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- W4244208473 endingPage "043001" @default.
- W4244208473 startingPage "043001" @default.
- W4244208473 abstract "In the last 40 years a wide range of molecules, including neutrals, cations and anions, containing up to 13 atoms—in addition to detections of and —have been found in the harsh environment of the interstellar medium. The exquisite sensitivity and very high spectral and, more recently, spatial resolution, of modern telescopes has enabled the physics of star formation to be probed through rotational line emission. In this article, I review the basic properties of interstellar clouds and the processes that initiate the chemistry and generate chemical complexity, particularly in regions of star and planet formation. Our understanding of astrochemistry has evolved over the years. Before 1990, the general consensus was that molecules were formed in binary, gas-phase, or volume, reactions, most importantly ion-neutral reactions despite the very low ionization in clouds. Since then, observations have indicated unambiguously that there is also a contribution from surface processes, particularly on the icy mantles that form around refractory grain cores in cold, dense gas. The balance between these two processes depends on particular physical conditions and can vary during the life cycle of a particular volume of interstellar cloud." @default.
- W4244208473 created "2022-05-12" @default.
- W4244208473 creator A5050502051 @default.
- W4244208473 date "2015-07-14" @default.
- W4244208473 modified "2023-09-26" @default.
- W4244208473 title "Astrochemistry" @default.
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