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Chapter 15 The Formation of Planetary Systems
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Chapter 15 The Formation of Planetary Systems

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  1. Chapter 15The Formation of Planetary Systems

  2. Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Terrestrial and Jovian Planets 15.3 Interplanetary Debris 15.4 Solar System Regularities and Irregularities 15.5 Searching for Extrasolar Planets 15.6 Properties of Exoplanets 15.7 Is Our Solar System Unusual?

  3. 15.1 Modeling Planet Formation • Any model must explain • Planets are relatively isolated in space • Planetary orbits are nearly circular • Planetary orbits all lie in (nearly) the same plane • Direction of orbital motion is the same as direction of Sun’s rotation • Direction of most planets’ rotation is also the same as the Sun’s

  4. 6. Most moons’ orbits are also in the same sense 7. Solar system is highly differentiated 8. Asteroids are very old, and not like either inner or outer planets 9. Kuiper belt, asteroid-sized icy bodies beyond the orbit of Neptune 10. Oort cloud is similar to Kuiper belt in composition, but farther out and with random orbits

  5. Solar system is evidently not a random assemblage, but has a single origin. Planetary condensation theory, first discussed in Chapter 6, seems to work well. Lots of room for variation; there are also irregularities (Uranus’s axial tilt, Venus’s retrograde rotation, etc.) that must be allowed for by the model.

  6. Condensation theory: • Large interstellar cloud of gas and dust starts to contract, heating as it does so • Sun forms in center; dust provides condensation nuclei, around which planets form • As planets grow, they sweep up smaller debris near them

  7. 15.2 Terrestrial and Jovian Planets Terrestrial (rocky) planets formed near Sun, due to high temperature—nothing else could condense there.

  8. T Tauri stars are in a highly active phase of their evolution and have strong solar winds. These winds sweep away the gas disk, leaving the planetesimals and gas giants.

  9. Jovian planets: • Once they were large enough, may have captured gas from the contracting nebula • Or may not have formed from accretion at all, but directly from instabilities in the outer, cool regions of the nebula

  10. Detailed information about the cores of jovian planets should help us distinguish between the two possibilities. Also possible: The jovian planets may have formed farther from the Sun and “migrated” inward.

  11. Any theory of the origin of the solar system must explain all of these EXCEPT the orbits of the planets are nearly circular, and in the same plane. the direction that planets orbit the Sun is opposite to the Sun’s spin. the terrestrial planets have higher density and lower mass. comets do not necessarily orbit in the plane of the solar system.

  12. What is the name of the theory that is currently used to describe the formation of the solar system? perturbation theory condensation theory differentiation theory close-encounter theory

  13. The condensation sequence theory explains why our planet Earth has water and rain. stars are more likely to form large planets orbiting very near. terrestrial planets are different from jovianplanets. the Moon formed near the Earth. Pluto has such a circular orbit.

  14. The ________ theory would have the jovians growing quickly into giants after forming directly from the outer solar nebula. large impact core-accretion gravitational instability Perturbation Oortcloud

  15. Why did a major planet not form out in the Kuiper belt? One did, and its name is Pluto. Some may have, but they have since migrated to orbits nearer the Sun. Sednadisrupted objects closer to the Sun. Comets bombarded these bodies violently, breaking them apart. It was not in the ecliptic like the planets; there was no material out there.

  16. Compared to the formation of the terrestrial planets, Jupiter may have formed at a much higher temperature. condensed gravitationally rather than by accretion. condensed with mostly metallic materials. required a much longer time to form. not followed the condensation sequence at all.

  17. 15.3 Interplanetary Debris • Asteroid belt: • Orbits mostly between Mars and Jupiter • Jupiter’s gravity kept them from condensing into a planet, or accreting onto an existing one • Fragments left over from the initial formation of the solar system

  18. General timeline of solar system formation

  19. Icy planetesimals far from the Sun were ejected into distant orbits by gravitational interaction with the jovian planets, into the Kuiper belt and the Oort cloud. Some were left with extremely eccentric orbits and appear in the inner solar system as comets.

  20. Kuiper belt objects have been detected from Earth; a few are as large as, or larger than, Pluto, and their composition appears similar. About 1/3 of all Kuiper belt objects (including Pluto) have orbits that are in a 3:2 resonance with Neptune; such objects are called “plutinos.”

  21. 15.4 Solar System Regularities and Irregularities Condensation theory covers the 10 points mentioned at the beginning. What about the exceptions? 1. Mercury’s large metallic core may be the result of a collision between two planetesimals, where much of the mantle was lost. 2. Two large bodies may have merged to form Venus. 3. Earth–Moon system may have formed after a collision.

