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Destruction of Refractory Carbon in Protoplanetary Disks

Anderson, Dana E. and Bergin, Edwin A. and Blake, Geoffrey A. and Ciesla, Fred J. and Visser, Ruud and Lee, Jeong-Eun (2017) Destruction of Refractory Carbon in Protoplanetary Disks. Astrophysical Journal, 845 (1). Art. No. 13. ISSN 1538-4357. https://resolver.caltech.edu/CaltechAUTHORS:20170825-081934060

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Abstract

The Earth and other rocky bodies in the inner solar system contain significantly less carbon than the primordial materials that seeded their formation. These carbon-poor objects include the parent bodies of primitive meteorites, suggesting that at least one process responsible for solid-phase carbon depletion was active prior to the early stages of planet formation. Potential mechanisms include the erosion of carbonaceous materials by photons or atomic oxygen in the surface layers of the protoplanetary disk. Under photochemically generated favorable conditions, these reactions can deplete the near-surface abundance of carbon grains and polycyclic aromatic hydrocarbons by several orders of magnitude on short timescales relative to the lifetime of the disk out to radii of ~20–100+ au from the central star depending on the form of refractory carbon present. Due to the reliance of destruction mechanisms on a high influx of photons, the extent of refractory carbon depletion is quite sensitive to the disk's internal radiation field. Dust transport within the disk is required to affect the composition of the midplane. In our current model of a passive, constant-α disk, where α = 0.01, carbon grains can be turbulently lofted into the destructive surface layers and depleted out to radii of ~3–10 au for 0.1–1 μm grains. Smaller grains can be cleared out of the planet-forming region completely. Destruction may be more effective in an actively accreting disk or when considering individual grain trajectories in non-idealized disks.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aa7da1DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aa7da1/metaPublisherArticle
https://arxiv.org/abs/1707.08982varXivDiscussion Paper
ORCID:
AuthorORCID
Anderson, Dana E.0000-0002-8310-0554
Bergin, Edwin A.0000-0003-4179-6394
Blake, Geoffrey A.0000-0003-0787-1610
Ciesla, Fred J.0000-0002-0093-065X
Visser, Ruud0000-0003-1775-5461
Lee, Jeong-Eun0000-0003-3119-2087
Additional Information:© 2017 American Astronomical Society. Received 2016 May 5. Accepted 2017 July 1. Published 2017 August 4. The authors thank the anonymous reviewer whose comments and suggestions improved this work. This material is based upon work supported by the National Science Foundation, via the Graduate Research Fellowship Program under grant No. DGE-1144469 and the Astronomy and Astrophysics Research Grants Program under grant No. AST-1514918.
Funders:
Funding AgencyGrant Number
NSF Graduate Research FellowshipDGE-1144469
NSFAST-1514918
UNSPECIFIED
Subject Keywords:astrochemistry; planets and satellites: composition; planets and satellites: formation; protoplanetary disks
Issue or Number:1
Record Number:CaltechAUTHORS:20170825-081934060
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170825-081934060
Official Citation:Dana E. Anderson et al 2017 ApJ 845 13
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:80788
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:25 Aug 2017 18:58
Last Modified:03 Oct 2019 18:35

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