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Krestianinov E, Amelin Y, Yin QZ, Cary P, Huyskens MH, Miller A, Dey S, Hibiya Y, Tang H, Young ED, Pack A, Di Rocco T. Igneous meteorites suggest Aluminium-26 heterogeneity in the early Solar Nebula. Nat Commun 2023; 14:4940. [PMID: 37643999 PMCID: PMC10465487 DOI: 10.1038/s41467-023-40026-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/26/2022] [Accepted: 07/04/2023] [Indexed: 08/31/2023] Open
Abstract
The short-lived radionuclide aluminium-26 (26Al) isotope is a major heat source for early planetary melting. The aluminium-26 - magnesium-26 (26Al-26Mg) decay system also serves as a high-resolution relative chronometer. In both cases, however, it is critical to establish whether 26Al was homogeneously or heterogeneously distributed throughout the solar nebula. Here we report a precise lead-207 - lead-206 (207Pb-206Pb) isotopic age of 4565.56 ± 0.12 million years (Ma) for the andesitic achondrite Erg Chech 002. Our analysis, in conjunction with published 26Al-26Mg data, reveals that the initial 26Al/27Al in the source material of this achondrite was notably higher than in various other well-preserved and precisely dated achondrites. Here we demonstrate that the current data clearly indicate spatial heterogeneity of 26Al by a factor of 3-4 in the precursor molecular cloud or the protoplanetary disk of the Solar System, likely associated with the late infall of stellar materials with freshly synthesized radionuclides.
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Affiliation(s)
- Evgenii Krestianinov
- Research School of Earth Sciences, Australian National University, Canberra, 2601, Australia.
| | - Yuri Amelin
- Research School of Earth Sciences, Australian National University, Canberra, 2601, Australia
- Guangzhou Institute of Geochemistry, Chinese Academy of Sciences, Guangzhou, GD, 510640, China
- Korea Basic Science Institute, Ochang, Cheongwon, Cheongju, Chungbuk, 28119, Korea
| | - Qing-Zhu Yin
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Paige Cary
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Magdalena H Huyskens
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Audrey Miller
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Supratim Dey
- Department of Earth and Planetary Sciences, University of California, Davis, Davis, CA, 95616, USA
| | - Yuki Hibiya
- Department of General Systems Studies, University of Tokyo, Komaba 3-8-1, Meguro, Tokyo, 153-0041, Japan
- Research Center for Advanced Science and Technology, University of Tokyo, Komaba 4-6-1, Meguro, Tokyo, 153-8904, Japan
| | - Haolan Tang
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, CA, 90095, USA
| | - Edward D Young
- Department of Earth, Planetary and Space Sciences, University of California, Los Angeles, Los Angeles, CA, 90095, USA
| | - Andreas Pack
- Geochemistry and Isotope Geology Department, Georg-August-Universität Göttingen, Goldschmidtstraße 1, 37077, Göttingen, Germany
| | - Tommaso Di Rocco
- Geochemistry and Isotope Geology Department, Georg-August-Universität Göttingen, Goldschmidtstraße 1, 37077, Göttingen, Germany
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2
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Chiera NM, Dressler R, Sprung P, Talip Z, Schumann D. High precision half-life measurement of the extinct radio-lanthanide Dysprosium-154. Sci Rep 2022; 12:8988. [PMID: 35643721 PMCID: PMC9148308 DOI: 10.1038/s41598-022-12684-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/17/2021] [Accepted: 05/13/2022] [Indexed: 11/11/2022] Open
Abstract
Sixty years after the discovery of 154Dy, the half-life of this pure alpha-emitter was re-measured. 154Dy was radiochemically separated from proton-irradiated tantalum samples. Sector field- and multicollector-inductively coupled plasma mass spectrometry were used to determine the amount of 154Dy retrieved. The disintegration rate of the radio-lanthanide was measured by means of α-spectrometry. The half-life value was determined as (1.40 ± 0.08)∙106 y, with an uncertainty reduced by a factor of ~ 10 compared to the currently adopted value of (3.0 ± 1.5)∙106 y. This precise half-life value is useful for the the correct testing and evaluation of p-process nucleosynthetic models using 154Dy as a seed nucleus or as a reaction product, as well as for the safe disposal of irradiated target material from accelerator driven facilities. As a first application of the half-life value determined in this work, the excitation functions for the production of 154Dy in proton-irradiated Ta, Pb, and W targets were re-evaluated, which are now in agreement with theoretical calculations.
