Open AccessFrom the Oort cloud to observable short‐period comets – I. The initial stage of cometary capture
Author(s) -
Rickman H.,
Valsecchi G. B.,
Froeschlé Cl.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04295.x
Subject(s) - physics , ecliptic , interstellar comet , astrophysics , asteroid , celestial mechanics , astronomy , observable , solar system , jupiter (rocket family) , comet , orbit (dynamics) , solar wind , spacecraft , quantum mechanics , magnetic field , engineering , aerospace engineering
We investigate the first stage of the dynamical evolution of Oort cloud comets entering the planetary region for the first time. To this purpose, we integrate numerically the motions of a large number of fictitious comets pertaining to two samples, both with perihelion distances up to 5.7 au and random inclinations; the first sample is composed of comets whose orbits have at least one node close to 5.2 au, while the second is not subject to this constraint. We examine the orbits when the comets come to aphelion after their first perihelion passage within the planetary region, and find that there is a clear statistical dependence of the energy perturbations on the Tisserand parameter. There appear to be two main processes, of comparable importance, governing the shortening of semimajor axes to values of less than 1000 au, i.e. planetary close encounters, especially with Jupiter, and indirect perturbations due to the shifting of the motion from barycentric to heliocentric and back; the former process mostly affects comets crossing the ecliptic at about 5.2 au, or on low‐inclination orbits, while the latter mostly affects comets of small perihelion distance. This last result may help to understand the relative paucity of Halley‐type comets with perihelion distances larger than about 1.5 au.