  22. 4. Late collision may have caused Mars’s north–south asymmetry and stripped most of its atmosphere. 5. Uranus’s tilted axis may be the result of a glancing collision. 6. Miranda may have been almost destroyed in a collision. 7. Interactions between jovianprotoplanets and planetesimals could be responsible for irregular moons. 8. Binary Kuiper belt objects (including the Pluto-Charon system) could have formed through collisions before ejection by interactions with the jovian planets.

  23. Many of these explanations have one thing in common—a catastrophic, or near-catastrophic, collision at a critical time during formation. Normally, one does not like to explain things by calling on one-time events, but it is clear that the early solar system involved almost constant collisions. Some must have been exceptionally large.

  24. 15.5 Searching for Extrasolar Planets Most extrasolar planets have been discovered indirectly, through their gravitational or optical effects, and they cannot be seen directly due to the glare of their star. This is one exception; the planet orbits about 100 AU from its star, Fomalhaut.

  25. Planets around other stars can be detected if they are large enough to cause the star to “wobble” as the planet and star orbit around their common center of mass.

  26. If the “wobble” is transverse to our line of sight, it can also be detected through the Doppler shift as the star's motion changes.

  27. An extrasolar planet may also be detected if its orbit lies in the plane of the line of sight to us. The planet will then eclipse the star, and if the planet is large enough, some decrease in luminosity may be observed.

  28. 15.6 Properties of Exoplanets • More than 450 extrasolar planets have been discovered so far: • Most have masses comparable to Jupiter’s • Orbits are generally much smaller, and in some cases very much smaller, than the orbit of Jupiter • Orbits have high eccentricity

  29. This plot shows the mass, semimajor axis, and eccentricity for 400 extrasolar planets, with the mass ranges corresponding roughly to Jupiter, Neptune, and Earth included for comparison

  30. Orbits of 60 of the known extrasolar planets. Note that some of them are very close to their star:

  31. Planets orbiting within 0.1 AU of their stars are called “hot Jupiters”; they are not included in the previous figure but are numerous. Stars with composition like our Sun are much more likely to have planets, showing that the “dusty disk” theory is plausible. Some of these “planets” may actually be brown dwarfs, but probably not many.

  32. 15.7 Is Our Solar System Unusual? The other planetary systems discovered so far appear to be very different from our own. Selection effect biases sample toward massive planets orbiting close to parent star; lower-mass planets cannot be detected this way.

  33. Recently, more Jupiter-like planets have been found; this one has almost the mass of Jupiter and an orbital period of 9.1 years. The blue line is the same curve for Jupiter.

  34. Current theories include the possibility that Jupiter-like planets could migrate inward, through friction with the solar nebula

  35. A method of detecting Earth-like planets is much desired but will not be available for some time. The most promising detection method involves looking for changes in a star’s brightness as a planet transits across it. Until we can observe such planets, we will not be able to draw conclusions about the uniqueness of our own system.

  36. This figure shows the size of the habitable zone – where there is a possibility of liquid water being present – as a function of the mass of the parent star.

  37. Astronomers have detected most extrasolar planets by observing the “wobble” of their parent stars using spectroscopy. starlight reflected by their surfaces. eclipses when the planets block the light of their parent stars. the planets’ changing phases as they orbit their stars.

  38. Beyond our own solar system, the planets found to date have tended to be Kuiper belt objects, far from the glare of their suns. large jovians far from stars like our Sun. large jovians with orbits more like terrestrial planets. terrestrials very close to their star, and transiting its disk. imaginary, with no present proof that they really exist.

  39. Extrasolar planets the size of Earth have NOT been seen yet with current techniques because small planets probably don’t exist. the large planets nearby have swept them up. Earth-like planets take time to form. large planets orbiting near to their stars are more easily detected. small planets can only be seen if they cross in front of their star.

  40. Summary of Chapter 15 • The solar system is orderly, not random; need formation theory that explains this. • Condensation theory is the current favorite—large cloud of interstellar gas and dust starts to collapse, the Sun forms at the center, and dust particles act as accretion nuclei to form the planets. • Rocky planets would form close to the Sun; outer planets contain materials that would vaporize or escape at higher temperatures. • Jovian planets may have formed directly from instabilities in the cloud. • Asteroids never condensed into a larger object.

  41. Summary of Chapter 15 (cont.) • Leftover planetesimals were ejected from the main solar system and are now in the Kuiper belt and the Oort cloud. Some occasionally enter the inner solar system as comets. • Collisions probably explain oddities of planets and moons. • Over 450 extrasolar planets have been observed; most are massive and orbit very close to their star. This is probably the result of selection bias. • Further conclusions cannot be drawn until it is possible to detect terrestrial planets.