REVIEW 7 cited by
Streaming Instabilities in Protoplanetary Disks
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
Signed reviews
read the original abstract
Interpenetrating streams of solids and gas in a Keplerian disk produce a local, linear instability. The two components mutually interact via aerodynamic drag, which generates radial drift and triggers unstable modes. The secular instability does not require self-gravity, yet it generates growing particle density perturbations that could seed planetesimal formation. Growth rates are slower than dynamical, but faster than radial drift, timescales. Growth rates, like streaming velocities, are maximized for marginal coupling (stopping times comparable dynamical times). Fastest growth occurs when the solid to gas density ratio is order unity and feedback is strongest. Curiously, growth is strongly suppressed when the densities are too nearly equal. The relation between background drift and wave properties is explained by analogy with Howard's semicircle theorem. The three-dimensional, two-fluid equations describe a sixth order (in the complex frequency) dispersion relation. A terminal velocity approximation allows simplification to an approximate cubic dispersion relation. To describe the simplest manifestation of this instability, we ignore complicating (but possibly relevant) factors like vertical stratification, dispersion of particle sizes, turbulence, and self-gravity. We consider applications to planetesimal formation and compare our work to other studies of particle-gas dynamics.
Forward citations
Cited by 7 Pith papers
-
Geometry of dust rings in protoplanetary disks: the case of LkCa 15
The 69 au dust ring in LkCa 15 is broad and thick at 0.88 mm and progressively narrower and thinner at 1.34 and 3.08 mm, implying a massive population of small grains alongside a more concentrated large-grain population.
-
SMA 200-400 GHz Survey for 10 faint Class II Disks in the Taurus Molecular Cloud
Faint Class II disks in Taurus show the same 198-358 GHz spectral index distribution as brighter disks, suggesting they too are optically thick at submillimeter wavelengths.
-
Dust and Gas Transport in Substructured Nonideal MHD Wind-Launching Disks with Embedded Planets
In magnetized wind-launching disks, planet-opened gaps remain partially permeable: small grains and gas leak through, while large grains are filtered, making substructures regulators rather than barriers.
-
Full one-fluid dusty gas with multiple grain species in SPH
Presents and benchmarks an SPH code for the full one-fluid dusty gas with multiple species that conserves mass, momentum, angular momentum and energy while recovering analytic solutions where the terminal velocity app...
-
Formation of multiple dust rings and gaps in protoplanetary discs by a single migrating planet II: radiative discs and observational signatures
One migrating planet produces multiple observable dust rings and gaps lasting ≥400 kyr; cooling controls jump number but not structure lifetime.
-
Dust Growth in Binary Systems: Inhibition of dust settling and growth in circumbinary discs
Dust grains in circumbinary discs end up five times smaller than in single-star discs, and the conditions for streaming-instability clumping are not met, arguing against in-situ planet formation there.
-
Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation
2D radiation-hydrodynamical simulations find accretion outbursts unstable to Rossby-wave instability, forming vortices that suppress planetesimal formation until post-burst quiescence.
Discussion (0). Continue with ORCID to comment.