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Lotay G, Lennarz A, Ruiz C, Akers C, Chen AA, Christian G, Connolly D, Davids B, Davinson T, Fallis J, Hutcheon DA, Machule P, Martin L, Mountford DJ, Murphy ASJ. Radiative Capture on Nuclear Isomers: Direct Measurement of the ^{26m}Al(p,γ)^{27}Si Reaction. PHYSICAL REVIEW LETTERS 2022; 128:042701. [PMID: 35148128 DOI: 10.1103/physrevlett.128.042701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/07/2021] [Revised: 12/10/2021] [Accepted: 12/24/2021] [Indexed: 06/14/2023]
Abstract
We present the first direct measurement of an astrophysical reaction using a radioactive beam of isomeric nuclei. In particular, we have measured the strength of the key 447-keV resonance in the ^{26m}Al(p,γ)^{27}Si reaction to be 432_{-226}^{+146} meV and find that this resonance dominates the thermally averaged reaction rate for temperatures between 0.3 and 2.5 GK. This work represents a critical development in resolving one of the longest standing issues in nuclear astrophysics research, relating to the measurement of proton capture reactions on excited quantum levels, and offers unique insight into the destruction of isomeric ^{26}Al in astrophysical plasmas.
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Affiliation(s)
- G Lotay
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - A Lennarz
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - C Ruiz
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics and Astronomy, University of Victoria, Victoria, BC V8W 2Y2, Canada
| | - C Akers
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, University of York, Heslington, York YO10 5DD, United Kingdom
| | - A A Chen
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - G Christian
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - D Connolly
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - B Davids
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
- Department of Physics, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada
| | - T Davinson
- School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom
| | - J Fallis
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - D A Hutcheon
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - P Machule
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - L Martin
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - D J Mountford
- School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom
| | - A St J Murphy
- School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom
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4
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Hallam S, Lotay G, Gade A, Doherty DT, Belarge J, Bender PC, Brown BA, Browne J, Catford WN, Elman B, Estradé A, Hall MR, Longfellow B, Lunderberg E, Montes F, Moukaddam M, O'Malley P, Ong WJ, Schatz H, Seweryniak D, Schmidt K, Timofeyuk NK, Weisshaar D, Zegers RGT. Exploiting Isospin Symmetry to Study the Role of Isomers in Stellar Environments. PHYSICAL REVIEW LETTERS 2021; 126:042701. [PMID: 33576674 DOI: 10.1103/physrevlett.126.042701] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/23/2020] [Revised: 11/23/2020] [Accepted: 01/12/2021] [Indexed: 06/12/2023]
Abstract
Proton capture on the excited isomeric state of ^{26}Al strongly influences the abundance of ^{26}Mg ejected in explosive astronomical events and, as such, plays a critical role in determining the initial content of radiogenic ^{26}Al in presolar grains. This reaction also affects the temperature range for thermal equilibrium between the ground and isomeric levels. We present a novel technique, which exploits the isospin symmetry of the nuclear force, to address the long-standing challenge of determining proton-capture rates on excited nuclear levels. Such a technique has in-built tests that strongly support its veracity and, for the first time, we have experimentally constrained the strengths of resonances that dominate the astrophysical ^{26m}Al(p,γ)^{27}Si reaction. These constraints demonstrate that the rate is at least a factor ∼8 lower than previously expected, indicating an increase in the stellar production of ^{26}Mg and a possible need to reinvestigate sensitivity studies involving the thermal equilibration of ^{26}Al.
