Tidal barrier and the asymptotic mass of proto gas-giant planets

Ian Dobbs-Dixon, Shulin Li, Douglas N.C. Lin

    Research output: Contribution to journalArticle

    Abstract

    Although late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along with more massive and longer period companions. Here, we suggest a potential solution. We show that supersonic infall of surrounding gas onto a protoplanet is only possible interior to both its Bondi and Roche radii. Although the initial Bondi radius is much smaller than its Roche radius, the former overtakes the latter during its growth. Thereafter, a positive pressure gradient is required to induce the gas to enter the Roche lobe of the protoplanet and flow is significantly reduced. We present the results of analysis and numerical simulations to show that the accretion rate increases rapidly with the ratio of the protoplanets Roche to Bondi radii. Based on these results we suggest that in regions with low geometric aspect ratios gas accretion is quenched, resulting in relatively low protoplanetary masses.

    Original languageEnglish (US)
    Pages (from-to)263-266
    Number of pages4
    JournalProceedings of the International Astronomical Union
    Volume3
    Issue numberS249
    DOIs
    StatePublished - Jan 1 2007

    Fingerprint

    gas giant planets
    protoplanets
    planet
    gases
    gas
    radii
    accretion
    planets
    gas supply
    pressure gradient
    Jupiter
    solar system
    simulation
    Jupiter (planet)
    pressure gradients
    lobes
    aspect ratio
    ice
    depletion
    stars

    Keywords

    • Accretion
    • Planet formation

    ASJC Scopus subject areas

    • Astronomy and Astrophysics

    Cite this

    Tidal barrier and the asymptotic mass of proto gas-giant planets. / Dobbs-Dixon, Ian; Li, Shulin; Lin, Douglas N.C.

    In: Proceedings of the International Astronomical Union, Vol. 3, No. S249, 01.01.2007, p. 263-266.

    Research output: Contribution to journalArticle

    Dobbs-Dixon, Ian ; Li, Shulin ; Lin, Douglas N.C. / Tidal barrier and the asymptotic mass of proto gas-giant planets. In: Proceedings of the International Astronomical Union. 2007 ; Vol. 3, No. S249. pp. 263-266.
    @article{ee934e4e3aa84b9590261654bc047c8e,
    title = "Tidal barrier and the asymptotic mass of proto gas-giant planets",
    abstract = "Although late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along with more massive and longer period companions. Here, we suggest a potential solution. We show that supersonic infall of surrounding gas onto a protoplanet is only possible interior to both its Bondi and Roche radii. Although the initial Bondi radius is much smaller than its Roche radius, the former overtakes the latter during its growth. Thereafter, a positive pressure gradient is required to induce the gas to enter the Roche lobe of the protoplanet and flow is significantly reduced. We present the results of analysis and numerical simulations to show that the accretion rate increases rapidly with the ratio of the protoplanets Roche to Bondi radii. Based on these results we suggest that in regions with low geometric aspect ratios gas accretion is quenched, resulting in relatively low protoplanetary masses.",
    keywords = "Accretion, Planet formation",
    author = "Ian Dobbs-Dixon and Shulin Li and Lin, {Douglas N.C.}",
    year = "2007",
    month = "1",
    day = "1",
    doi = "10.1017/S174392130801572X",
    language = "English (US)",
    volume = "3",
    pages = "263--266",
    journal = "Proceedings of the International Astronomical Union",
    issn = "1743-9213",
    publisher = "Cambridge University Press",
    number = "S249",

    }

    TY - JOUR

    T1 - Tidal barrier and the asymptotic mass of proto gas-giant planets

    AU - Dobbs-Dixon, Ian

    AU - Li, Shulin

    AU - Lin, Douglas N.C.

    PY - 2007/1/1

    Y1 - 2007/1/1

    N2 - Although late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along with more massive and longer period companions. Here, we suggest a potential solution. We show that supersonic infall of surrounding gas onto a protoplanet is only possible interior to both its Bondi and Roche radii. Although the initial Bondi radius is much smaller than its Roche radius, the former overtakes the latter during its growth. Thereafter, a positive pressure gradient is required to induce the gas to enter the Roche lobe of the protoplanet and flow is significantly reduced. We present the results of analysis and numerical simulations to show that the accretion rate increases rapidly with the ratio of the protoplanets Roche to Bondi radii. Based on these results we suggest that in regions with low geometric aspect ratios gas accretion is quenched, resulting in relatively low protoplanetary masses.

    AB - Although late stage gap formation reduces the surface density in the vicinity of protoplanets, simulations suggest gas may continue to leak through the protoplanets tidal barrier, replenishing the gas supply and allowing protoplanets to acquire masses comparable to or larger than that of Jupiter. Global gas depletion is a possible explanation for gaseous planets with lower masses in weak-line T-Tauri disks and ice giants in our own solar system, but it is unlikely to have stalled the growth of multiple systems around nearby stars that contain relatively low-mass, close-in planets along with more massive and longer period companions. Here, we suggest a potential solution. We show that supersonic infall of surrounding gas onto a protoplanet is only possible interior to both its Bondi and Roche radii. Although the initial Bondi radius is much smaller than its Roche radius, the former overtakes the latter during its growth. Thereafter, a positive pressure gradient is required to induce the gas to enter the Roche lobe of the protoplanet and flow is significantly reduced. We present the results of analysis and numerical simulations to show that the accretion rate increases rapidly with the ratio of the protoplanets Roche to Bondi radii. Based on these results we suggest that in regions with low geometric aspect ratios gas accretion is quenched, resulting in relatively low protoplanetary masses.

    KW - Accretion

    KW - Planet formation

    UR - http://www.scopus.com/inward/record.url?scp=44249109071&partnerID=8YFLogxK

    UR - http://www.scopus.com/inward/citedby.url?scp=44249109071&partnerID=8YFLogxK

    U2 - 10.1017/S174392130801572X

    DO - 10.1017/S174392130801572X

    M3 - Article

    VL - 3

    SP - 263

    EP - 266

    JO - Proceedings of the International Astronomical Union

    JF - Proceedings of the International Astronomical Union

    SN - 1743-9213

    IS - S249

    ER -