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  1. H205Cosmic Origins • Today: Forming the Solar System • Finish EP6 APOD

  2. The Origin of the Solar System • All objects in the Solar System seem to have formed at nearly the same time, out of the same original cloud of gas and dust • Radioactive dating of rocks from the Earth, Moon, and some asteroids suggests an age of about 4.5 billion yrs • A similar age is found for the Sun based on current observations and nuclear reaction rates

  3. A theory of the Solar System’s formation must account for what we observe: • Planets orbit in the same direction and in the same plane • Two families of planets: terrestrial & Jovian • Compositions of planets • Ages 4.5 billion years (or less) • Other details – structure of asteroids, cratering of planetary surfaces, detailed chemical composition of surface rocks and atmospheres, etc.

  4. The Solar Nebula Hypothesis • Derived from 18th century ideas of Laplace and Kant • Proposes that Solar System evolved from a rotating, flattened disk of gas and dust (an interstellar cloud), the outer part of the disk becoming the planets and the inner part becoming the Sun

  5. Explains the Solar System’s flatness and the common direction of motion of the planets around the Sun Interstellar clouds are common between the stars in our galaxy and this suggests that most stars may have planets around them The Solar Nebula Hypothesis

  6. Interstellar Clouds • The cloud that formed Solar System was probably a few light years in diameter and 2 solar masses • Typical clouds are 71% hydrogen, 27% helium, and traces of the other elements

  7. Interstellar Dust • Clouds also contain tiny dust particles called interstellar grains • Grain size from large molecules to a few micrometers • They are a mixture of silicates, iron and carbon compounds, and water ice Dust grains are very small - about 4000 could fit across a sucker stick

  8. In the Beginning… • Triggered by a collision with another cloud or a nearby exploding star, rotation forces clouds to gravitationally collapse into a rotating disk

  9. The Solar Nebula • Over a few million years the cloud collapses into a rotating disk with a bulge in the center • This disk, about 200 AU across and 10 AU thick, is called the solar nebula • The bulge becomes the Sun and the disk condenses into planets

  10. Temperatures in the Solar Nebula • Before the planets formed, the inner part of the disk was hot, heated by gas falling onto the disk and a young Sun – the outer disk was colder than the freezing point of water Astronomers have observed many gas/dust disks where planets may be forming

  11. Condensationoccurs when gas cools below a critical temperature at a given gas pressure Gas molecules bind together to form liquid or solid particles On Earth, water vapor condenses to form clouds Steam condenses on the bathroom mirror Condensation

  12. Condensation in the Solar Nebula • Iron vapor condenses at 1300 K, silicates condense at 1200 K, and water vapor condenses at room temperature • In a mixture of gases, materials with the highest vaporization temperature condense first • The Sun kept the inner solar nebula (out to almost Jupiter’s orbit) too hot for anything but iron and silicate materials to condense • The outer solar nebula cold enough for ice to condense

  13. The Formation of the Planets

  14. Grains stick together • Next step is for the tiny particles to stick together, perhaps by electrical forces, into bigger pieces in a process called accretion • As long as collisions are not too violent, accretion leads to objects, called planetesimals, ranging in size from millimeters to kilometers

  15. Planetesimals • Planetesimals in the inner solar nebula were rocky-iron composites, while planetesimals in the outer solar nebula were icy-rocky-iron composites • Planets formed from “gentle” collisions of the planetesimals, which dominated over more violent shattering collisions

  16. Formation of the Planets • Simulations show that planetesimal collisions gradually lead to approximately circular planetary orbits • As planetesimals grew in size and mass their increased gravitational attraction helped them grow faster into clumps and rings surrounding the Sun

  17. Formation of the Planets • Planet growth was especially fast in the outer solar nebula due to: • Larger volume of material to draw upon • Larger objects (bigger than Earth) could start gravitationally capturing gases like H and He

  18. Craters Everywhere! • Continued planetesimal bombardment and internal radioactivity melted the planets and led to the density differentiation of planetary interiors

  19. Formation of Moons • Moons of the outer planets were probably formed from planetesimals orbiting the growing planets • Not large enough to capture H or He, the outer moons are mainly rock and ice giving them solid surfaces

  20. Where did OUR Moon come from??? Lunar Formation Before Apollo • Three hypotheses for the Moon’s origin: • Co-Accretion Theory • Capture Theory • Fission Theory The Spongmonkies: We Like The Moon

  21. The Earth-Moon System It’s the little dot inside! • The Moon’s diameter is ¼ of the Earth’s • The Moon’s surface is very dark, like a charcoal briquet • The Moon’s mass is 1/80th of the Earth’s • The Moon has no atmosphere

  22. Something’s Different… • Unlike most of the other moons in the solar system, the Moon is very large relative to its central planet • These oddities indicate that the Moon formed differently from the other solar system moons!

