AffiliationUniv Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA
Keywordsplanets and satellites: formation
stars: individual (GY 91)
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationThe Astrophysical Journal, 857:18 (7pp), 2018 April 10
Rights© 2018. The American Astronomical Society. All rights reserved
Collection InformationThis 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 firstname.lastname@example.org.
AbstractWe present the highest spatial resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations to date of the Class I protostar GY 91 in the rho Ophiuchus L1688 molecular cloud complex. Our 870 mu m and 3 mm dust continuum maps show that the GY 91 disk has a radius of similar to 80 au, and an inclination of similar to 40 degrees, but most interestingly that the disk has three dark lanes located at 10, 40, and 70 au. We model these features assuming they are gaps in the disk surface density profile and find that their widths are 7, 30, and 10 au. These gaps bear a striking resemblance to the gaps seen in the HL Tau disk, suggesting that there may be Saturn-mass planets hiding in the disk. To constrain the relative ages of GY 91 and HL Tau, we also model the disk and envelope of HL Tau and find that they are of similar ages, although GY 91. may be younger. Although snow lines and magnetic dead zones can also produce dark lanes, if planets are indeed carving these gaps then Saturn-mass planets must form within the first similar to 0.5 Myr of the lifetime of protoplanetary disks.
VersionFinal published version
SponsorsNSF AAG