期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 806, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/806/1/L7
关键词
astrochemistry; planets and satellites: composition; protoplanetary disks; stars: individual (HL Tau); stars: pre-main sequence
资金
- NSF Astronomy Astrophysics
- NASA Origins of Solar Systems grant programs
- NSF INSPIRE [AST-1344133]
- Direct For Mathematical & Physical Scien [1344133] Funding Source: National Science Foundation
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1109857] Funding Source: National Science Foundation
- Division Of Astronomical Sciences [1344133] Funding Source: National Science Foundation
Water and simple organic molecular ices dominate the mass of solid materials available for planetesimal and planet formation beyond the water snow line. Here we analyze ALMA long baseline 2.9, 1.3 and 0.87 mm continuum images of the young star HL Tau, and suggest that the emission dips observed are due to rapid pebble growth around the condensation fronts of abundant volatile species. Specifically, we show that the prominent innermost dip at 13 AU is spatially resolved in the 0.87 mm image, and its center radius is coincident with the expected midplane condensation front of water ice. In addition, two other prominent dips, at distances of 32 and 63 AU, cover the mid-plane condensation fronts of pure ammonia or ammonia hydrates and clathrate hydrates (especially with CO and N-2) formed from amorphous water ice. The spectral index map of HL Tau between 1.3 and 0.87 mm shows that the flux ratios inside the dips are statistically larger than those of nearby regions in the disk. This variation can be explained by a model with two dust populations, where most of the solid mass resides in a component that has grown to decimeter size scales inside the dips. Such growth is in accord with recent numerical simulations of volatile condensation, dust coagulation, and settling.
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