Structure in the Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron

@article{Quillen2002StructureIT,
  title={Structure in the Eridani Dusty Disk Caused by Mean Motion Resonances with a 0.3 Eccentricity Planet at Periastron},
  author={A. Quillen and Stephen L. Thorndike},
  journal={The Astrophysical Journal},
  year={2002},
  volume={578}
}
  • A. Quillen, Stephen L. Thorndike
  • Published 2002
  • Physics
  • The Astrophysical Journal
  • The morphology of the Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5 : 3 and 3 : 2 exterior mean motion resonances with a 0.3 eccentricity 10-4 M☉ planet at periastron at a semimajor axis of 40 AU. The morphology will differ when the planet is at apastron, in about 140 yr. Moderate eccentricity planets in outer extrasolar systems will cause observable variations in the morphology of associated dusty rings. 
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