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Affiliation(s)
- S Hallam
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - G Lotay
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - A Gade
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - D T Doherty
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - J Belarge
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - P C Bender
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - B A Brown
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - J Browne
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - W N Catford
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - B Elman
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
| | - A Estradé
- Department of Physics, Central Michigan University, Mount Pleasant, Michigan 48859, USA
| | - M R Hall
- Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - B Longfellow
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
| | - E Lunderberg
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
| | - F Montes
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - M Moukaddam
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - P O'Malley
- Department of Physics, University of Notre Dame, Notre Dame, Indiana 46556, USA
| | - W-J Ong
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
| | - H Schatz
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - D Seweryniak
- Physics Division, Argonne National Laboratory, Argonne, Illinois 60439, USA
| | - K Schmidt
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
| | - N K Timofeyuk
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
| | - D Weisshaar
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - R G T Zegers
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA
- Joint Institute for Nuclear Astrophysics, Center for the Evolution of the Elements, Michigan State University, East Lansing, Michigan 48824, USA
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5
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Zucolotto ME, Tosi AA, Villaça CVN, Moutinho ALR, Andrade DPP, Faulstich F, Gomes AMS, Rios DC, Rocha MC. Serra Pelada: the first Amazonian Meteorite fall is a Eucrite (basalt) from Asteroid 4-Vesta. AN ACAD BRAS CIENC 2018; 90:3-16. [PMID: 29424394 DOI: 10.1590/0001-3765201820170854] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 10/02/2017] [Accepted: 12/11/2017] [Indexed: 11/22/2022] Open
Abstract
Serra Pelada is the newest Brazilian eucrite and the first recovered fall from Amazonia (State of Pará, Brazil, June 29th 2017). In this paper, we report on its petrography, chemistry, mineralogy and its magnetic properties. Study of four thin sections reveals that the meteorite is brecciated, containing basaltic and gabbroic clasts, as well of recrystallized impact melt, embedded into a fine-medium grained matrix. Chemical analyses suggest that Serra Pelada is a monomict basaltic eucritic breccia, and that the meteorite is a normal member of the HED suite. Our results provide additional geological and compositional information on the lithological diversity of its parent body. The mineralogy of Serra Pelada consists basically of low-Ca pyroxene and high-Ca plagioclase with accessory minerals such as quartz, sulphide (troilite), chromite - ulvöspinel and ilmenite. These data are consistent with the meteorite being an eucrite, a basaltic achondrite and a member of the howardite-eucrite-diogenite (HED) clan of meteorites which most likely are from the crust asteroid 4 Vesta.
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Affiliation(s)
- Maria Elizabeth Zucolotto
- LABET/MN/UFRJ, Laboratório Extraterrestre, Departamento de Geologia e Paleontologia, Museu Nacional, Universidade Federal do Rio de Janeiro, Quinta da Boa Vista, São Cristóvão, 20940-040 Rio de Janeiro, RJ, Brazil
| | - Amanda A Tosi
- LABSONDA/IGEO/UFRJ, Instituto de Geociências, Universidade Federal do Rio de Janeiro, Av. Athos da Silveira Ramos, 274, Cidade Universitária, 21941-972 Rio de Janeiro, RJ, Brazil
| | - Caio V N Villaça
- LABSONDA/IGEO/UFRJ, Instituto de Geociências, Universidade Federal do Rio de Janeiro, Av. Athos da Silveira Ramos, 274, Cidade Universitária, 21941-972 Rio de Janeiro, RJ, Brazil
| | - André L R Moutinho
- Colecionador da International Meteorite Colector Association (IMCA #2731), R. Roberto dos Santos, 163, 12300-000 Jacareí, SP, Brazil
| | - Diana P P Andrade
- OV/UFRJ, Observatório do Valongo, Universidade Federal do Rio de Janeiro, Ladeira Pedro Antônio, 43, Saúde, 20080-090 Rio de Janeiro, RJ, Brazil
| | - Fabiano Faulstich
- LABET/MN/UFRJ, Laboratório Extraterrestre, Departamento de Geologia e Paleontologia, Museu Nacional, Universidade Federal do Rio de Janeiro, Quinta da Boa Vista, São Cristóvão, 20940-040 Rio de Janeiro, RJ, Brazil
| | - Angelo M S Gomes
- IF/UFRJ, Instituto de Física, Universidade Federal do Rio de Janeiro, Av. Athos da Silveira Ramos,149, CT, Bloco A, Cidade Universitária, 21941-972 Rio de Janeiro, RJ, Brazil
| | - Debora C Rios
