{
  "id": "1408.1215",
  "version": "v2",
  "published": "2014-08-06T08:58:55.000Z",
  "updated": "2014-09-11T09:42:17.000Z",
  "title": "Terrestrial Planet Formation in the Presence of Migrating Super-earths",
  "authors": [
    "André Izidoro",
    "Alessandro Morbidelli",
    "Sean N. Raymond"
  ],
  "comment": "Accepted for publication in The Astrophysical Journal; proof corrected version",
  "categories": [
    "astro-ph.EP"
  ],
  "abstract": "Super-Earths with orbital periods less than 100 days are extremely abundant around Sun-like stars. It is unlikely that these planets formed at their current locations. Rather, they likely formed at large distances from the star and subsequently migrated inward. Here we use N-body simulations to study the effect of super-Earths on the accretion of rocky planets. In our simulations, one or more super-Earths migrates inward through a disk of planetary embryos and planetesimals embedded in a gaseous disk. We tested a wide range of migration speeds and configurations. Fast-migrating super-Earths ($\\tau_{mig} \\sim$0.01-0.1 Myr) only have a modest effect on the protoplanetary embryos and planetesimals. Sufficient material survives to form rocky, Earth-like planets on orbits exterior to the super-Earths'. In contrast, slowly migrating super-Earths shepherd rocky material interior to their orbits and strongly deplete the terrestrial planet-forming zone. In this situation any Earth-sized planets in the habitable zone are extremely volatile-rich and are therefore probably not Earth-like.",
  "revisions": [
    {
      "version": "v1",
      "updated": "2014-08-06T08:58:55.000Z",
      "abstract": "Super-Earths with orbital periods less than 100 days are extremely abundant around Sun-like stars. It is unlikely that these planets formed at their current locations. Rather, they likely formed at large distances from the star and subsequently migrated inward. Here we use N-body simulations to study the effect of super-Earths on the accretion of rocky planets. In our simulations, one or more super-Earths migrates inward through a disk of planetary embryos and planetesimals embedded in a gaseous disk. We tested a wide range of migration speeds and configurations. Fast-migrating super-Earths ($\\tau_{mig} \\sim$0.01-0.1 Myr) only have a modest effect on the protoplanetary embryos and planetesimals. Sufficient material survives to form rocky, Earth-like planets on orbits exterior to the super-Earths'. In contrast, slowly-migrating super-Earths shepherd rocky material interior to their orbits and strongly deplete the terrestrial planet-forming zone. In this situation any Earth-sized planets in the habitable zone are extremely volatile-rich and are therefore probably not Earth-like.",
      "comment": "Accepted for publication in The Astrophysical Journal",
      "journal": null,
      "doi": null
    },
    {
      "version": "v2",
      "updated": "2014-09-11T09:42:17.000Z"
    }
  ],
  "analyses": {
    "keywords": [
      "terrestrial planet formation",
      "super-earths shepherd rocky material interior",
      "migrating super-earths shepherd rocky material"
    ],
    "tags": [
      "journal article"
    ],
    "publication": {
      "doi": "10.1088/0004-637X/794/1/11",
      "journal": "The Astrophysical Journal",
      "year": 2014,
      "month": "Oct",
      "volume": 794,
      "number": 1,
      "pages": 11
    },
    "note": {
      "typesetting": "TeX",
      "pages": 0,
      "language": "en",
      "license": "arXiv",
      "status": "editable",
      "adsabs": "2014ApJ...794...11I"
    }
  }
}