H$_2$ formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations
Valentine Wakelam, Emeric Bron, Stephanie Cazaux, Francois Dulieu,, C\'ecile Gry, Pierre Guillard, Emilie Habart, Liv Hornek{\ae}r, Sabine, Morisset, Gunnar Nyman, Valerio Pirronello, Stephen D. Price, Valeska, Valdivia, Gianfranco Vidali, Naoki Watanabe
TL;DR
This paper reviews the current understanding of molecular hydrogen formation on interstellar dust grains, integrating theoretical, experimental, modeling, and observational perspectives amid recent astrophysical advances.
Contribution
It synthesizes diverse viewpoints on H$_2$ formation, highlighting recent progress and future prospects with JWST in understanding interstellar environments.
Findings
H$_2$ forms efficiently on dust grain surfaces.
Recent models align with observational data.
Future JWST observations will refine understanding.
Abstract
Molecular hydrogen is the most abundant molecule in the universe. It is the first one to form and survive photo-dissociation in tenuous environments. Its formation involves catalytic reactions on the surface of interstellar grains. The micro-physics of the formation process has been investigated intensively in the last 20 years, in parallel of new astrophysical observational and modeling progresses. In the perspectives of the probable revolution brought by the future satellite JWST, this article has been written to present what we think we know about the H formation in a variety of interstellar environments.
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