# Flattened loose particles from numerical simulations compared to Rosetta collected particles

## TL;DR

This study uses numerical simulations to analyze the physical structure of cometary dust particles, comparing flattened particle aspect ratios from simulations and observations to infer their aggregation history and physical properties.

## Contribution

The paper introduces a simple impact flattening simulation to interpret COSIMA particle data, distinguishing between different aggregate growth modes based on fractal dimensions.

## Key findings

- COSIMA's aspect ratio data supports two aggregate families with different fractal dimensions.
- Variations in cohesive strength and velocity influence particle morphology.
- The results suggest two distinct dust particle populations ejected from the comet nucleus.

## Abstract

Cometary dust particles are remnants of the primordial accretion of refractory material that occurred during the initial stages of the Solar System formation. Understanding their physical structure can help constrain their accretion process. We have developed a simple numerical simulation of aggregate impact flattening to interpret the properties of particles collected by COSIMA. The aspect ratios of flattened particles from both simulations and observations are compared to differentiate between initial families of aggregates characterized by different fractal dimensions $D_f$. This dimension can differentiate between certain growth modes. The diversity of aspect ratios measured by COSIMA is consistent with either two families of aggregates with different initial $D_f$ (a family of compact aggregates with fractal dimensions close to 2.5-3 and some fluffier aggregates with fractal dimensions around 2). Alternatively, the distribution of morphologies seen by COSIMA could originate from a single type of aggregation process, such as DLPA, but to explain the range of aspect ratios observed by COSIMA a large range of dust particle cohesive strength is necessary. Furthermore, variations in cohesive strength and velocity may play a role in the higher aspect ratio range detected (>0.3). Our work allows us to explain the particle morphologies observed by COSIMA and those generated by laboratory experiments in a consistent framework. Taking into account all observations from the three dust instruments on-board Rosetta, we favor an interpretation of our simulations based on two different families of dust particles with significantly distinct fractal dimensions ejected from the cometary nucleus.