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Title: Planetary Torque in 3D Isentropic Disks

Abstract

Planetary migration is inherently a three-dimensional (3D) problem, because Earth-size planetary cores are deeply embedded in protoplanetary disks. Simulations of these 3D disks remain challenging due to the steep resolution requirements. Using two different hydrodynamics codes, FARGO3D and PEnGUIn, we simulate disk–planet interaction for a one to five Earth-mass planet embedded in an isentropic disk. We measure the torque on the planet and ensure that the measurements are converged both in resolution and between the two codes. We find that the torque is independent of the smoothing length of the planet’s potential ( r {sub s}), and that it has a weak dependence on the adiabatic index of the gaseous disk ( γ ). The torque values correspond to an inward migration rate qualitatively similar to previous linear calculations. We perform additional simulations with explicit radiative transfer using FARGOCA, and again find agreement between 3D simulations and existing torque formulae. We also present the flow pattern around the planets that show active flow is present within the planet’s Hill sphere, and meridional vortices are shed downstream. The vertical flow speed near the planet is faster for a smaller r {sub s} or γ , up to supersonic speeds for themore » smallest r {sub s} and γ in our study.« less

Authors:
 [1]; ;  [2];  [3]
  1. Department of Astronomy, University of California at Berkeley, Campbell Hall, Berkeley, CA 94720-3411 (United States)
  2. Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Av. Universidad s/n, 62210 Cuernavaca, Mor. (Mexico)
  3. Université de la Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange UMR 7293, Nice (France)
Publication Date:
OSTI Identifier:
22663758
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (Online); Journal Volume: 153; Journal Issue: 3; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; COMPUTERIZED SIMULATION; F CODES; HYDRODYNAMICS; INDEXES; ISENTROPIC PROCESSES; MASS; P CODES; PLANETS; PROTOPLANETS; RADIANT HEAT TRANSFER; RESOLUTION; SATELLITES; THREE-DIMENSIONAL CALCULATIONS; TORQUE; VORTICES

Citation Formats

Fung, Jeffrey, Masset, Frédéric, Velasco, David, and Lega, Elena, E-mail: jeffrey.fung@berkeley.edu. Planetary Torque in 3D Isentropic Disks. United States: N. p., 2017. Web. doi:10.3847/1538-3881/153/3/124.
Fung, Jeffrey, Masset, Frédéric, Velasco, David, & Lega, Elena, E-mail: jeffrey.fung@berkeley.edu. Planetary Torque in 3D Isentropic Disks. United States. doi:10.3847/1538-3881/153/3/124.
Fung, Jeffrey, Masset, Frédéric, Velasco, David, and Lega, Elena, E-mail: jeffrey.fung@berkeley.edu. Wed . "Planetary Torque in 3D Isentropic Disks". United States. doi:10.3847/1538-3881/153/3/124.
@article{osti_22663758,
title = {Planetary Torque in 3D Isentropic Disks},
author = {Fung, Jeffrey and Masset, Frédéric and Velasco, David and Lega, Elena, E-mail: jeffrey.fung@berkeley.edu},
abstractNote = {Planetary migration is inherently a three-dimensional (3D) problem, because Earth-size planetary cores are deeply embedded in protoplanetary disks. Simulations of these 3D disks remain challenging due to the steep resolution requirements. Using two different hydrodynamics codes, FARGO3D and PEnGUIn, we simulate disk–planet interaction for a one to five Earth-mass planet embedded in an isentropic disk. We measure the torque on the planet and ensure that the measurements are converged both in resolution and between the two codes. We find that the torque is independent of the smoothing length of the planet’s potential ( r {sub s}), and that it has a weak dependence on the adiabatic index of the gaseous disk ( γ ). The torque values correspond to an inward migration rate qualitatively similar to previous linear calculations. We perform additional simulations with explicit radiative transfer using FARGOCA, and again find agreement between 3D simulations and existing torque formulae. We also present the flow pattern around the planets that show active flow is present within the planet’s Hill sphere, and meridional vortices are shed downstream. The vertical flow speed near the planet is faster for a smaller r {sub s} or γ , up to supersonic speeds for the smallest r {sub s} and γ in our study.},
doi = {10.3847/1538-3881/153/3/124},
journal = {Astronomical Journal (Online)},
number = 3,
volume = 153,
place = {United States},
year = {Wed Mar 01 00:00:00 EST 2017},
month = {Wed Mar 01 00:00:00 EST 2017}
}