  23. Earth and Moon by Richard Swarts

  24. Co-Accretion Theory • Earth and Moon were twins, forming side by side from a common cloud of gas and dust

  25. Capture Theory • Moon was originally a small planet orbiting the Sun and was subsequently captured by Earth’s gravity during a close approach

  26. Fission Theory • The Moon spun out of a very fast rotating Earth in the early days of the Solar System

  27. One small step for man, one giant leap for mankind Moon Rocks!

  28. Hypotheses Failed! • Each of these hypotheses gave different predictions about Moon’s composition: • In capture theory, the Moon and Earth would be very different in composition, while twin theory would require they have the same composition • In fission theory, the Moon’s composition should be close to the Earth’s crust • Moon rock samples proved surprising • For some elements, the composition was the same, but for others, it was very different • None of the three hypotheses could explain these observations

  29. So Where Did the Moon Come From? • Did the Earth and Moon form together as a binary system? • NO… • Did the Earth capture the Moon after both were already formed? • NO… • Did the early Earth break apart into the Earth-Moon system? • NO… • What do the Moon rocks tell us? • The Moon was formed from the Earth’s crust

  30. What Is the Earth Made of? • The Earth is made of many chemical elements • Iron, Silicon, Magnesium, Oxygen, Carbon • And water! Earth rocks contain water!

  31. What’s Inside the Earth? • The chemical elements on Earth are separated (Earth is differentiated!) • Iron and nickel in the core • Lighter elements in the mantle and crust

  32. What about the MOON? • What is it made of? • Where did it come from? It’s not green cheese!

  33. What’s Inside the Moon? Maybe there is a tiny iron core inside • The Moon has a TINY iron core • The Moon does not appear to be as differentiated as the Earth

  34. What Have We Learned from Moon Rocks? • The composition of moon rocks is very similar to the composition of the Earth’s crust But, unlike the Earth, the Moon has very little iron And Moon rocks are dry!

  35. Giant Impact Theory • Does it work? • It sounds like science fiction!

  36. The Large Impact Hypothesis • Moon formed from debris blasted out of the Earth by the impact of a Mars-sized body • Age of lunar rocks and lack of impact site on Earth suggests collision occurred at least 4.5 billion years ago

  37. Impact Theory • A large body, about the size of Mars impacts the early Earth Told through the art of William Hartmann

  38. The collision blasts material from the Earth’s crust into space

  39. The material forms a disk around the Earth

  40. Material in the disk coalesces to form the Moon

  41. The early Moon is hot from the heat of accretion

  42. The Large Impact Solution • This “large impact” idea explains: • The impact would vaporize low-melting-point materials (e.g., water) and disperse them explaining their lack in the Moon • Only surface rock blasted out of Earth leaving Earth’s core intact and little iron in the Moon • Easily explains composition similarities and differences with Earth • The splashed-out rocks that would make the Moon would more naturally lie near the ecliptic than the Earth’s equatorial plane – explains why the plane of the Moon’s orbit is not the Earth’s equatorial plane • Explains Earth’s tilted rotation axis

  43. What Happened to the Moon’s Iron? The Earth gobbled it!

  44. Forming the Moon We See Today • As Moon’s surface solidified, stray fragments from original collision created craters that blanket highlands • A few of the larger fragments created the large basins for the maria to form • By the time the maria filled with molten material and solidified, little material was left for further lunar bombardment – thus the smooth nature of the maria

  45. Highlands and Mare

  46. The Early Moon • When the Moon formed it was much closer to the Earth • The Moon is moving away from the Earth at about 2 inches per year • The day and the month were originally much shorter than they are today • Tides were originally much greater

  47. Leftovers of the Solar System • Asteroids and comets are remnants of the formation of the Solar System • Some may be planetesimals • Best source of information about the Solar System’s early years • Asteroids and comets play a central role in planetary impact and in particular can have a large influence on Earth’s biological life

  48. Asteroids • Asteroids are small, generally rocky bodies that orbit Sun • Most asteroids (thousands) lie in the asteroid belt, a region between the orbits of Mars and Jupiter • The combined mass of all the asteroids is probably less than 1/1000 the mass of the Earth Asteroid Gaspara, image from Galileo spacecraft

  49. The Asteroid Belt