Chemistry of comet atmospheres

TL;DR

This paper reviews the composition and chemical diversity of comet atmospheres, highlighting recent findings from spectroscopy, in-situ measurements, and the Rosetta mission, and discusses unresolved questions about their origins.

Contribution

It provides a comprehensive overview of cometary coma composition, recent isotopic measurements, and identifies key areas for future research to understand comet origins.

Findings

Cometary comae are dominated by water, CO, or CO2.

Multiple molecules, including complex organics, have been detected.

Isotopic ratios from Rosetta offer clues on comet origins.

Abstract

The composition of cometary ices provides key information on the thermal and chemical properties of the outer parts of the protoplanetary disk where they formed 4.6 Gy ago. This chapter reviews our knowledge of composition of cometary comae based on remote spectroscopy and in-situ investigations techniques. Cometary comae can be dominated by water vapour, CO or CO2. The abundances of several dozen of molecules, with a growing number of complex organics, have been measured in comets. Many species that are not directly sublimating from the nucleus ices have also been observed and traced out into the coma in order to determine their production mechanisms. Chemical diversity in the comet population and compositional heterogeneity of the coma are discussed. With the completion of the Rosetta mission, isotopic ratios, which hold additional clues on the origin of cometary material, have been measured in several species. Finally, important pending questions (e.g., the nitrogen deficiency in comets) and the need for further work in certain critical areas are discussed in order to answer questions and resolve discrepancies between techniques.