Detections of trans-Neptunian ice in protoplanetary disks

Abstract

We present Herschel Space Observatory PACS spectra of T Tauri stars, in which we detect amorphous and crystalline water ice features. Using irradiated accretion disk models, we determine the disk structure and ice abundance in each of the systems. Combining a model-independent comparison of the ice feature strength and disk size with a detailed analysis of the model ice location, we estimate that the ice emitting region is at disk radii >30AU, consistent with a proto-Kuiper belt. Vertically, the ice emits most below the photodesorption zone, consistent with Herschel observations of cold water vapor. The presence of crystallized water ice at a disk location a) colder than its crystallization temperature and b) where it should have been re-amorphized in ~1 Myr suggests that localized generation is occurring; the most likely cause appears to be micrometeorite impact or planetesimal collisions. Based on simple tests with UV models and different ice distributions, we suggest that the SED shape from 20 to 50 micron may probe the location of the water ice snow line in the disk upper layers. This project represents one of the first extra-solar probes of the spatial structure of the cometary ice reservoir thought to deliver water to terrestrial planets.

arXiv commentAccepted to ApJ on Nov. 20th 2014; 16 pages, including 11 figures and 4 tables

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• Dust continuum emission and the upper limit fluxes of sub-millimeter water lines of the protoplanetary disk around HD 163296 observed by ALMA
• Simulating Observations of Ices in Protoplanetary Disks
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• The nitrogen carrier in protoplanetary disks
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• Constraining the detectability of water ice in debris disks
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• THz Time-Domain Spectroscopy of Mixed CO2-CH3OH Interstellar Ice Analogs
• Vacuum ultraviolet photodesorption and photofragmentation of formaldehyde-containing ices
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• Development of the Fabry-Perot interferometers for the HIRMES spectrometer on SOFIA
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