The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

Authors

Shangjia Zhang, University of Nevada, Las Vegas
Zhaohuan Zhu, University of Nevada, Las VegasFollow
Jane Huang, Universidad de Chile
Viviana V. Guzmán, Joint ALMA Observatory; Pontificia Universidad Católica de Chile
Sean M. Andrews, Harvard-Smithsonian Center for AstrophysicsFollow
Tilman Birnstiel, Ludwig-Maximilians-Universität MünchenFollow
Cornelis P. Dullemond, Heidelberg University
John M. Carpenter, Joint ALMA ObservatoryFollow
Andrea Isella, Rice UniversityFollow
Laura M. Pérez, Universidad de ChileFollow
Myriam Benisty, Unidad Mixta Internacional Franco-Chilena de Astronomía, CNRS/INSU UMIFollow
David J. Wilner, Harvard-Smithsonian Center for AstrophysicsFollow
Clément Baruteau, CNRS/Institut de Recherche en Astrophysique et Planétologie
Xue-Ning Bai, Tsinghua UniversityFollow
Luca Ricci, California State University NorthridgeFollow

Document Type

Article

Publication Date

12-26-2018

Publication Title

Astrophysical Journal Letters

Volume

869

Issue

2

First page number:

1

Last page number:

32

Abstract

The Disk Substructures at High Angular Resolution Project (DSHARP) provides a large sample of protoplanetary disks with substructures that could be induced by young forming planets. To explore the properties of planets that may be responsible for these substructures, we systematically carry out a grid of 2D hydrodynamical simulations, including both gas and dust components. We present the resulting gas structures, including the relationship between the planet mass, as well as (1) the gaseous gap depth/width and (2) the sub/super-Keplerian motion across the gap. We then compute dust continuum intensity maps at the frequency of the DSHARP observations. We provide the relationship between the planet mass, as well as (1) the depth/width of the gaps at millimeter intensity maps, (2) the gap edge ellipticity and asymmetry, and (3) the position of secondary gaps induced by the planet. With these relationships, we lay out the procedure to constrain the planet mass using gap properties, and study the potential planets in the DSHARP disks. We highlight the excellent agreement between observations and simulations for AS 209 and the detectability of the young solar system analog. Finally, under the assumption that the detected gaps are induced by young planets, we characterize the young planet population in the planet mass–semimajor axis diagram. We find that the occurrence rate for >5 M J planets beyond 5–10 au is consistent with direct imaging constraints. Disk substructures allow us to probe a wide-orbit planet population (Neptune to Jupiter mass planets beyond 10 au) that is not accessible to other planet searching techniques.

Keywords

Hydrodynamics; Planet-disk interactions; Planets and satellites: Detection; Planets and satellites: Formation; Protoplanetary disks; Submillimeter: Planetary systems

Disciplines

Astrophysics and Astronomy

File Format

PDF

File Size

9.394 Kb

Language

English

Repository Citation

Zhang, S., Zhu, Z., Huang, J., Guzmán, V. V., Andrews, S. M., Birnstiel, T., Dullemond, C. P., Carpenter, J. M., Isella, A., Pérez, L. M., Benisty, M., Wilner, D. J., Baruteau, C., Bai, X., Ricci, L. (2018). The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation. Astrophysical Journal Letters, 869(2), 1-32.
http://dx.doi.org/10.3847/2041-8213/aaf744