{
  "id": "2112.00747",
  "version": "v1",
  "published": "2021-12-01T19:00:01.000Z",
  "updated": "2021-12-01T19:00:01.000Z",
  "title": "Kepler-167e as a Probe of the Formation Histories of Cold Giants with Inner Super-Earths",
  "authors": [
    "Yayaati Chachan",
    "Paul A. Dalba",
    "Heather A. Knutson",
    "Benjamin J. Fulton",
    "Daniel Thorngren",
    "Charles Beichman",
    "David R. Ciardi",
    "Andrew W. Howard",
    "Judah Van Zandt"
  ],
  "comment": "accepted for publication in ApJ, 19 pages, 10 figures. Table 1 will be provided in MRT format upon publication",
  "journal": "ApJ, 926, 62 (2022)",
  "doi": "10.3847/1538-4357/ac3ed6",
  "categories": [
    "astro-ph.EP"
  ],
  "abstract": "The observed correlation between outer giant planets and inner super-Earths is emerging as an important constraint on planet formation theories. In this study we focus on Kepler-167, which is currently the only system known to contain both inner transiting super-Earths and a confirmed outer transiting gas giant companion beyond 1 au. Using long term radial velocity monitoring, we measure the mass of the gas giant Kepler-167e ($P=1071$ days) to be $1.01^{+0.16}_{-0.15}$ M$_{\\rm J}$, thus confirming it as a Jupiter analog. We re-fit the $Kepler$ photometry to obtain updated radii for all four planets. Using a planetary structure model, we estimate that Kepler-167e contains $66\\pm19$ M$_{\\oplus}$ of solids and is significantly enriched in metals relative to its solar-metallicity host star. We use these new constraints to explore the broader question of how systems like Kepler-167 form in the pebble accretion framework for giant planet core formation. We utilize simple disk evolution models to demonstrate that more massive and metal-rich disks, which are the most favorable sites for giant planet formation, can also deliver enough solids to the inner disk to form systems of super-Earths. We use these same models to constrain the nature of Kepler-167's protoplanetary disk, and find that it likely contained $\\gtrsim 300$ M$_{\\oplus}$ of dust and was $\\gtrsim 40$ au in size. These values overlap with the upper end of the observed dust mass and size distributions of Class 0 and I disks, and are also consistent with the observed occurrence rate of Jupiter analogs around sun-like stars.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2021-12-01T19:00:01.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "inner super-earths",
      "simple disk evolution models",
      "cold giants",
      "formation histories",
      "outer transiting gas giant"
    ],
    "tags": [
      "journal article"
    ],
    "note": {
      "typesetting": "TeX",
      "pages": 19,
      "language": "en",
      "license": "arXiv",
      "status": "editable"
    }
  }
}