Dust-void evolution driven by turbulent dust flux can induce runaway migration of Earth-mass planets

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F25%3A10510782" target="_blank" >RIV/00216208:11320/25:10510782 - isvavai.cz</a>

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=eb4SDQ1dQs" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=eb4SDQ1dQs</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202451869" target="_blank" >10.1051/0004-6361/202451869</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Dust-void evolution driven by turbulent dust flux can induce runaway migration of Earth-mass planets

Popis výsledku v původním jazyce

Torques from asymmetric dust structures (so-called dust-void and filamentary structures) formed around low-mass planets embedded in a nonturbulent dust-gas disk can exceed the torques produced by the gas disk component and then go on to dominate the planet&apos;s orbital dynamics. Here, we investigate how these structures (hence the dust torque) change when the effect of turbulent dust diffusion and dust feedback are included, along with the direct implications on the migration of Earth-like planets. Using the FARGO3D code, we performed 2D and 3D multifluid hydrodynamic simulations, focusing on a non-migrating planet with a mass of M-p = 1.5 M-circle plus in 2D and on migrating planets with M-p is an element of [1.5, 12] M-circle plus in 3D. We varied the delta-dimensionless diffusivity parameter in the range [0, 3 x 10(-3)] and considered three different Stokes numbers, St = {0.04, 0.26, 0.55}, which are representative of the gas-dominated, the transitional, and the gravity-dominated regimes, respectively. In our 2D models, we find that turbulent diffusion of dust prevents the formation of the dust-void and filamentary structures when delta &gt; 3 x 10(-4). Otherwise, dust structures survive turbulent diffusion flow. However, dust and total torques become positive only in transitional and gravity-dominated regimes. In our 3D models, we find that the dust-void is drastically modified and the high-density ring-shaped barrier delineating the dust-void disappears if delta greater than or similar to 10(-4), due to the effect of dust turbulent diffusion along with the back-reaction of the dust. For all values of delta, the filament in front of the planet is replaced by a low-density trench. Remarkably, as we have allowed the planets to migrate, the evolving dust-void can drive either runaway migration or outward (inward) oscillatory-torque migration. Our study thus suggests that low-mass Earth-like planets can undergo runaway migration in dusty disks.

Název v anglickém jazyce

Dust-void evolution driven by turbulent dust flux can induce runaway migration of Earth-mass planets

Popis výsledku anglicky

Torques from asymmetric dust structures (so-called dust-void and filamentary structures) formed around low-mass planets embedded in a nonturbulent dust-gas disk can exceed the torques produced by the gas disk component and then go on to dominate the planet&apos;s orbital dynamics. Here, we investigate how these structures (hence the dust torque) change when the effect of turbulent dust diffusion and dust feedback are included, along with the direct implications on the migration of Earth-like planets. Using the FARGO3D code, we performed 2D and 3D multifluid hydrodynamic simulations, focusing on a non-migrating planet with a mass of M-p = 1.5 M-circle plus in 2D and on migrating planets with M-p is an element of [1.5, 12] M-circle plus in 3D. We varied the delta-dimensionless diffusivity parameter in the range [0, 3 x 10(-3)] and considered three different Stokes numbers, St = {0.04, 0.26, 0.55}, which are representative of the gas-dominated, the transitional, and the gravity-dominated regimes, respectively. In our 2D models, we find that turbulent diffusion of dust prevents the formation of the dust-void and filamentary structures when delta &gt; 3 x 10(-4). Otherwise, dust structures survive turbulent diffusion flow. However, dust and total torques become positive only in transitional and gravity-dominated regimes. In our 3D models, we find that the dust-void is drastically modified and the high-density ring-shaped barrier delineating the dust-void disappears if delta greater than or similar to 10(-4), due to the effect of dust turbulent diffusion along with the back-reaction of the dust. For all values of delta, the filament in front of the planet is replaced by a low-density trench. Remarkably, as we have allowed the planets to migrate, the evolving dust-void can drive either runaway migration or outward (inward) oscillatory-torque migration. Our study thus suggests that low-mass Earth-like planets can undergo runaway migration in dusty disks.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GM21-23067M" target="_blank" >GM21-23067M: Hydrodynamické interakce planet s protoplanetárními disky a původ těsných exoplanetárních soustav</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2025

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

698

Číslo periodika v rámci svazku

kveten

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

13

Strana od-do

A21

Kód UT WoS článku

001495082400009

EID výsledku v databázi Scopus

2-s2.0-105006785100