Finite Lifetime Fragment Model 4 for Striae Formation in the Dust Tails of Comets (FLM 4) Acceleration by Lorenz-force

TL;DR

This paper introduces a new dynamic model explaining the formation of striae in comet dust tails through Lorentz-force acceleration of charged particles, accounting for their structure, luminosity, and lifespan.

Contribution

The paper presents a novel model that describes striae formation via Lorentz-force acceleration of small charged dust particles, improving upon previous theories.

Findings

Model explains striae structure and luminosity

Particles decay within 100 days at 1 AU

Predicts striae formation and disappearance patterns

Abstract

The striations in the dust tails of comets are referred to as striae, and their origin has long been a mystery. We introduce a new dynamic model to describe the forms of the striae observed in comets Hale-Bopp (C/1995 O1), West (C/1975 V1), and Seki-Lines (C/1962 C1). Charged particles made of refractory materials, with radii less than 0.5micrometer, are expelled from the comet's nucleus and accelerated by Lorentz forces near the nucleus. These particles decay many times to form striae, which have a lifespan of less than about 100 days at a distance of 1 astronomical unit from the sun. Over time, they continue to decay and eventually disappear from view. The following dynamic model explains these material science processes. Particles expelled from the comet's nucleus are subjected to three forces: solar gravity, solar radiation pressure, and Lorentz forces near the nucleus. As these particles decrease in size, the Lorentz forces and radiation pressure cause fluctuations, increasing and decreasing to form striae. This model, which is less of a dynamic approximation than previous theories (FLM3), explains the structure of the striae, enables predictions of their luminosity, and clarifies their origin.