Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 731720.0, MPI für Astronomie / Publikationen_mpia
The VLA view of the HL Tau disk: Disk mass, grain evolution, and early planet formation
Authors:Carrasco-González, C.; Henning, T.; Chandler, C. J.; Linz, H.; Pérez, L.; Rodríguez, L. F.; Galván-Madrid, R.; Anglada, G.; Birnstiel, T.; van Boekel, R.; Flock, M.; Klahr, H.; Macias, E.; Menten, K.; Osorio, M.; Testi, L.; Torrelles, J. M.; Zhu, Z.
Date of Publication (YYYY-MM-DD):2016
Title of Journal:The Astrophysical Journal Letters
Issue / Number:1
Start Page:id. L16 (6 pp)
Audience:Not Specified
Abstract / Description:The first long-baseline ALMA campaign resolved the disk around the young star HL Tau into a number of axisymmetric bright and dark rings. Despite the very young age of HL Tau, these structures have been interpreted as signatures for the presence of (proto)planets. The ALMA images triggered numerous theoretical studies based on disk–planet interactions, magnetically driven disk structures, and grain evolution. Of special interest are the inner parts of disks, where terrestrial planets are expected to form. However, the emission from these regions in HL Tau turned out to be optically thick at all ALMA wavelengths, preventing the derivation of surface density profiles and grain-size distributions. Here, we present the most sensitive images of HL Tau obtained to date with the Karl G. Jansky Very Large Array at 7.0 mm wavelength with a spatial resolution comparable to the ALMA images. At this long wavelength, the dust emission from HL Tau is optically thin, allowing a comprehensive study of the inner disk. We obtain a total disk dust mass of (1–3) × 10‑3 M , depending on the assumed opacity and disk temperature. Our optically thin data also indicate fast grain growth, fragmentation, and formation of dense clumps in the inner densest parts of the disk. Our results suggest that the HL Tau disk may be actually in a very early stage of planetary formation, with planets not already formed in the gaps but in the process of future formation in the bright rings.
Free Keywords:planets and satellites: formation; protoplanetary disks; stars: formation; stars: individual: HL Tau; stars: protostars; techniques: interferometric
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X %R 10.3847/2041-8205/821/1/L16
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.