- GPA, Universidade Federal da Bahia/UFBA, Instituto de Geociências, R. Barão de Geremoabo s/n, Ondina, 40170-290 Salvador, BA, Brazil
| | - Marcilio C Rocha
- Universidade Federal do Pará/UFPA, Departamento de Geociências e Engenharias, Rua Augusto Correa, nº 01, Campus Universitário do Guamá, 66075-110, Belém, PA, Brazil
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6
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Kayanuma M, Kidachi K, Shoji M, Komatsu Y, Sato A, Shigeta Y, Aikawa Y, Umemura M. A theoretical study of the formation of glycine via hydantoin intermediate in outer space environment. Chem Phys Lett 2017. [DOI: 10.1016/j.cplett.2017.09.016] [Citation(s) in RCA: 10] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/18/2022]
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7
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Margerin V, Lotay G, Woods PJ, Aliotta M, Christian G, Davids B, Davinson T, Doherty DT, Fallis J, Howell D, Kirsebom OS, Mountford DJ, Rojas A, Ruiz C, Tostevin JA. Inverse Kinematic Study of the (26g)Al(d,p)(27)Al Reaction and Implications for Destruction of (26)Al in Wolf-Rayet and Asymptotic Giant Branch Stars. PHYSICAL REVIEW LETTERS 2015; 115:062701. [PMID: 26296114 DOI: 10.1103/physrevlett.115.062701] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/27/2015] [Indexed: 06/04/2023]
Abstract
In Wolf-Rayet and asymptotic giant branch (AGB) stars, the (26g)Al(p,γ)(27)Si reaction is expected to govern the destruction of the cosmic γ-ray emitting nucleus (26)Al. The rate of this reaction, however, is highly uncertain due to the unknown properties of key resonances in the temperature regime of hydrogen burning. We present a high-resolution inverse kinematic study of the (26g)Al(d,p)(27)Al reaction as a method for constraining the strengths of key astrophysical resonances in the (26g)Al(p,γ)(27)Si reaction. In particular, the results indicate that the resonance at E(r)=127 keV in (27)Si determines the entire (26g)Al(p,γ)(27)Si reaction rate over almost the complete temperature range of Wolf-Rayet stars and AGB stars.
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Affiliation(s)
- V Margerin
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - G Lotay
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
- National Physical Laboratory, Teddington, Middlesex TW11 0LW, United Kingdom
| | - P J Woods
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - M Aliotta
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - G Christian
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - B Davids
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - T Davinson
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - D T Doherty
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - J Fallis
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - D Howell
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - O S Kirsebom
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - D J Mountford
- School of Physics and Astronomy, University of Edinburgh, Edinburgh, EH9 3FD, United Kingdom
| | - A Rojas
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - C Ruiz
- TRIUMF, Vancouver, British Columbia V6T 2A3, Canada
| | - J A Tostevin
- Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom
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8
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Bennett MB, Wrede C, Chipps KA, José J, Liddick SN, Santia M, Bowe A, Chen AA, Cooper N, Irvine D, McNeice E, Montes F, Naqvi F, Ortez R, Pain SD, Pereira J, Prokop C, Quaglia J, Quinn SJ, Schwartz SB, Shanab S, Simon A, Spyrou A, Thiagalingam E. Classical-NOVA CONTRIBUTION to the Milky Way's ²⁶Al abundance: exit channel of the key ²⁵Al(p,γ) ²⁶Si resonance. PHYSICAL REVIEW LETTERS 2013; 111:232503. [PMID: 24476263 DOI: 10.1103/physrevlett.111.232503] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/20/2013] [Revised: 10/07/2013] [Indexed: 06/03/2023]
Abstract
Classical novae are expected to contribute to the 1809-keV Galactic γ-ray emission by producing its precursor 26Al, but the yield depends on the thermonuclear rate of the unmeasured 25Al(p,γ)26Si reaction. Using the β decay of 26P to populate the key J(π)=3(+) resonance in this reaction, we report the first evidence for the observation of its exit channel via a 1741.6±0.6(stat)±0.3(syst) keV primary γ ray, where the uncertainties are statistical and systematic, respectively. By combining the measured γ-ray energy and intensity with other experimental data on 26Si, we find the center-of-mass energy and strength of the resonance to be E(r)=414.9±0.6(stat)±0.3(syst)±0.6(lit.) keV and ωγ=23±6(stat)(-10)(+11)(lit.) meV, respectively, where the last uncertainties are from adopted literature data. We use hydrodynamic nova simulations to model 26Al production showing that these measurements effectively eliminate the dominant experimental nuclear-physics uncertainty and we estimate that novae may contribute up to 30% of the Galactic 26Al.
