TY - JOUR

T1 - Dust clearing by radial drift in evolving protoplanetary discs

AU - Appelgren, Johan

AU - Lambrechts, Michiel

AU - Johansen, Anders

N1 - Publisher Copyright: © ESO 2020.

PY - 2020

Y1 - 2020

N2 - Recent surveys have revealed that protoplanetary discs typically have dust masses that appear to be insufficient to account for the high occurrence rate of exoplanet systems. We demonstrate that this observed dust depletion is consistent with the radial drift of pebbles. Using a Monte Carlo method we simulate the evolution of a cluster of protoplanetary discs using a 1D numerical method to viscously evolve each gas disc together with the radial drift of dust particles that have grown to 100 μm in size. For a 2 Myr-old cluster of stars, we find a slightly sublinear scaling between the gas disc mass and the gas accretion rate (Mg Ṁ 0.9). However, for the dust mass we find that evolved dust discs have a much weaker scaling with the gas accretion rate, with the precise scaling depending on the age at which the cluster is sampled and the intrinsic age spread of the discs in the cluster. Ultimately, we find that the dust mass present in protoplanetary discs is on the order of 10-100 M- in 1-3 Myr-old star-forming regions, a factor of 10-100 depleted from the original dust budget. As the dust drains from the outer disc, pebbles pile up in the inner disc and locally increase the dust-to-gas ratio by up to a factor of four above the initial value. In these regions of high dust-to-gas ratio we find conditions that are favourable for planetesimal formation via the streaming instability and subsequent growth by pebble accretion. We also find the following scaling relations with stellar mass within a 1-2 Myr-old cluster: a slightly super-linear scaling between the gas accretion rate and stellar mass (Ṁ M-1.4), a slightly super-linear scaling between the gas disc mass and the stellar mass (Mg M-1.4), and a super-linear relation between the dust disc mass and stellar mass (Md M-1.4-4.1).

AB - Recent surveys have revealed that protoplanetary discs typically have dust masses that appear to be insufficient to account for the high occurrence rate of exoplanet systems. We demonstrate that this observed dust depletion is consistent with the radial drift of pebbles. Using a Monte Carlo method we simulate the evolution of a cluster of protoplanetary discs using a 1D numerical method to viscously evolve each gas disc together with the radial drift of dust particles that have grown to 100 μm in size. For a 2 Myr-old cluster of stars, we find a slightly sublinear scaling between the gas disc mass and the gas accretion rate (Mg Ṁ 0.9). However, for the dust mass we find that evolved dust discs have a much weaker scaling with the gas accretion rate, with the precise scaling depending on the age at which the cluster is sampled and the intrinsic age spread of the discs in the cluster. Ultimately, we find that the dust mass present in protoplanetary discs is on the order of 10-100 M- in 1-3 Myr-old star-forming regions, a factor of 10-100 depleted from the original dust budget. As the dust drains from the outer disc, pebbles pile up in the inner disc and locally increase the dust-to-gas ratio by up to a factor of four above the initial value. In these regions of high dust-to-gas ratio we find conditions that are favourable for planetesimal formation via the streaming instability and subsequent growth by pebble accretion. We also find the following scaling relations with stellar mass within a 1-2 Myr-old cluster: a slightly super-linear scaling between the gas accretion rate and stellar mass (Ṁ M-1.4), a slightly super-linear scaling between the gas disc mass and the stellar mass (Mg M-1.4), and a super-linear relation between the dust disc mass and stellar mass (Md M-1.4-4.1).

KW - Accretion, accretion disks

KW - Methods: numerical

KW - Planets and satellites: formation

KW - Protoplanetary disks

U2 - 10.1051/0004-6361/202037650

DO - 10.1051/0004-6361/202037650

M3 - Journal article

AN - SCOPUS:85087832275

VL - 638

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A156

ER -