Hydroxylated Mg-rich Amorphous Silicates as Catalysts for Molecular Hydrogen Formation in the Interstellar Medium

Abstract

Abstract We present results from an experimental study on the interaction of atomic deuterium with magnesium-rich amorphous enstatite- and forsterite-type silicates. Infrared spectroscopy was used to examine the process. During deuterium atom exposure, deuteroxyl group formation was observed. The cross section for OD group formation, estimated from the OD stretching band intensity with D atom fluence, is σ f ,OD = 4.2 × 10 −18 cm 2 for both silicates. HD (D 2 ) molecules form via D atom abstraction of chemisorbed H (D) atoms from OH (OD) groups, with a cross section of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mi>σ</mml:mi> <mml:mrow> <mml:mi>f</mml:mi> <mml:mo>,</mml:mo> <mml:msub> <mml:mi mathvariant="normal">D</mml:mi> <mml:mn>2</mml:mn> </mml:msub> </mml:mrow> </mml:msub> </mml:math> = 7.0 × 10 −18 cm 2 . Quantum-chemical calculations on enstatite and forsterite amorphous nanoclusters were used to analyze chemisorption and abstraction energies of hydrogen atoms. The formation of OH groups on forsterite is barrierless, while enstatite has a small energy barrier. H 2 abstraction from hydroxyl groups is barrierless in both silicates. The results support our interpretation of IR spectral changes during D atom exposure as addition and exchange reactions, with catalytic molecular deuterium formation. These findings, obtained at 300 K, are relevant to astrophysical environments like photodissociation regions and interstellar clouds at lower temperatures. Amorphous silicates, like carbon grains, undergo hydrogenation in the diffuse interstellar medium due to interactions with atomic hydrogen and UV photons. The detection of these components on comet 67P/Churyumov–Gerasimenko connects primitive solar system objects to interstellar dust, offering new insights into their evolution.