Abstract
Massive stars disrupt their natal molecular cloud material by dissociating molecules, ionizing atoms and molecules, and heating gas and dust. This interaction occurs in Photo-Dissociation Regions (PDRs) where stellar far-ultraviolet photons create a largely neutral, warm region. PDR emission dominates the IR spectra of star-forming galaxies and provides a unique tool to study in detail the physical and chemical processes that are relevant for interstellar and circumstellar media including diffuse clouds, molecular cloud, protoplanetary disk surfaces, planetary nebulae, and starburst galaxies. I will review a number of less-well-understood issues on the physical and chemical processes relevant for PDRs. Specifically, I will discuss the formation of H\(_2\) as well as the role of large molecules in the photo-electric heating and chemical composition of the gas. I will also review the chemical evolution of Polycyclic Aromatic Hydrocarbon molecules driven by photo-dissociation and isomerization processes. Relevant laboratory studies and quantum chemical calculations will be pointed out.
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Notes
- 1.
Note that the H- and H\(_2\)-loss channel have very comparable energies from these sp\(^3\) sites (2.72 and 2.85 eV West et al. 2014).
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Tielens, A.G.G.M. (2023). Physics and Chemistry of PhotoDissociation Regions. In: Mennella, V., Joblin, C. (eds) European Conference on Laboratory Astrophysics ECLA2020. ECLA 2021. Astrophysics and Space Science Proceedings, vol 59. Springer, Cham. https://doi.org/10.1007/978-3-031-29003-9_15
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