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- W190268718 abstract "Both theory and observation suggest that metallicity profoundly alters the properties and structure of the Photodissociation Regions (PDRs; e.g., Madden et al. 1997). Several factors contribute to the differences between high and low metallicity systems: altered gas phase and grain surface chemistry due to the low Si, C and S elemental abundances, and diminished dust shielding because of the low dust-to-gas ratio. Since there is less dust shielding, UV photons penetrate more deeply into the molecular clouds leaving H 2 unaffected but photodissociating most other molecules everywhere except in the most opaque clumps. Thus, a low-metallicity system contains large regions where hydrogen remains molecular but the usual tracers of molecular gas like CO are photodissociated." @default.
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- W190268718 date "1999-01-01" @default.
- W190268718 modified "2023-10-18" @default.
- W190268718 title "Photodissociation Regions in the Large Magellanic Cloud and IC 10" @default.
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- W190268718 doi "https://doi.org/10.1017/s0074180900117619" @default.
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