2017/09/15 by Matthew J. Holman, Matthew J. Payne, Wesley Fraser +37 · 19 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Brown dwarf #Dwarf planet #Exoplanet #Neptune #Orbit (dynamics) #Planet #Population #Solar System #Stellar, planetary, and galactic studies #astro-ph.EP
paper · pdf · doi:10.3847/2041-8213/aaadb3
published in The Astrophysical Journal Letters 855(1), L6 (IOP Publishing)
arxiv created 2017/09/15 · openalex created_date 2017/09/25 · openalex publication_date 2018/02/28 · arxiv updated 2018/03/14 · openalex updated_date 2026/08/06
Abstract We report the discovery of an H r = 3.4 ± 0.1 dwarf planet candidate by the Pan-STARRS Outer Solar System Survey. 2010 JO 179 is red with ( g − r ) = 0.88 ± 0.21, roughly round, and slowly rotating, with a period of 30.6 hr. Estimates of its albedo imply a diameter of 600–900 km. Observations sampling the span between 2005 and 2016 provide an exceptionally well determined orbit for 2010 JO 179 , with a semimajor axis of 78.307 ± 0.009 au; distant orbits known to this precision are rare. We find that 2010 JO 179 librates securely within the 21:5 mean-motion resonance with Neptune on 100 Myr timescales, joining the small but growing set of known distant dwarf planets on metastable resonant orbits. These imply a substantial trans-Neptunian population that shifts between stability in high-order resonances, the detached population, and the eroding population of the scattering disk.