¹Kurihara, Kanoko,^1,2Numa, Norika,¹Niki, Sota,¹Akamune, Mai,¹Nakazato, Masaki,^1,3Yamashita, Shuji,⁴Itoh, Shoichi,¹Hirata, Takafumi
Geochemical Journal 57, E9-E16 Open Access Link to Article [DOI https://doi.org/10.2343/geochemj.GJ23015]
¹Geochemical Research Center, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan
²Section of Public Relations, Math Channel, 2-26-12 Yoyogi, Shibuya-ku, Tokyo, 151-0053, Japan
³National Metrology Institute of Japan (NMIJ), National Institute of Advanced Industrial Science and Technology (AIST), 1-1-1 Umezono, Ibaraki, Tsukuba, 305-8563, Japan
⁴Graduate School of Science, Kyoto Univeristy, Kitashirakawa Oiwakecho, Sakyo-ku, Kyoto, 606-8502, Japan

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^1,2,3Min Li,^2,4Zhaohuan Zhu,⁵Shichun Huang,⁶Ning Sui,⁷Michail I. Petaev,^2,4Jason H. Steffen
The Astrophysical Journal 958, 58 Open Access Link to Article [DOI 10.3847/1538-4357/acfb02]
¹College of Physics, Jilin Normal University, Siping, Jilin 136000, People’s Republic of China
²Department of Physics and Astronomy, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy., Las Vegas, NV 89154, USA
³Key Laboratory of Functional Materials Physics and Chemistry of the Ministry of Education, Jilin Normal University, Changchun, Jilin 130103, People’s Republic of China
⁴Nevada Center for Astrophysics, University of Nevada, Las Vegas, 4505 S. Maryland Pkwy., Las Vegas, NV 89154, USA
⁵Department of Earth and Planetary Sciences, University of Tennessee, Knoxville, 1621 Cumberland Ave., Knoxville, TN 37996, USA
⁶College of Physics, Jilin University, Changchun, Jilin 130012, People’s Republic of China
⁷Department of Earth and Planetary Sciences, Harvard University, 20 Oxford St., Cambridge, MA 02138, USA

The temperatures of observed protoplanetary disks are not sufficiently high to produce the accretion rate needed to form stars, nor are they sufficient to explain the volatile depletion patterns in CM, CO, and CV chondrites and terrestrial planets. We revisit the role that stellar outbursts, caused by high-accretion episodes, play in resolving these two issues. These outbursts provide the necessary mass to form the star during the disk lifetime and provide enough heat to vaporize planet-forming materials. We show that these outbursts can reproduce the observed chondrite abundances at distances near 1 au. These outbursts would also affect the growth of calcium-aluminum-rich inclusions and the isotopic compositions of carbonaceous and noncarbonaceous chondrites.

¹Ihor Kyrylenko,^1,2Oleksiy Golubov,¹Ivan Slyusarev,³Jaakko Visuri,^3,4,5Maria Gritsevich,^1,2Yurij N. Krugly,^1,6Irina Belskaya,¹asilij G. Shevchenko
The Astrophysical Journal 953, 20 Open Access Link to Article [DOI 10.3847/1538-4357/acdc21]
¹Institute of Astronomy of V.N. Karazin Kharkiv National University, 35 Sumska Street, Kharkiv 61022, Ukraine
²Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Poznan, Poland
³Finnish Fireball Network, Ursa Astronomical Association, Kopernikuksentie 1, Helsinki FI-00130, Finland
⁴Finnish Geospatial Research Institute, Vuorimiehentie 5, FI-02150 Espoo, Finland
⁵Department of Physics, University of Helsinki, Gustaf Hällsrömin katu 2a, Helsinki FI-00014, Finland
⁶LESIA, Observatoire de Paris, Université PSL, CNRS, Université Paris Cité, Sorbonne Université, Meudon, France

A bright fireball observed on 2020 November 7, over Scandinavia, produced the first iron meteorite with a well-determined pre-atmospheric trajectory. We calculated the orbit of this meteoroid and found that it demonstrates no close affinity with the orbit of any known asteroid. We found that the meteoroid (or its parent body) most probably entered the near-Earth orbit from the main asteroid belt via either ν₆ secular resonance with Saturn (89%) or 3:1 mean-motion resonance with Jupiter (11%). The long YORP timescale of the meteoroid suggests that it could have been produced in the main asteroid belt and survived the journey to the near-Earth orbit.