Variations on a theme - the evolution of hydrocarbon solids: I. Compositional and spectral modelling - the eRCN and DG models

TL;DR

This paper introduces a comprehensive model for hydrogenated amorphous hydrocarbons that predicts their compositional and spectral evolution in the interstellar medium based on microphysical properties and environmental conditions.

Contribution

It develops an extended random covalent network model and a defective graphite model to accurately describe the evolution of amorphous hydrocarbon solids in space.

Findings

Provides formulas to determine structural and spectral properties based on hydrogen content.

Shows hydrogen loss leads to a transition from aliphatic-rich to aromatic-rich materials.

Predicts optical property changes due to UV and thermal annealing in space environments.

Abstract

Context. The compositional properties of hydrogenated amorphous carbons are known to evolve in response to the local conditions. Aims. To present a model for low-temperature, amorphous hydrocarbon solids, based on the microphysical properties of random and defected networks of carbon and hydrogen atoms, that can be used to study and predict the evolution of their properties in the interstellar medium. Methods. We adopt an adaptable and prescriptive approach to model these materials, which is based on a random covalent network (RCN) model, extended here to a full compositional derivation (the eRCN model), and a defective graphite (DG) model for the hydrogen poorer materials where the eRCN model is no longer valid. Results. We provide simple expressions that enable the determination of the structural, infrared and spectral properties of amorphous hydrocarbon grains as a function of the hydrogen atomic fraction, XH. Structural annealing, resulting from hydrogen atom loss, results in a transition from H-rich, aliphatic-rich to H-poor, aromatic-rich materials. Conclusions. The model predicts changes in the optical properties of hydrogenated amorphous carbon dust in response to the likely UV photon-driven and/or thermal annealing processes resulting, principally, from the radiation field in the environment. We show how this dust component will evolve, compositionally and structurally in the interstellar medium in response to the local conditions.