The Formation of Planetary Systems The Solar System and Beyond
updated Mar 2, 2005, jeb PRELIMINARY



Search for the Theory of Formation of Solar System

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The Observables

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Planetary Irregularities



The Condensation with Accretion Model

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    Steps in the evolutionary process of the condensation theory
  1. Very large (about 100,000 AU) gas cloud fragment with dust collapses.
  2. Centrifugal effects
  3. Gas molecules and dust grains in circular orbits
  4. Collapsing gas and dust heats through collisions
  5. Nebula cools
  6. Gas and dust particles in parallel, circular orbits
  7. Massive planetesimals pull in nearby nebula (core-accretion theory)
  8. Icy planetesimals near Jupiter and Saturn flung out of solar system.
  9. Early Sun has magnetic field and spews out ions
  10. Proto-sun core gets to about 10 million degrees Kelvin


Interplanetary Debris



Catastrophes

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The Angular Momentum Problem

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While conceding that they do not know which explanation is correct, astronomers believe the angular momentum problem has a solution and the condensation model is basically correct



Search for Other Planetary Systems

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Planetary Properties

    of the detected extrasolar planets
  1. Masses comparable to Jupiter (1/3 - 10 x MJUPITER)
  2. Many orbits are smaller than Jupiter or Saturn (many very close - 0.1 AU - to Star)
  3. Many orbits are highly eccentric, compared to Jupiter and Saturn


Is Our Solar System Unusual?

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Search for Protostars

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Conclusions

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Other Sources on The Origin of the Solar System

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