Benzene formation in the inner regions of protostellar disks

Abstract

Benzene (c-C6H6) formation in the inner 3 AU of a protostellar disk can be efficient, resulting in high abundances of benzene in the midplane region. The formation mechanism is different to that found in interstellar clouds and in protoplanetary nebulae, and proceeds mainly through the reaction between allene (C3H4) and its ion. This has implications for PAH formation, in that some fraction of PAHs seen in the solar system could be native rather than inherited from the interstellar medium.

9 pages, 2 colour figures, to be published in the Astrophysical Journal Letters

References in corpus (4)

• Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores
• ISO spectroscopy of disks around Herbig Ae/Be stars
• The gas temperature in the surface layers of protoplanetary disks
• On the Ionisation Fraction in Protoplanetary Disks II: The Effect of Turbulent Mixing on Gas--phase Chemistry

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• Carbon chemistry in Galactic Bulge Planetary Nebulae
• The diverse chemistry of protoplanetary disks as revealed by JWST
• The chemistry of disks around T Tauri and Herbig Ae/Be stars
• The composition of the protosolar disk and the formation conditions for comets
• Laboratory investigations of the interaction between benzene and bare silicate grain surfaces
• MINDS. Hydrocarbons detected by JWST/MIRI in the inner disk of Sz28 consistent with a high C/O gas-phase chemistry
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• The Influence of Galactic Cosmic Rays on Ion-Neutral Hydrocarbon Chemistry in the Upper Atmospheres of Free-Floating Exoplanets
• Hydrocarbon chemistry in inner regions of planet forming disks
• MINDS: The very low-mass star and brown dwarf sample -- Hidden water in carbon-dominated protoplanetary disks
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• Optical and infrared emission of H II complexes as a clue to the PAH life cycle
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