Global calculations of density waves and gap formation in protoplanetary disks using a moving Mesh

Paul C. Duffell, Andrew I. MacFadyen

    Research output: Contribution to journalArticle

    Abstract

    We calculate the global quasi-steady state of a thin disk perturbed by a low-mass protoplanet orbiting at a fixed radius using extremely high resolution numerical integrations of Euler's equations in two dimensions. The calculations are carried out using a moving computational domain, which greatly reduces advection errors and allows for much longer time steps than a fixed grid. We calculate the angular momentum flux and the torque density as a function of radius and compare them with analytical predictions. We discuss the quasi-steady state after 100 orbits and the prospects for gap formation by low-mass planets.

    Original languageEnglish (US)
    Article number7
    JournalAstrophysical Journal
    Volume755
    Issue number1
    DOIs
    StatePublished - Aug 10 2012

    Fingerprint

    quasi-steady states
    protoplanetary disks
    mesh
    radii
    protoplanets
    advection
    numerical integration
    torque
    angular momentum
    planets
    planet
    grids
    orbits
    high resolution
    prediction
    predictions
    calculation

    Keywords

    • hydrodynamics
    • methods: numerical
    • planet-disk interactions
    • planets and satellites: formation
    • protoplanetary disks

    ASJC Scopus subject areas

    • Space and Planetary Science
    • Astronomy and Astrophysics

    Cite this

    Global calculations of density waves and gap formation in protoplanetary disks using a moving Mesh. / Duffell, Paul C.; MacFadyen, Andrew I.

    In: Astrophysical Journal, Vol. 755, No. 1, 7, 10.08.2012.

    Research output: Contribution to journalArticle

    @article{6fc4869e18fb4b73a23b8464eb474691,
    title = "Global calculations of density waves and gap formation in protoplanetary disks using a moving Mesh",
    abstract = "We calculate the global quasi-steady state of a thin disk perturbed by a low-mass protoplanet orbiting at a fixed radius using extremely high resolution numerical integrations of Euler's equations in two dimensions. The calculations are carried out using a moving computational domain, which greatly reduces advection errors and allows for much longer time steps than a fixed grid. We calculate the angular momentum flux and the torque density as a function of radius and compare them with analytical predictions. We discuss the quasi-steady state after 100 orbits and the prospects for gap formation by low-mass planets.",
    keywords = "hydrodynamics, methods: numerical, planet-disk interactions, planets and satellites: formation, protoplanetary disks",
    author = "Duffell, {Paul C.} and MacFadyen, {Andrew I.}",
    year = "2012",
    month = "8",
    day = "10",
    doi = "10.1088/0004-637X/755/1/7",
    language = "English (US)",
    volume = "755",
    journal = "Astrophysical Journal",
    issn = "0004-637X",
    publisher = "IOP Publishing Ltd.",
    number = "1",

    }

    TY - JOUR

    T1 - Global calculations of density waves and gap formation in protoplanetary disks using a moving Mesh

    AU - Duffell, Paul C.

    AU - MacFadyen, Andrew I.

    PY - 2012/8/10

    Y1 - 2012/8/10

    N2 - We calculate the global quasi-steady state of a thin disk perturbed by a low-mass protoplanet orbiting at a fixed radius using extremely high resolution numerical integrations of Euler's equations in two dimensions. The calculations are carried out using a moving computational domain, which greatly reduces advection errors and allows for much longer time steps than a fixed grid. We calculate the angular momentum flux and the torque density as a function of radius and compare them with analytical predictions. We discuss the quasi-steady state after 100 orbits and the prospects for gap formation by low-mass planets.

    AB - We calculate the global quasi-steady state of a thin disk perturbed by a low-mass protoplanet orbiting at a fixed radius using extremely high resolution numerical integrations of Euler's equations in two dimensions. The calculations are carried out using a moving computational domain, which greatly reduces advection errors and allows for much longer time steps than a fixed grid. We calculate the angular momentum flux and the torque density as a function of radius and compare them with analytical predictions. We discuss the quasi-steady state after 100 orbits and the prospects for gap formation by low-mass planets.

    KW - hydrodynamics

    KW - methods: numerical

    KW - planet-disk interactions

    KW - planets and satellites: formation

    KW - protoplanetary disks

    UR - http://www.scopus.com/inward/record.url?scp=84864448758&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=84864448758&partnerID=8YFLogxK

    U2 - 10.1088/0004-637X/755/1/7

    DO - 10.1088/0004-637X/755/1/7

    M3 - Article

    VL - 755

    JO - Astrophysical Journal

    JF - Astrophysical Journal

    SN - 0004-637X

    IS - 1

    M1 - 7

    ER -