FORMATION OF SUPER-EARTH MASS PLANETS AT 125–250 AU FROM A SOLAR-TYPE STAR

2015/01/31 by Scott J. Kenyon, S. J. Kenyon, Benjamin C. Bromley +1
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Formation and evolution of the Solar System #Planet #Planetary mass #Planetary system #Protoplanet #Solar System #Stellar, planetary, and galactic studies #Terrestrial planet #astro-ph.EP #astro-ph.SR

paper · pdf · doi:10.1088/0004-637x/806/1/42

48 pages of text, 23 figures, ApJ in press, revised version contains new text on aspects of the calculations and a more comprehensive description of the origin of the second phase of runaway growth

arxiv created 2015/04/21 · openalex publication_date 2015/06/05 · arxiv updated 2015/06/11 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

We investigate pathways for the formation of icy super-Earth mass planets orbiting at 125–250 AU around a 1 star. An extensive suite of coagulation calculations demonstrates that swarms of 1 cm–10 m planetesimals can form super-Earth mass planets on timescales of 1–3 Gyr. Collisional damping of 10 −2 −10 2 cm particles during oligarchic growth is a highlight of these simulations. In some situations, damping initiates a second runaway growth phase where 1000–3000 km protoplanets grow to super-Earth sizes. Our results establish the initial conditions and physical processes required for in situ formation of super-Earth planets at large distances from the host star. For nearby dusty disks in HD 107146, HD 202628, and HD 207129, ongoing super-Earth formation at 80–150 AU could produce gaps and other structures in the debris. In the solar system, forming a putative planet X at AU ( AU) requires a modest (very massive) protosolar nebula.

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