期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 802, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/802/2/L23
关键词
astrochemistry; ISM: abundances; protoplanetary disks; stars: formation
资金
- National Science Foundation [1008800]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1008800] Funding Source: National Science Foundation
- Grants-in-Aid for Scientific Research [25108004, 23103004, 23540266] Funding Source: KAKEN
In this Letter, we model the chemistry of DCO+ in protoplanetary disks. We find that the overall distribution of the DCO+ abundance is qualitatively similar to that of CO but is dominated by a thin layer located at the inner disk surface. To understand its distribution, we investigate the different key gas-phase deuteration pathways that can lead to the formation of DCO+. Our analysis shows that the recent update in the exothermicity of the reaction involving CH2D+ as a parent molecule of DCO+ favors deuterium fractionation in warmer conditions. As a result, the formation of DCO+ is enhanced in the inner warm surface layers of the disk where X-ray ionization occurs. Our analysis points out that DCO+ is not a reliable tracer of the CO snow line as previously suggested. We thus predict that DCO+ is a tracer of active deuterium and, in particular, X-ray ionization of the inner disk.
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