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Sökning: id:"swepub:oai:DiVA.org:ltu-99300" > NEOMOD: A New Orbit...

LIBRIS Formathandbok  (Information om MARC21)
FältnamnIndikatorerMetadata
00006024naa a2200517 4500
001oai:DiVA.org:ltu-99300
003SwePub
008230808s2023 | |||||||||||000 ||eng|
0247 a https://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-993002 URI
0247 a https://doi.org/10.3847/1538-3881/ace0402 DOI
040 a (SwePub)ltu
041 a engb eng
042 9 SwePub
072 7a ref2 swepub-contenttype
072 7a art2 swepub-publicationtype
1001 a Nesvorný, Davidu Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA4 aut
2451 0a NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
264 1b Institute of Physics (IOP),c 2023
338 a electronic2 rdacarrier
500 a Validerad;2023;Nivå 2;2023-08-08 (hanlid);Funder: Czech Science Foundation (21-11058S); NASA Planetary Defense Coordination Office
520 a 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.
650 7a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe
650 7a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng
650 7a TEKNIK OCH TEKNOLOGIERx Elektroteknik och elektronikx Annan elektroteknik och elektronik0 (SwePub)202992 hsv//swe
650 7a ENGINEERING AND TECHNOLOGYx Electrical Engineering, Electronic Engineering, Information Engineeringx Other Electrical Engineering, Electronic Engineering, Information Engineering0 (SwePub)202992 hsv//eng
653 a Onboard Space Systems
653 a Rymdtekniska system
7001 a Deienno, Rogeriou Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA4 aut
7001 a Bottke, William F.u Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USA4 aut
7001 a Jedicke, Robertu Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA4 aut
7001 a Naidu, Shantanuu Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA4 aut
7001 a Chesley, Steven R.u Department of Earth and Space Sciences, University of California, 595 Charles Young Drive East, 5656 Geology Building, Los Angeles, CA 90095, USA4 aut
7001 a Chodas, Paul W.u Department of Earth and Space Sciences, University of California, 595 Charles Young Drive East, 5656 Geology Building, Los Angeles, CA 90095, USA4 aut
7001 a Granvik, Mikaelu Luleå tekniska universitet,Rymdteknik,Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Finland4 aut0 (Swepub:ltu)mikgra
7001 a Vokrouhlický, Davidu Institute of Astronomy, Charles University, V Holešovičkách 2, CZ18000 Prague 8, Czech Republic4 aut
7001 a Brož, Miroslavu Institute of Astronomy, Charles University, V Holešovičkách 2, CZ18000 Prague 8, Czech Republic4 aut
7001 a Morbidelli, Alessandrou Laboratoire Lagrange, UMR7293, Université Côte d’Azur, CNRS, Observatoire de la Côte d’Azur, Bouldervard de l’Observatoire, F-06304, Nice Cedex 4, France4 aut
7001 a Christensen, Ericu Lunar and Planetary Laboratory, The University of Arizona, 1629 E. University Boulevard, Tucson, AZ 85721-0092, USA4 aut
7001 a Shelly, Frank C.u Lunar and Planetary Laboratory, The University of Arizona, 1629 E. University Boulevard, Tucson, AZ 85721-0092, USA4 aut
7001 a Bolin, Bryce T.u 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, USA4 aut
7102 a Department of Space Studies, Southwest Research Institute, 1050 Walnut Street, Suite 300, Boulder, CO 80302, USAb Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822-1839, USA4 org
7730 t Astronomical Journald : Institute of Physics (IOP)g 166:2q 166:2x 0004-6256x 1538-3881
8564 u https://doi.org/10.3847/1538-3881/ace040y Fulltext
8564 u https://ltu.diva-portal.org/smash/get/diva2:1786338/FULLTEXT01.pdfx primaryx Raw objecty fulltext:print
8564 8u https://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-99300
8564 8u https://doi.org/10.3847/1538-3881/ace040

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