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Migrating planets

Murray1, Hansen, Holman

  • 1N. Murray, B. Hansen, M. Holman, Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada. S. Tremaine, Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3.

Science (New York, N.Y.)
|January 9, 1998
PubMed
Summary
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Planetary migration occurs when planets interact with planetesimal disks, causing them to move inward. A critical disk density can lead to significant inward migration, explaining massive planets in close orbits.

Area of Science:

  • Planetary Science
  • Astrophysics
  • Exoplanet Research

Background:

  • Planets forming in disks of planetesimals can undergo orbital migration.
  • Understanding planet migration is key to explaining observed exoplanet system architectures.

Purpose of the Study:

  • To investigate the mechanism of planetary instability and inward migration within planetesimal disks.
  • To determine the critical conditions for significant planetary migration.

Main Methods:

  • Simulating resonant interactions between a planet and a disk of planetesimals.
  • Analyzing the transfer of angular momentum and its effect on orbital parameters.
  • Calculating the critical surface density of planetesimals required for instability.

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Main Results:

  • Resonant interactions lead to increased planetesimal eccentricities and angular momentum loss.
  • This process causes the planet to migrate to smaller orbital radii.
  • A critical surface density (approx. 0.03 solar masses within Jupiter's orbit) triggers large-scale inward migration.

Conclusions:

  • Planetary instability in dense planetesimal disks drives significant inward migration.
  • This mechanism provides a plausible explanation for Jupiter-mass exoplanets found in close-in orbits.