanets • https://earthsky.org/space/2-colliding-exoplanets-kepler-107-system

  31. Discussion • Was Apollo worth it? • What could have improved its return?

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