Dust settling instability in protoplanetary discs
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Dust settling instability in protoplanetary discs. / Krapp, Leonardo; Youdin, Andrew N.; Kratter, Kaidin M.; Benitez-Llambay, Pablo.
I: Monthly Notices of the Royal Astronomical Society, Bind 497, Nr. 3, 09.2020, s. 2715-2729.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Dust settling instability in protoplanetary discs
AU - Krapp, Leonardo
AU - Youdin, Andrew N.
AU - Kratter, Kaidin M.
AU - Benitez-Llambay, Pablo
PY - 2020/9
Y1 - 2020/9
N2 - The streaming instability (SI) has been extensively studied in the linear and non-linear regimes as a mechanism to concentrate solids and trigger planetesimal formation in the mid-plane of protoplanetary discs. A related dust settling instability (DSI) applies to particles while settling towards the mid-plane. The DSI has previously been studied in the linear regime, with predictions that it could trigger particle clumping away from the mid-plane. This work presents a range of linear calculations and non-linear simulations, performed with FARGO3D, to assess conditions for DSI growth. We expand on previous linear analyses by including particle size distributions and performing a detailed study of the amount of background turbulence needed to stabilize the DSI. When including binned size distributions, the DSI often produces converged growth rates with fewer bins than the standard SI. With background turbulence, we find that the most favourable conditions for DSI growth are weak turbulence, characterized by alpha less than or similar to 10(-6) with intermediate-sized grains that settle from one gas scale height. These conditions could arise during a sudden decrease in disc turbulence following an accretion outburst. Ignoring background turbulence, we performed a parameter survey of local 2D DSI simulations. Particle clumping was either weak or occurred slower than particles settle. Clumping was reduced by a factor of 2 in a comparison 3D simulation. Overall, our results strongly disfavour the hypothesis that the DSI significantly promotes planetesimal formation. Non-linear simulations of the DSI with different numerical methods could support or challenge these findings.
AB - The streaming instability (SI) has been extensively studied in the linear and non-linear regimes as a mechanism to concentrate solids and trigger planetesimal formation in the mid-plane of protoplanetary discs. A related dust settling instability (DSI) applies to particles while settling towards the mid-plane. The DSI has previously been studied in the linear regime, with predictions that it could trigger particle clumping away from the mid-plane. This work presents a range of linear calculations and non-linear simulations, performed with FARGO3D, to assess conditions for DSI growth. We expand on previous linear analyses by including particle size distributions and performing a detailed study of the amount of background turbulence needed to stabilize the DSI. When including binned size distributions, the DSI often produces converged growth rates with fewer bins than the standard SI. With background turbulence, we find that the most favourable conditions for DSI growth are weak turbulence, characterized by alpha less than or similar to 10(-6) with intermediate-sized grains that settle from one gas scale height. These conditions could arise during a sudden decrease in disc turbulence following an accretion outburst. Ignoring background turbulence, we performed a parameter survey of local 2D DSI simulations. Particle clumping was either weak or occurred slower than particles settle. Clumping was reduced by a factor of 2 in a comparison 3D simulation. Overall, our results strongly disfavour the hypothesis that the DSI significantly promotes planetesimal formation. Non-linear simulations of the DSI with different numerical methods could support or challenge these findings.
KW - hydrodynamics
KW - methods: numerical
KW - planets and satellites: formation
KW - protoplanetary discs
KW - circumstellar matter
KW - PLANETESIMAL FORMATION
KW - STREAMING INSTABILITY
KW - NONLINEAR EVOLUTION
KW - TURBULENCE DRIVEN
KW - SOLAR
KW - GAS
KW - DISKS
KW - ACCRETION
KW - DYNAMICS
KW - GROWTH
U2 - 10.1093/mnras/staa1854
DO - 10.1093/mnras/staa1854
M3 - Journal article
VL - 497
SP - 2715
EP - 2729
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 3
ER -
ID: 250544204