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Evidence for the start of planet formation in a young circumstellar disk
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Evidence for the start of planet formation in a young circumstellar disk
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Journal Article
Evidence for the start of planet formation in a young circumstellar disk
2018
Overview
The growth of dust grains in protoplanetary disks is a necessary first step towards planet formation
1
. This growth has been inferred from observations of thermal dust emission
2
towards mature protoplanetary systems (age >2 million years) with masses that are, on average, similar to Neptune
3
. In contrast, the majority of confirmed exoplanets are heavier than Neptune
4
. Given that young protoplanetary disks are more massive than their mature counterparts, this suggests that planet formation starts early, but evidence for grain growth that is spatially and temporally coincident with a massive reservoir in young disks remains scarce. Here, we report observations on a lack of emission of carbon monoxide isotopologues within the inner ~15 au of a very young (age ~100,000 years) disk around the solar-type protostar TMC1A. By using the absence of spatially resolved molecular line emission to infer the gas and dust content of the disk, we conclude that shielding by millimetre-size grains is responsible for the lack of emission. This suggests that grain growth and millimetre-size dust grains can be spatially and temporally coincident with a mass reservoir sufficient for giant planet formation. Hence, planet formation starts during the earliest, embedded phases in the life of young stars.
Evidence for the earliest phase of planet formation, dust grain growth, has been seen in the very young and massive circumstellar disk around low-mass protostar TMC1A. Such systems, still rich in gas, are responsible for the high-mass end of the exoplanet mass distribution.
Publisher
Nature Publishing Group UK,Nature Publishing Group
Subject
