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Isotopic fractionation in interstellar molecules

Published online by Cambridge University Press:  04 September 2018

Kenji Furuya
Kenji Furuya*
Affiliation:
Center for Computational Sciences, University of Tsukuba, 1-1-1 Tennoudai, 305-8577 Tsukuba, Japan email: furuya@ccs.tsukuba.ac.jp
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Abstract

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The level of isotopic fractionation in molecules provides insights into their formation environments and how they formed. In this article, we review hydrogen and nitrogen isotopic fractionation in low-mass star-forming regions. Interstellar molecules are significantly enriched in deuterium. The importance of the nuclear spin states of light species on deuterium fractionation and the usefulness of singly and doubly deuterated molecules as chemical tracers are discussed. Observations have revealed that molecules in prestellar cores are enriched in or depleted in 15N depending on molecules. Compared with deuterium fractionation chemistry, our understanding of 15N fractionation chemistry is not well established. We briefly discuss potential 15N fractionation routes, i.e., isotopic-exchange reactions and isotopic selective photodissociation of N2. In addition, the selective freeze-out of 15N atoms onto dust grains around the transition between N atoms and N2 is discussed as a potential mechanism that causes the depletion of 15N in the gas phase.

Keywords

AstrochemistryISM: abundancesISM: moleculesstar: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S332: Astrochemistry VII: Through the Cosmos from Galaxies to Planets , March 2017 , pp. 163 - 174
Copyright
Copyright © International Astronomical Union 2018 

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