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    The abundance and thermal history of water ice in the disk surrounding HD 142527 from the DIGIT Herschel Key Program

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    Author
    Min, M.
    Bouwman, J.
    Dominik, C.
    Waters, L. B. F. M.
    Pontoppidan, K. M.
    Hony, S.
    Mulders, G. D.
    Henning, Th.
    van Dishoeck, E. F.
    Woitke, P.
    Evans II, Neal J.
    Team, The DIGIT
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    Affiliation
    Univ Arizona, Lunar & Planetary Lab
    Issue Date
    2016-08-29
    Keywords
    protoplanetary disks
    stars: individual: HD 142527
    stars: pre-main sequence
    
    Metadata
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    Publisher
    EDP SCIENCES S A
    Citation
    The abundance and thermal history of water ice in the disk surrounding HD 142527 from the DIGIT Herschel Key Program 2016, 593:A11 Astronomy & Astrophysics
    Journal
    Astronomy & Astrophysics
    Rights
    © ESO, 2016.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    Context. The presence or absence of ice in protoplanetary disks is of great importance to the formation of planets. By enhancing solid surface density and increasing sticking efficiency, ice catalyzes the rapid formation of planetesimals and decreases the timescale of giant planet core accretion. Aims. In this paper, we analyze the composition of the outer disk around the Herbig star HD 142527. We focus on the composition of water ice, but also analyze the abundances of previously proposed minerals. Methods. We present new Herschel far-infrared spectra and a re-reduction of archival data from the Infrared Space Observatory (ISO). We modeled the disk using full 3D radiative transfer to obtain the disk structure. Also, we used an optically thin analysis of the outer disk spectrum to obtain firm constraints on the composition of the dust component. Results. The water ice in the disk around HD 142527 contains a large reservoir of crystalline water ice. We determine the local abundance of water ice in the outer disk (i.e., beyond 130AU). The re-reduced ISO spectrum differs significantly from that previously published, but matches the new Herschel spectrum at their common wavelength range. In particular, we do not detect any significant contribution from carbonates or hydrous silicates, in contrast to earlier claims. Conclusions. The amount of water ice detected in the outer disk requires similar to 80% of oxygen atoms. This is comparable to the water ice abundance in the outer solar system, comets, and dense interstellar clouds. The water ice is highly crystalline while the temperatures where we detect it are too low to crystallize the water on relevant timescales. We discuss the implications of this finding.
    Note
    Open Access Journal.
    ISSN
    0004-6361
    1432-0746
    DOI
    10.1051/0004-6361/201425432
    Version
    Final published version
    Sponsors
    NASA through Jet Propulsion Laboratory, California Institute of Technology; EU [284405]
    Additional Links
    http://www.aanda.org/10.1051/0004-6361/201425432
    ae974a485f413a2113503eed53cd6c53
    10.1051/0004-6361/201425432
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