# Aerosols optical properties in Titan's Detached Haze Layer before the equinox

## TL;DR

This study analyzes Titan's detached haze layer using Cassini UV observations, revealing stable aerosol properties over time in the southern hemisphere and size variations in the northern hemisphere, with implications for understanding Titan's atmospheric aerosols.

## Contribution

It introduces a method to extract aerosol optical properties from high-resolution UV images and demonstrates their stability and variability across Titan's hemispheres over several years.

## Key findings

- Aerosols consist of at least ten 60 nm monomers.
- Aerosol properties are stable in the southern hemisphere.
- Northern hemisphere aerosols tend to decrease in size and increase in opacity.

## Abstract

UV observations with Cassini ISS Narrow Angle Camera of Titan's detached haze is an excellent tool to probe its aerosols content without being affected by the gas or the multiple scattering. Unfortunately, its low extent in altitude requires a high resolution calibration and limits the number of images available in the Cassini dataset. However, we show that it is possible to extract on each profile the local maximum of intensity of this layer and confirm its stability at $500 \pm 8$ km during the 2005-2007 period for all latitudes lower than 45$^\circ$N. Using the fractal aggregate scattering model of Tomasko et al. (2008) and a single scattering radiative transfer model, it is possible to derive the optical properties required to explain the observations made at different phase angles. Our results indicates that the aerosols have at least ten monomers of 60 nm radius, while the typical tangential column number density is about $2\cdot 10^{10}$ agg.m$^{-2}$. Moreover, we demonstrate that these properties are constant within the error bars in the southern hemisphere of Titan over the observed time period. In the northern hemisphere, the size of the aerosols tend to decrease relatively to the southern hemisphere and are associated with a higher tangential opacity. However, the lower number of observations available in this region due to the orbital constraints is a limiting factor in the accuracy of these results. Assuming a fixed homogeneous content we notice that the tangential opacity can fluctuate up to a factor 3 among the observations at the equator. These variations could be linked with short scale temporal and/or longitudinal events changing the local density of the layer.