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Title: Gas Mass Tracers in Protoplanetary Disks: CO is Still the Best
Authors: Molyarova, T.
Akimkin, V.
Semenov, D.
Henning, T.
Vasyunin, A.
Wiebe, D.
Issue Date: 2017
Publisher: Institute of Physics Publishing
Citation: Gas Mass Tracers in Protoplanetary Disks: CO is Still the Best / T. Molyarova, V. Akimkin, D. Semenov et al. // Astrophysical Journal. — 2017. — Vol. 849. — Iss. 2. — 130.
Abstract: Protoplanetary disk mass is a key parameter controlling the process of planetary system formation. CO molecular emission is often used as a tracer of gas mass in the disk. In this study, we consider the ability of CO to trace the gas mass over a wide range of disk structural parameters, and we search for chemical species that could possibly be used as alternative mass tracers to CO. Specifically, we apply detailed astrochemical modeling to a large set of models of protoplanetary disks around low-mass stars to select molecules with abundances correlated with the disk mass and being relatively insensitive to other disk properties. We do not consider sophisticated dust evolution models, restricting ourselves to the standard astrochemical assumption of 0.1 μm dust. We find that CO is indeed the best molecular tracer for total gas mass, despite the fact that it is not the main carbon carrier, provided reasonable assumptions about CO abundance in the disk are used. Typically, chemical reprocessing lowers the abundance of CO by a factor of 3, compared to the case where photodissociation and freeze-out are the only ways of CO depletion. On average, only 13% C atoms reside in gas-phase CO, albeit with variations from 2% to 30%. CO 2 , H 2 O, and H 2 CO can potentially serve as alternative mass tracers, with the latter two only applicable if disk structural parameters are known. © 2017. The American Astronomical Society. All rights reserved.
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85034590488
WOS ID: 000414987100004
PURE ID: 6156012
ISSN: 0004-637X
DOI: 10.3847/1538-4357/aa9227
metadata.dc.description.sponsorship: We thank the referee for fruitful comments that helped us improve our model and formulate better conclusions. T.M., V.A., and D.W. acknowledge financial support from the Russian Science Foundation (17-12-01441; Sections 2, 3, 5). D.S. acknowledges support from the Heidelberg Institute of Theoretical Studies for the project “Chemical kinetics models and visualization tools: Bridging biology and astronomy.” A.V. acknowledges support from the European Research Council (ERC; project PALs 320620).
RSCF project card: 17-12-01441
Appears in Collections:Научные публикации, проиндексированные в SCOPUS и WoS CC

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