English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We study the turbulence induced in the dust layer of a protoplanetary diskbased on the energetics of dust accretion due to gas drag. We estimateturbulence strength from the energy supplied by dust accretion, using theradial drift velocity of the dust particles in a laminar disk. Our estimate ofthe turbulence strength agrees with previous analytical and numerical researchon the turbulence induced by Kelvin-Helmholtz and/or streaming instabilitiesfor particles whose stopping time is less than the Keplerian time. For suchsmall particles, the strongest turbulence is expected to occur when thedust-to-gas ratio of the disk is ~C_eff^(1/2) (h_g / r) ~ 10^(-2), where C_eff~ 0.2 represents the energy supply efficiency to turbulence and h_g / r ~ 5 x10^(-2) is the aspect ratio of the gas disk. The maximum viscosity parameter isalpha_max ~ C_eff T_s (h_g / r)^2 ~ 10^(-4) T_s, where T_s (<1) is thenon-dimensional stopping time of the dust particles. Modification in thedust-to-gas ratio from the standard value, 10^(-2), by any process, results inweaker turbulence and a thinner dust layer, and consequently may accelerate thegrowth process of the dust particles.

Induced Turbulence and the Density Structure of the Dust Layer in a Protoplanetary Disk