Laboratory Experiments on the Radiation Astrochemistry of Water Ice Phases

TL;DR

This study systematically compares radiation-induced chemical changes in different phases of water ice at 20 K, revealing phase-dependent amorphization, compaction, and peroxide production with implications for astrophysical environments.

Contribution

It provides the first detailed comparison of radiation effects across multiple water ice phases, highlighting phase-dependent chemical and physical transformations.

Findings

Amorphization of RAI, Ic, and Ih phases under electron irradiation.

ASW undergoes compaction instead of amorphization.

Hydrogen peroxide yield varies with ice phase, highest in ASW.

Abstract

Water (H2O) ice is ubiquitous component of the universe, having been detected in a variety of interstellar and Solar System environments where radiation plays an important role in its physico-chemical transformations. Although the radiation chemistry of H2O astrophysical ice analogues has been well studied, direct and systematic comparisons of different solid phases are scarce and are typically limited to just two phases. In this article, we describe the results of an in-depth study of the 2 keV electron irradiation of amorphous solid water (ASW), restrained amorphous ice (RAI) and the cubic (Ic) and hexagonal (Ih) crystalline phases at 20 K so as to further uncover any potential dependence of the radiation physics and chemistry on the solid phase of the ice. Mid-infrared spectroscopic analysis of the four investigated H2O ice phases revealed that electron irradiation of the RAI, Ic, and Ih phases resulted in their amorphization (with the latter undergoing the process more slowly) while ASW underwent compaction. The abundance of hydrogen peroxide (H2O2) produced as a result of the irradiation was also found to vary between phases, with yields being highest in irradiated ASW. This observation is the cumulative result of several factors including the increased porosity and quantity of lattice defects in ASW, as well as its less extensive hydrogen-bonding network. Our results have astrophysical implications, particularly with regards to H2O-rich icy interstellar and Solar System bodies exposed to both radiation fields and temperature gradients.