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Warm dust surface chemistry in protoplanetary disks : formation of phyllosilicates

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1812.04357v1.pdf (1.969Mb)
Date
03/2020
Author
Thi, W. F.
Hocuk, S.
Kamp, I.
Woitke, P.
Rab, Ch
Cazaux, S.
Caselli, P.
D'Angelo, M.
Funder
European Commission
European Commission
Grant ID
284405
Keywords
Astrochemistry
Methods: numerical
Stars: pre-main-sequence
QB Astronomy
QD Chemistry
3rd-DAS
Metadata
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Abstract
Context. The origin of the reservoirs of water on Earth is debated. The Earth’s crust may contain at least three times more water than the oceans. This crust water is found in the form of phyllosilicates, whose origin probably differs from that of the oceans. Aims. We test the possibility to form phyllosilicates in protoplanetary disks, which can be the building blocks of terrestrial planets. Methods. We developed an exploratory rate-based warm surface chemistry model where water from the gas-phase can chemisorb on dust grain surfaces and subsequently diffuse into the silicate cores. We applied the phyllosilicate formation to a zero-dimensional chemical model and to a 2D protoplanetary disk model (PRODIMO). The disk model includes in addition to the cold and warm surface chemistry continuum and line radiative transfer, photoprocesses (photodissociation, photoionisation, and photodesorption), gas-phase cold and warm chemistry including three-body reactions, and detailed thermal balance. Results. Despite the high energy barrier for water chemisorption on silicate grain surfaces and for diffusion into the core, the chemisorption sites at the surfaces can be occupied by a hydroxyl bond (–OH) at all gas and dust temperatures from 80 to 700 K for a gas density of 2 × 104 cm−3. The chemisorption sites in the silicate cores are occupied at temperatures between 250 and 700 K. At higher temperatures thermal desorption of chemisorbed water occurs. The occupation efficiency is only limited by the maximum water uptake of the silicate. The timescales for complete hydration are at most 105 yr for 1 mm radius grains at a gas density of 108 cm−3. Conclusions. Phyllosilicates can be formed on dust grains at the dust coagulation stage in protoplanetary disks within 1 Myr. It is however not clear whether the amount of phyllosilicate formed by warm surface chemistry is sufficient compared to that found in Solar System objects.
Citation
Thi , W F , Hocuk , S , Kamp , I , Woitke , P , Rab , C , Cazaux , S , Caselli , P & D'Angelo , M 2020 , ' Warm dust surface chemistry in protoplanetary disks : formation of phyllosilicates ' , Astronomy & Astrophysics , vol. 635 , A16 . https://doi.org/10.1051/0004-6361/201731747
Publication
Astronomy & Astrophysics
Status
Peer reviewed
DOI
https://doi.org/10.1051/0004-6361/201731747
ISSN
0004-6361
Type
Journal article
Rights
Copyright © 2019 ESO. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/201731747
Description
Funding: Dr. Thomas Müller, and Dr. Victor Ali-Lagoa. IK,WFT, CR, and PW acknowledge fundingfrom the EU FP7- 2011 under Grant Agreement nr. 284405. CR also acknowl-edges funding by the Austrian Science Fund (FWF), project number P24790.
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  • University of St Andrews Research
URL
https://arxiv.org/abs/1812.04357v1
URI
http://hdl.handle.net/10023/18612

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