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

Abstract

The Disk Substructures at High Angular Resolution Project (DSHARP) provides a large sample of protoplanetary disks having substructures which 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 2-D hydrodynamical simulations including both gas and dust components. We present the resulting gas structures, including the relationship between the planet mass and 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 and 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 probe a wide-orbit planet population (Neptune to Jupiter mass planets beyond 10 au) that is not accessible to other planet searching techniques.

Importance of radiative effects in gap opening by planets in protoplanetary disks

“…2), we expect exactly (or at least) one secondary gap in our locally isothermal simulation. The fact that we indeed observe it suggests that our results agree with Zhang et al (2018) in the locally isothermal limit. In addition, we observe the secondary gap at the location inferred by the fitting formula suggested in that study.…”

“…Our results on HD 163296 can also be compared to the 2D locally isothermal simulations by Zhang et al (2018). In Fig.…”

“…(1c)) in the absence of a planet (we can ignore compression heating in this scenario because its contribution is negligible). We adopted values inferred in Table 3 by Zhang et al (2018) for HD 163296 such that the surface density at r gap = {10, 48, 86} au is Σ(r gap ) = {100, 10, 3} g/cm 2 , respectively. We then fit a power law to these three points and find that a fit of Σ(r) HD ≈ 10 r r p −3/2 g cm 2 ≈ 3200 r au −3/2 g cm 2 (5) matches very well.…”

“…We then fit a power law to these three points and find that a fit of Σ(r) HD ≈ 10 r r p −3/2 g cm 2 ≈ 3200 r au −3/2 g cm 2 (5) matches very well. For AS 209, we simply adopt a setup similar to that by Zhang et al (2018), such that…”

“…We use numerical simulations to address the importance of proper treatment of radiative effects for two systems that mimic the properties of HD 163296 and AS 209 Zhang et al 2018) and show that an adiabatic equation of state Article number, page 1 of 10 arXiv:2003.02298v1 [astro-ph.EP] 4 Mar 2020 A&A proofs: manuscript no. isorad-astroph can produce different results with respect to a locally isothermal model when the gap-opening capabilities of a planet are modeled.…”