TY - JOUR

T1 - Formation of pebbles in (gravito-)viscous protoplanetary disks with various turbulent strengths

AU - Vorobyov, Eduard I.

AU - Elbakyan, Vardan G.

AU - Johansen, Anders

AU - Lambrechts, Michiel

AU - Skliarevskii, Aleksandr M.

AU - Stoyanovskaya, O. P.

N1 - We are thankful to the anonymous referee for useful comments that helped to improve the manuscript. E.I.V and A.M.S. acknowledge support by the Ministry of Science and Higher Education of the Russian Federation (State assignment in the field of scientific activity, Southern Federal University, VnGr /2020-03-IF, 2020). S.O.P. acknowledges support from the Ministry of Higher Education and Science of Russian Federation, project of LIH SB RAS FWGG-2021-0001 V.G.E. acknowledges the Swedish Institute for a visitor grant allowing to conduct research at Lund University and the funding from the UK Science and Technologies Facilities Council, grant No. ST/S000453/1. A.J. acknowledges funding from the European Research Foundation (ERC Consolidator Grant 724687-PLANETESYS), the Knut and Alice Wallenberg Foundation (Wallenberg Scholar Grant 2019.0442), the Swedish Research Council (Project Grant 2018-04867), the Danish National Research Foundation (DNRF Chair Grant DNRF159), and the Göran Gustafsson Foundation. ML was supported by the Knut and Alice Wallenberg Foundation (Grant 2012.0150). The simulations were performed on the Vienna Scientific Cluster (VSC-4). Публикация для корректировки.

PY - 2023/2/1

Y1 - 2023/2/1

N2 - Aims. Dust plays a crucial role in the evolution of protoplanetary disks. We study the dynamics and growth of initially submicron dust particles in self-gravitating young protoplanetary disks with various strengths of turbulent viscosity. We aim to understand the physical conditions that determine the formation and spatial distribution of pebbles when both disk self-gravity and turbulent viscosity are at work. Methods. We performed thin-disk hydrodynamics simulations of self-gravitating protoplanetary disks over an initial time period of 0.5 Myr using the FEOSAD code. Turbulent viscosity was parameterized in terms of the spatially and temporally constant α parameter, while the effects of gravitational instability on dust growth were accounted for by calculating the effective parameter αGI. We considered the evolution of the dust component, including the momentum exchange with gas, dust self-gravity, and a simplified model of dust growth. Results. We find that the level of turbulent viscosity strongly affects the spatial distribution and total mass of pebbles in the disk. The α = 10-2 model is viscosity-dominated, pebbles are completely absent, and the dust-to-gas mass ratio deviates from the reference 1:100 value by no more than 30% throughout the extent of the disk. On the contrary, the α = 10-3 model and, especially, the α = 10-4 model are dominated by gravitational instability. The effective parameter α + αGI is now a strongly varying function of radial distance. As a consequence, a bottleneck effect develops in the innermost disk regions, which makes gas and dust accumulate in a ring-like structure. Pebbles are abundant in these models, although their total mass and spatial extent is sensitive to the dust fragmentation velocity and to the strength of gravitoturbulence. The use of the standard dust-to-gas mass conversion is not suitable for estimating the mass of pebbles. Conclusions. Our numerical experiments demonstrate that pebbles can already be abundant in protoplanetary disks at the initial stages of disk evolution. Dust growth models that consider disk self-gravity and ice mantles may be important for studying planet formation via pebble accretion.

AB - Aims. Dust plays a crucial role in the evolution of protoplanetary disks. We study the dynamics and growth of initially submicron dust particles in self-gravitating young protoplanetary disks with various strengths of turbulent viscosity. We aim to understand the physical conditions that determine the formation and spatial distribution of pebbles when both disk self-gravity and turbulent viscosity are at work. Methods. We performed thin-disk hydrodynamics simulations of self-gravitating protoplanetary disks over an initial time period of 0.5 Myr using the FEOSAD code. Turbulent viscosity was parameterized in terms of the spatially and temporally constant α parameter, while the effects of gravitational instability on dust growth were accounted for by calculating the effective parameter αGI. We considered the evolution of the dust component, including the momentum exchange with gas, dust self-gravity, and a simplified model of dust growth. Results. We find that the level of turbulent viscosity strongly affects the spatial distribution and total mass of pebbles in the disk. The α = 10-2 model is viscosity-dominated, pebbles are completely absent, and the dust-to-gas mass ratio deviates from the reference 1:100 value by no more than 30% throughout the extent of the disk. On the contrary, the α = 10-3 model and, especially, the α = 10-4 model are dominated by gravitational instability. The effective parameter α + αGI is now a strongly varying function of radial distance. As a consequence, a bottleneck effect develops in the innermost disk regions, which makes gas and dust accumulate in a ring-like structure. Pebbles are abundant in these models, although their total mass and spatial extent is sensitive to the dust fragmentation velocity and to the strength of gravitoturbulence. The use of the standard dust-to-gas mass conversion is not suitable for estimating the mass of pebbles. Conclusions. Our numerical experiments demonstrate that pebbles can already be abundant in protoplanetary disks at the initial stages of disk evolution. Dust growth models that consider disk self-gravity and ice mantles may be important for studying planet formation via pebble accretion.

KW - Hydrodynamics

KW - Protoplanetary disks

KW - Stars: formation

UR - https://www.scopus.com/record/display.uri?eid=2-s2.0-85148852768&origin=inward&txGid=68bd637b209e8a450bd152c022700058

UR - https://www.mendeley.com/catalogue/154276e8-b3d0-3722-9c7c-70035e8f6a6e/

U2 - 10.1051/0004-6361/202244500

DO - 10.1051/0004-6361/202244500

M3 - Article

VL - 670

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A81

ER -