Celestial Mechanics and Polarization Optics of the Kordylewski Dust Cloud in the Earth-Moon Lagrange Point L5 Part I. 3D Celestial Mechanical Modelling of Dust Cloud Formation

TL;DR

This paper models the formation of the Kordylewski dust cloud at Earth-Moon L5 using 3D celestial mechanics, providing insights into its structure and potential observational signatures.

Contribution

It introduces a detailed 3D four-body simulation of dust cloud formation at L5, filling a gap in computational studies of the KDC's characteristics.

Findings

Mapped the size and shape of dust conglomerates around L5

Simulated particle retention over 3650 days

Lays groundwork for polarimetric observation studies

Abstract

Since the discovery in 1772 of the triangular Lagrange points L4 and L5 in the gravitational field of two bodies moving under the sole influence of mutual gravitational forces, astronomers found a large number of minor celestial bodies around these points of the Sun-Jupiter, Sun-Earth, Sun-Mars and Sun-Neptune systems. The L4 and L5 points of the Earth and Moon may be empty due to the gravitational perturbation of the Sun. However, in 1961 Kordylewski found two bright patches near the L5 point, which may refer to an accumulation of interplanetary particles. Since that time this formation is called the Kordylewski dust cloud (KDC). Until now only a very few computer simulations studied the formation and characteristics of the KDC. To fill this gap, we investigated a three-dimensional four-body problem consisting of the Sun, Earth, Moon and one test particle, 1860000 times separately. We mapped the size and shape of the conglomeratum of particles not escaped from the system sooner than an integration time of 3650 days around L5. Polarimetric observations of a possible KDC around L5 are presented in the second part of this paper.