During the last days of this year, Cosmochemistry Papers will be on Christmas break. Normal service will commence on January, 2nd, 2024 .

Merry Christmas & Happy New Year to everyone!

¹Takaharu Saito,¹Hiroshi Hidaka,²Shigekazu Yoneda
The Astrophysical Journal 955, 85 Open Access Link to Article [DOI 10.3847/1538-4357/acf37b]
¹Department of Earth and Planetary Sciences, Nagoya University, Nagoya 464-8601, Japan; ²Department of Science and Engineering, National Museum of Nature and Science, Tsukuba 305-0005, Japan

The isotopic compositions of Sm and Gd in eight eucrites—five from a desert, Dar al Gani (DaG) 380, DaG 391, DaG 411, DaG 443, and DaG 480, and three from nondesert areas, Juvinas, Millibillillie, and Stannern—were determined to understand the cosmic-ray exposure (CRE) history for each meteorite from the isotopic shifts of 149Sm–150Sm and 157Gd–158Gd caused by the neutron capture reactions induced by cosmic-ray irradiation. Seven of the eight samples, excepting DaG 443, show readily detectable isotopic shifts of Sm and Gd corresponding to neutron fluences in the range of (0.28–2.38) × 1015 neutrons cm−2. The degrees of Sm isotopic shifts for six of these seven eucrites can be consistently explained by the CRE age histogram of eucrites obtained in previous studies. Exceptionally, DaG 480 shows larger isotopic shifts of Sm than those expected from the CRE age histogram, suggesting a multiple-irradiation history, including irradiation on the parent body. However, there is no clear difference in the CRE conditions between DaG 480 and other eucrites from the parameter εSm/εGd to identify the difference in the thermalization degree of neutrons in association with the CRE conditions.

¹Kurt Marti,²Mario Fischer-Gödde,³Carina Proksche
The Astrophysical Journal 956, 7 Open Access Link to Article [DOI 10.3847/1538-4357/acee81]
¹Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093-0314, USA
²Universität zu Köln, Institut für Geologie und Mineralogie, Zülpicher Str. 49b, D-50674 Köln, Germany; mfisch48@uni-koeln.de
³Geo Zentrum Nordbayern, Friedrich-Alexander-Universität Erlangen-Nürnberg, Schlossgarten 5, D-91054 Erlangen, Germany

Anomalies in isotopic abundances of Mo and Ru in solar system matter were found to document variable contributions of the nucleosynthetic s-process component. We report isotopic relations of ⁹²Mo versus ¹⁰⁰Ru in meteorites from chondritic parent bodies, iron meteorites, and achondrites that reveal deviations from expected s-process abundance variations. We show that two p-process isotopes ⁹²Mo and ⁹⁴Mo require the presence of distinct p-process components in meteoritic materials. The nucleosynthetic origin of abundant magic (N = 50) p-process nuclides, covering the mass range of Zr, Mo, and Ru, has long been an enigma, but contributions by several recognized pathways, including alpha and νp-antineutrino reactions on protons, may account for the observed relatively large solar system abundances. Specific core-collapse supernovae explosive regions may carry proton-rich matter. Since Mo and Ru isotopic records in solar system matter reveal the presence of more than one nucleosynthetic p-process component, these records are expected to be helpful in documenting different explosive synthesis pathways and the implied galactic evolution of p-nuclides.

^1,4Oshtrakh, Michael I.,^1,2Maksimova, Alevtina A.,¹Petrova, Evgeniya V.,¹Chukin, Andrey V.,³Felner, Israel
Hyperfine Interactions 244, 22 Link to Article [DOI 10.1007/s10751-023-01830-9]
¹Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation
²Department of Chemistry and Biochemistry, University of South Carolina, Columbia, 29208, SC, United States
³Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, Israel
⁴Department of Experimental Physics, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation

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¹Unsalan, Ozan,²Yilmaz, Berguzar,³Reva, Igor
ACS Earth and Space Chemistry 7, 1992 – 2005 Link to Article [DOI 10.1021/acsearthspacechem.3c00108]
¹Faculty of Science, Department of Physics, Ege University, Izmir, Bornova, 35100, Turkey
²Natural and Applied Sciences, Department of Biotechnology, Ege University, Izmir, Bornova, 35100, Turkey
³CIEPQPF, Department of Chemical Engineering, University of Coimbra, Rua Sílvio Lima, Coimbra, 3030-790, Portugal

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¹Jonatan Michimani,¹Eduardo Rondón,²Davide Perna,²Simone Ieva,²Elisabetta Dotto,²Elena Mazzotta Epifani,^3,4Antonella Barucci,²Vasiliki Petropoulou,²Daniela Lazzaro
Monthly Notices of the Royal Astronomical Society 526, 2067–2076 Link to Article [https://doi.org/10.1093/mnras/stad2883]
¹Observatório Nacional, Rua Gal. José Cristino 77, 20921-400 Rio de Janeiro, Brazil
²INAF – Osservatorio Astronomico di Roma, Via Frascati 33, I-00078, Monte Porzio Catone, Italy
³LESIA, Observatoire de Paris, PSL Research University, CNRS,
⁴Univ. Paris Diderot, Sorbonne Paris Cité, UPMC Univ., Paris 06, Sorbonne Universités, 5 Place J. Janssen, F-92195 Meudon Pricipal Cedex, France

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¹A Carbognani,^2,3M Fenucci
Monthly Notices of the Royal Astronomical Society 525, 1705–1725 Link to Article [https://doi.org/10.1093/mnras/stad2382]
¹INAF – Osservatorio di Astrofisica e Scienza dello Spazio, Via Gobetti 93/3, I-40129 Bologna, Italy
²ESA ESRIN/PDO/NEO Coordination Centre, Largo Galileo Galilei, 1, I-00044 Frascati (RM), Italy
³Elecnor Deimos, Via Giuseppe Verdi, 6, I-28060 San Pietro Mosezzo (NO), Italy

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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.