Haze Formation on Triton
Kazumasa Ohno, Xi Zhang, Ryo Tazaki, Satoshi Okuzumi

TL;DR
This paper presents the first microphysical model of Triton's haze formation, exploring particle growth, composition, and observational signatures to better understand the moon's hazy atmosphere.
Contribution
It introduces a self-consistent haze microphysical model for Triton, including effects of condensation and particle aggregation, which was not previously available.
Findings
Haze particles grow into fractal aggregates with sizes 0.1-1 μm.
Including C2H4 ice condensation better explains observations.
UV and visible data can distinguish between icy spheres and aggregates.
Abstract
The largest moon of Neptune, Triton, possess a cold and hazy atmosphere. Since the discovery of near-surface haze layer during the Voyager fly in 1989, the haze formation mechanism has not been investigated in detail. Here, we provide the first haze microphysical model on Triton. Our model solves the evolution of both size and porosity distributions of haze particles in a self-consistent manner. We simulated the formation of sphere and aggregate hazes with and without condensation of the CH ice. The haze particles can grow into fractal aggregates with mass-equivalent sphere sizes of -- and fractal dimension of --. The ice-free hazes cannot simultaneously explain both UV and visible observations of Voyager 2, while including the condensation of CH ices provides two better solutions. For ice aggregates, the required total haze…
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