Possible formation pathways for the low-density Neptune-mass planet HAT-P-26b

Mohamad Ali-Dib, Gunjan Lakhlani

    Research output: Contribution to journalArticlepeer-review

    Abstract

    We investigate possible pathways for the formation of the low-density Neptune-mass planet HAT-P-26b. We use two different formation models based on pebble and planetesimal accretion, and includes gas accretion, disc migration and simple photoevaporation. The models track the atmospheric oxygen abundance, in addition to the orbital period, and mass of the forming planets, which we compare to HAT-P-26b. We find that pebble accretion can explain this planet more naturally than planetesimal accretion that fails completely unless we artificially enhance the disc metallicity significantly. Pebble accretion models can reproduce HAT-P-26b with either a high initial core mass and low amount of envelope enrichment through core erosion or pebbles dissolution, or the opposite, with both scenarios being possible. Assuming a low envelope enrichment factor as expected from convection theory and comparable to the values we can infer from the D/H measurements in Uranus and Neptune, our most probable formation pathway for HAT-P-26b is through pebble accretion starting around 10 au early in the disc's lifetime.

    Original languageEnglish (US)
    Pages (from-to)1325-1331
    Number of pages7
    JournalMonthly Notices of the Royal Astronomical Society
    Volume473
    Issue number1
    DOIs
    StatePublished - Jan 1 2018

    Keywords

    • Planets and satellites: composition
    • Planets and satellites: formation

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Space and Planetary Science

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