• DOI:10.1046/j.1365-8711.2003.06714.x
• Corpus ID: 2822011

The populations of comet-like bodies in the Solar system

@article{Horner2003ThePO,
  title={The populations of comet-like bodies in the Solar system},
  author={Jonathan Horner and N. Wyn Evans and Mark E. Bailey and David J. Asher},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2003},
  volume={343},
  pages={1057-1066}
}

• J. Horner, N. Evans, +1 author D. Asher
• Published 16 April 2003
• Physics, Geology
• Monthly Notices of the Royal Astronomical Society

A new classification scheme is introduced for comet-like bodies in the Solar system. It covers the traditional comets as well as the Centaurs and Edgeworth–Kuiper belt objects. At low inclinations, close encounters with planets often result in near-constant perihelion or aphelion distances, or in perihelion–aphelion interchanges, so the minor bodies can be labelled according to the planets predominantly controlling them at perihelion and aphelion. For example, a JN object has a perihelion under the control of Jupiter and aphelion under the control of Neptune, and so on. This provides 20 dynamically distinct categories of outer Solar system objects in the Jovian and trans-Jovian regions. The Tisserand parameter with respect to the planet controlling perihelion is also often roughly constant under orbital evolution. So, each category can be further subdivided according to the Tisserand parameter.

The dynamical evolution of comets, however, is dominated not by the planets nearest at perihelion or aphelion, but by the more massive Jupiter. The comets are separated into four categories – Encke-type, short-period, intermediate and long-period – according to aphelion distance. The Tisserand parameter categories now roughly correspond to the well-known Jupiter-family comets, transition types and Halley types. In this way, the nomenclature for the Centaurs and Edgeworth–Kuiper belt objects is based on, and consistent with, that for comets. Given the perihelion and aphelion distances together with the Tisserand parameter, our classification scheme provides a description for any comet-like body in the Solar system. The usefulness of the scheme is illustrated with examples drawn from numerical simulations and from the present-day Solar system.