HOW EMPTY ARE DISK GAPS OPENED BY GIANT PLANETS

By J. Fung, Ji-Ming Shi, E. Chiang. 2013

155 citations recorded by the source corpus.

Gap clearing by giant planets has been proposed to explain the optically thin cavities observed in many protoplanetary disks. How much material remains in the gap determines not only how detectable young planets are in their birth environments, but also how strong co-rotation torques are, which impacts how planets can survive fast orbital migration. We determine numerically how the average surface density inside the gap, Σ{sub gap}, depends on planet-to-star mass ratio q, Shakura-Sunyaev viscosity parameter α, and disk height-to-radius aspect ratio h/r. Our results are derived from our new graphics processing unit accelerated Lagrangian hydrodynamical code PEnGUIn and are verified by independent simulations with ZEUS90. For Jupiter-like planets, we find Σ{sub gap}∝q {sup –2.2}α{sup 1.4}(h/r){sup 6.6}, and for near brown dwarf masses, Σ{sub gap}∝q {sup –1}α{sup 1.3}(h/r){sup 6.1}. Surface density contrasts inside and outside gaps can be as large as 10{sup 4}, even when the planet does not accrete. We derive a simple analytic scaling, Σ{sub gap}∝q {sup –2}α{sup 1}(h/r){sup 5}, that compares reasonably well to empirical results, especially at low Neptune-like masses, and use discrepancies to highlight areas for progress.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d09432692d7ee8c31f03d51cfaadb1d6c38152cd

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

THE MASS–METALLICITY RELATION FOR GIANT PLANETS (2015, background): “Gap opening and the planetary starvation that results remains a topic of continuing research (e.g., Crida et al. 2006; Fung et al. 2014; Duffell & Dong 2015).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, background): “The threshold for a massive planet to open a gap within the disk depends on the ability of the accretion flow to refill the gap; weaker turbulence, and hence a weaker accretion flow, would allow smaller planets to open large disk gaps (Crida et al. 2006; Kley & Nelson 2012; Fung et al. 2014).”
Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA (2015, methodology): “Fung et al. (2014) have derived an analytical prescription based on the outcome of numerical simulations of the depth of the gap, which can set constraints on the mass of the planet in combination with the viscosity in their Eq.”
MAKE SUPER-EARTHS, NOT JUPITERS: ACCRETING NEBULAR GAS ONTO SOLID CORES AT 0.1 AU AND BEYOND (2014, methodology): “More generally, our 1D models can be improved by considering 2D/3D effects such as the opening of gaps in circumstellar disks (e.g., Fung et al. 2014) and the formation of circumplanetary disks (Lissauer et al. 2009; Ormel et al. 2014).”
Multiple Disk Gaps and Rings Generated by a Single Super-Earth (2017, background): “In the Σgas snapshots and the NIR images, as viscosity decreases the gaps deepen, as expected (e.g., Fung et al. 2014; Kanagawa et al. 2015; Duffell 2015).”
Radial Migration of Gap-opening Planets in Protoplanetary Disks. I. The Case of a Single Planet (2018, methodology): “Appendix Gap Structures Induced by Migrating Planets The gap depth and width have been investigated by the hydrodynamic simulations, for various planet masses, aspect ratios, and viscosities (Duffell & MacFadyen 2013; Fung et al. 2014; Kanagawa et al. 2015a, 2016, 2017).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “…our representative model temperatures, even relatively low-mass (∼several M⊕) planets can open narrow gaps (Zhu et al. 2013; Duffell & MacFadyen 2013; Fung et al. 2014) and trap solid particles (Paardekooper & Mellema 2006; Zhu et al. 2014; Picogna & Kley 2015) to produce features similar to the…”
The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, background): “…of Equation (22) to q=0.01 is justifiable since the dust is well coupled to the gas due to the small Stokes number under DSD1, and the previous study with a grid of much higher q (Fung et al. 2014) showed that the relation between gaseous gap properties and the planet mass can extend to q=0.01.”
The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview (2018, background): “It is also sufficient to detect the continuum emission that (indirectly) traces the ∼20% pressure variations produced by & 0.1 MJup planets (Fung et al. 2014), zonal flows (Simon & Armitage 2014), or weak vortices (e.g., Goodman et al. 1987), even if (contrary to expectations) there is no…”
Gas density drops inside dust cavities of transitional disks around young stars observed with ALMA (2015, background): “The decrease in gas density due to companion clearing depends on the mass of the companion and other parameters such as the viscosity (Zhu et al. 2011; Dodson-Robinson & Salyk 2011; Pinilla et al. 2012; Mulders et al. 2013; Fung et al. 2014).”
Turbulence in the TW Hya Disk (2018, background): “…turbulence affects the collisional velocities of planetesimals (Ida et al. 2008), the radial migration of sub-Jupiter mass planets (Nelson & Papaloizou 2004; Oishi et al. 2007; Baruteau et al. 2011) and the ability of more massive planets to open a gap (e.g. Kley & Nelson 2012; Fung et al. 2014).”
Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “A more massive planet will build a steeper pressure gradient, thereby forming a deeper and wider gap than would be created by a less massive planet (Fung et al. 2014; Kanagawa et al. 2015; Rosotti et al. 2016).”
Three Radial Gaps in the Disk of TW Hydrae Imaged with SPHERE (2016, background): “For more massive planets that create deep, nearly empty gaps the numerical models create broader gaps whose flanks are shallower (e.g. Fung et al. 2014).”
Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks (2014, background): “As Fung et al. (2014) pointed out, ∆gap,Σg ∼ 2× max(RHill, hg), where RHill ∝ rpM 1/3 p is the Hill radius of the planet (see also Figure 5 in Duffell & MacFadyen 2013).”
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, background): “In particular, non-thermal motions can influence processes ranging from the collisional growth of small dust grains (Testi et al. 2014) to the ability of massive planets to open a gap (e.g., Fung et al. 2014).”
IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS (2015, background): “For type-II migration, the picture may be somewhat more rudimentary, since gap-opening planets (Crida et al. 2006; Duffell and MacFadyen 2013; Fung et al. 2014) simply get carried inwards by the accretionary flow (Mor- 11 Examples of such systems include Kepler-79 and Kepler-223. bidelli and Crida…”