Formation of PAHs and Carbonaceous Solids in Gas-Phase Condensation Experiments

TL;DR

This study investigates how temperature influences the formation pathways of carbonaceous cosmic dust particles, revealing that lower temperatures favor PAH formation while higher temperatures produce fullerenes, impacting astrophysical dust composition.

Contribution

It provides experimental evidence linking condensation temperature to specific types of carbonaceous particles formed, advancing understanding of cosmic dust formation processes.

Findings

PAHs dominate at temperatures below 1700 K

Fullerene-like grains form above 3500 K

Condensation products vary with astrophysical environment temperature

Abstract

Carbonaceous grains represent a major component of cosmic dust. In order to understand their formation pathways, they have been prepared in the laboratory by gas-phase condensation reactions such as laser pyrolysis and laser ablation. Our studies demonstrate that the temperature in the condensation zone determines the formation pathway of carbonaceous particles. At temperatures lower than 1700 K, the condensation by-products are mainly polycyclic aromatic hydrocarbons (PAHs), that are also the precursors or building blocks for the condensing soot grains. The low-temperature condensates contain PAH mixtures that are mainly composed of volatile 3-5 ring systems. At condensation temperatures higher than 3500 K, fullerene-like carbon grains and fullerene compounds are formed. Fullerene fragments or complete fullerenes equip the nucleating particles. Fullerenes can be identified as soluble components. Consequently, condensation products in cool and hot astrophysical environments such as cool and hot AGB stars or Wolf Rayet stars should be different and should have distinct spectral properties.