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.

¹Peter Hoppe,^1,2Jan Leitner,^3,4,5Marco Pignatari,^6,7Sachiko Amari
The Astrophysical Journal Letters 943, L22 Open Access Link to Article [DOI 10.3847/2041-8213/acb157]
¹Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, D-55128 Mainz, Germany; peter.hoppe@mpic.de
²Institute of Earth Sciences, Heidelberg University, Im Neuenheimer Feld 234-236, D-69120 Heidelberg, Germany
³Konkoly Observatory, Konkoly Thege Miklos ut 15-17, 1121, Budapest, Hungary
⁴E. A. Milne Centre for Astrophysics, University of Hull, HU6 7RX, Hull, UK
⁵NuGrid Collaboration, USA 8
⁶McDonnell Center for the Space Sciences and Physics Department, Washington University, St. Louis, MO 63130, USA
⁷Geochemical Research Center, The University of Tokyo, Tokyo, 113-0033, Japan

We report C, N, Mg-Al, Si, and S isotope data of six 1–3 μm-sized SiC grains of Type X from the Murchison CM2 chondrite, believed to have formed in the ejecta of core-collapse supernova (CCSN) explosions. Their C, N, and Si isotopic compositions are fully compatible with previously studied X grains. Magnesium is essentially monoisotopic ²⁶Mg which gives clear evidence for the decay of radioactive ²⁶Al. Inferred initial ²⁶Al/²⁷Al ratios are between 0.6 and 0.78 which is at the upper end of previously observed ratios of X grains. Contamination with terrestrial or solar system Al apparently is low or absent, which makes the X grains from this study particularly interesting and useful for a quantitative comparison of Al isotope data with predictions from supernova models. The consistently high ²⁶Al/²⁷Al ratios observed here may suggest that the lower ²⁶Al/²⁷Al ratios of many X grains from the literature are the result of significant Al contamination and in part also of an improper quantification of ²⁶Al. The real dispersion of ²⁶Al/²⁷Al ratios in X grains needs to be explored by future studies. The high observed ²⁶Al/²⁷Al ratios in this work provide a crucial constraint for the production of ²⁶Al in CCSN models. We explored different CCSN models, including both “classical” and H ingestion CCSN models. It is found that the classical models cannot account for the high ²⁶Al/²⁷Al ratios observed here; in contrast, H ingestion models are able to reproduce the ²⁶Al/²⁷Al ratios along with C, N, and Si isotopic ratios reasonably well.

¹Yuki Hibiya,²Tsuyoshi Iizuka,²Hatsuki Enomoto,³Takehito Hayakawa
The Astrophysical Journal Letters 942, L15 Open Access Link to Article [DOI 10.3847/2041-8213/acab5d]
¹Research Center for Advanced Science and Technology, The University of Tokyo, 4-6-1 Komaba, Meguro-ku, Tokyo 153-8904
²Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
¹National Institutes for Quantum Science and Technology, 2-4 Shirakata, Tokai, Naka, Ibaraki 319-1106, Japan

The short-lived radionuclide, niobium-92 (⁹²Nb), has been used to estimate the site of nucleosynthesis for p-nuclei and the timing of planetary differentiation, assuming that it was uniformly distributed in the early solar system. Here, we present the internal niobium–zirconium (Nb–Zr) isochron dating of Northwest Africa (NWA) 6704, an achondrite thought to form in the outer protosolar disk due to nucleosynthetic isotope similarities with carbonaceous chondrites. The isochron defines an initial ⁹²Nb/⁹³Nb ratio of (2.72 ± 0.25) × 10⁻⁵ at the NWA 6704 formation, 4562.76 ± 0.30 million years ago. This corresponds to a ⁹²Nb/⁹³Nb ratio of (2.96 ± 0.27) × 10⁻⁵ at the time of solar system formation, which is ∼80% higher than the values obtained from meteorites formed in the inner disk. The results suggest that a significant proportion of the solar ⁹²Nb was produced by a nearby core-collapse supernova (CCSN) and that the outer disk was more enriched in CCSN ejecta, which could account for the heterogeneity of short-lived ²⁶Al and nucleosynthetic stable-isotope anomalies across the disk. We propose that NWA 6704 serves as the best anchor for mapping relative Nb–Zr ages of objects in the outer solar system onto the absolute timescale.