High-energy astrochemistry in the molecular interstellar medium

TL;DR

This review explores how high-energy radiation and particles influence astrochemistry in the interstellar medium, highlighting recent observations, laboratory experiments, and theoretical models that reveal complex organic molecule formation in extreme environments.

Contribution

It unifies the concept of high-energy astrochemistry, integrating recent observational, experimental, and theoretical advances into a comprehensive overview.

Findings

High-energy processes enable complex organic molecule formation in cold, dense regions.

Laboratory studies show radiation induces complex chemistry in astrophysical ices.

Theoretical models now incorporate cosmic-ray-driven processes in gas and ice phases.

Abstract

In the past decade, there has been a significant shift in astrochemistry with a renewed focus on the role of non-thermal processes on the molecular interstellar medium, in particular energetic particles (such as cosmic ray particles and fast electrons) and X-ray radiation. This has been brought about in large part due to new observations of interstellar complex organic molecules (iCOMS) in environments that would inhibit their formation, such as cold, dense gas in prestellar cores or in the highly energetic environments in galactic centers. In parallel, there has been a plethora of new laboratory investigations on the role of high-energy radiation and electrons on the chemistry of astrophysical ices, demonstrating the ability of this radiation to induce complex chemistry. In recent years, theoretical models have also begun to include newer cosmic-ray-driven processes in both the gas and ice phases. In this review, we unify aspects of the chemistry driven by X-ray radiation and energetic particles into a ``high-energy astrochemistry'', defining this term and reviewing the underlying chemical processes. We conclude by examining various laboratories where high-energy astrochemistry is at play and identify future issues to be tackled.