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  • Nesvorný, DavidDepartment of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA (author)

NEOMOD: A New Orbital Distribution Model for Near-Earth Objects

  • Article/chapterEnglish2023

Publisher, publication year, extent ...

  • Institute of Physics (IOP),2023
  • electronicrdacarrier

Numbers

  • LIBRIS-ID:oai:DiVA.org:ltu-99300
  • https://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-99300URI
  • https://doi.org/10.3847/1538-3881/ace040DOI

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  • Language:English
  • Summary in:English

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  • Subject category:ref swepub-contenttype
  • Subject category:art swepub-publicationtype

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  • Validerad;2023;Nivå 2;2023-08-08 (hanlid);Funder: Czech Science Foundation (21-11058S); NASA Planetary Defense Coordination Office
  • Near-Earth Objects (NEOs) are a transient population of small bodies with orbits near or in the terrestrial planet region. They represent a mid-stage in the dynamical cycle of asteroids and comets, which starts with their removal from the respective source regions—the main belt and trans-Neptunian scattered disk—and ends as bodies impact planets, disintegrate near the Sun, or are ejected from the solar system. Here we develop a new orbital model of NEOs by numerically integrating asteroid orbits from main-belt sources and calibrating the results on observations of the Catalina Sky Survey. The results imply a size-dependent sampling of the main belt with the ν 6 and 3:1 resonances producing ≃30% of NEOs with absolute magnitudes H = 15 and ≃80% of NEOs with H = 25. Hence, the large and small NEOs have different orbital distributions. The inferred flux of H < 18 bodies into the 3:1 resonance can be sustained only if the main-belt asteroids near the resonance drift toward the resonance at the maximal Yarkovsky rate (≃2 × 10−4 au Myr−1 for diameter D = 1 km and semimajor axis a = 2.5 au). This implies obliquities θ ≃ 0° for a < 2.5 au and θ ≃ 180° for a > 2.5 au, both in the immediate neighborhood of the resonance (the same applies to other resonances as well). We confirm the size-dependent disruption of asteroids near the Sun found in previous studies. An interested researcher can use the publicly available NEOMOD Simulator to generate user-defined samples of NEOs from our model.

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  • Deienno, RogerioDepartment of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA (author)
  • Bottke, William F.Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA (author)
  • Jedicke, RobertInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA (author)
  • Naidu, ShantanuJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA (author)
  • Chesley, Steven R.Department of Earth and Space Sciences, University of California, 595 Charles Young Drive East, 5656 Geology Building, Los Angeles, CA 90095, USA (author)
  • Chodas, Paul W.Department of Earth and Space Sciences, University of California, 595 Charles Young Drive East, 5656 Geology Building, Los Angeles, CA 90095, USA (author)
  • Granvik, MikaelLuleå tekniska universitet,Rymdteknik,Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Finland(Swepub:ltu)mikgra (author)
  • Vokrouhlický, DavidInstitute of Astronomy, Charles University, V Holešovičkách 2, CZ18000 Prague 8, Czech Republic (author)
  • Brož, MiroslavInstitute of Astronomy, Charles University, V Holešovičkách 2, CZ18000 Prague 8, Czech Republic (author)
  • Morbidelli, AlessandroLaboratoire Lagrange, UMR7293, Université Côte d’Azur, CNRS, Observatoire de la Côte d’Azur, Bouldervard de l’Observatoire, F-06304, Nice Cedex 4, France (author)
  • Christensen, EricLunar and Planetary Laboratory, The University of Arizona, 1629 E. University Boulevard, Tucson, AZ 85721-0092, USA (author)
  • Shelly, Frank C.Lunar and Planetary Laboratory, The University of Arizona, 1629 E. University Boulevard, Tucson, AZ 85721-0092, USA (author)
  • Bolin, Bryce T.Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USA; Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA; NASA Postdoctoral Program Fellow, Goddard Space Flight Center, 8800 Greenbelt Road, Greenbelt, MD 20771, USA (author)
  • Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USAInstitute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA (creator_code:org_t)

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  • In:Astronomical Journal: Institute of Physics (IOP)166:20004-62561538-3881

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