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Affiliation(s)
- M B Bennett
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - C Wrede
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Department of Physics, University of Washington, Seattle, Washington 98195, USA
| | - K A Chipps
- Department of Physics, Colorado School of Mines, Golden, Colorado 08401, USA
| | - J José
- Departament Física i Enginyeria Nuclear (UPC) and Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain
| | - S N Liddick
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - M Santia
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - A Bowe
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Physics Department, Kalamazoo College, Kalamazoo, Michigan 49006, USA
| | - A A Chen
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - N Cooper
- Department of Physics and Wright Nuclear Structure Laboratory, Yale University, New Haven, Connecticut 06520, USA
| | - D Irvine
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - E McNeice
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
| | - F Montes
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - F Naqvi
- Department of Physics and Wright Nuclear Structure Laboratory, Yale University, New Haven, Connecticut 06520, USA
| | - R Ortez
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Department of Physics, University of Washington, Seattle, Washington 98195, USA
| | - S D Pain
- Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA
| | - J Pereira
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - C Prokop
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Department of Chemistry, Michigan State University, East Lansing, Michigan 48824, USA
| | - J Quaglia
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA and Department of Electrical Engineering, Michigan State University, East Lansing, Michigan 48824, USA
| | - S J Quinn
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - S B Schwartz
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Geology and Physics Department, University of Southern Indiana, Evansville, Indiana 47712, USA
| | - S Shanab
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - A Simon
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - A Spyrou
- Department of Physics and Astronomy, Michigan State University, East Lansing, Michigan 48824, USA and National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA and Joint Institute for Nuclear Astrophysics, Michigan State University, East Lansing, Michigan 48824, USA
| | - E Thiagalingam
- Department of Physics and Astronomy, McMaster University, Hamilton, Ontario L8S 4M1, Canada
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9
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Abstract
The progression from astronomical observation to geochemical analysis epitomizes advancements in planetary exploration.
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Affiliation(s)
- Richard P Binzel
- Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA 02139, USA.
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Morris MA, Desch SJ. Phyllosilicate emission from protoplanetary disks: is the indirect detection of extrasolar water possible? ASTROBIOLOGY 2009; 9:965-978. [PMID: 20041749 DOI: 10.1089/ast.2008.0316] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/28/2023]
Abstract
Phyllosilicates are hydrous minerals formed by interaction between rock and liquid water, and are commonly found in meteorites that originate in the asteroid belt. Collisions between asteroids contribute to zodiacal dust, which therefore reasonably could include phyllosilicates. Collisions between planetesimals in protoplanetary disks may also produce dust that contains phyllosilicates. These minerals possess characteristic emission features in the mid-infrared and could be detectable in extrasolar protoplanetary disks. We have determined whether phyllosilicates in protoplanetary disks are detectable in the infrared, using instruments such as those on board the Spitzer Space Telescope and the Stratospheric Observatory for Infrared Astronomy (SOFIA). We calculated opacities for the phyllosilicates most common in meteorites and, using a two-layer radiative transfer model, computed the emission of radiation from a protoplanetary disk. We found that phyllosilicates present at the 3% level lead to observationally significant differences in disk spectra and should therefore be detectable with the use of infrared observations and spectral modeling. Detection of phyllosilicates in a protoplanetary disk would be diagnostic of liquid water in planetesimals in that disk and would demonstrate similarity to our own Solar System. We also discuss use of phyllosilicate emission to test the "water worlds" hypothesis, which proposes that liquid water in planetesimals should correlate with the inventory of short-lived radionuclides in planetary systems, especially (26)Al.
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Affiliation(s)
- Melissa A Morris
- School of Earth and Space Exploration, Arizona State University, Tempe, Arizona, USA.
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A unique basaltic micrometeorite expands the inventory of solar system planetary crusts. Proc Natl Acad Sci U S A 2009; 106:6904-9. [PMID: 19366660 DOI: 10.1073/pnas.0900328106] [Citation(s) in RCA: 36] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Micrometeorites with diameter approximately 100-200 microm dominate the flux of extraterrestrial matter on Earth. The vast majority of micrometeorites are chemically, mineralogically, and isotopically related to carbonaceous chondrites, which amount to only 2.5% of meteorite falls. Here, we report the discovery of the first basaltic micrometeorite (MM40). This micrometeorite is unlike any other basalt known in the solar system as revealed by isotopic data, mineral chemistry, and trace element abundances. The discovery of a new basaltic asteroidal surface expands the solar system inventory of planetary crusts and underlines the importance of micrometeorites for sampling the asteroids' surfaces in a way complementary to meteorites, mainly because they do not suffer dynamical biases as meteorites do. The parent asteroid of MM40 has undergone extensive metamorphism, which ended no earlier than 7.9 Myr after solar system formation. Numerical simulations of dust transport dynamics suggest that MM40 might originate from one of the recently discovered basaltic asteroids that are not members of the Vesta family. The ability to retrieve such a wealth of information from this tiny (a few micrograms) sample is auspicious some years before the launch of a Mars sample return mission.
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Trieloff M. 4.5 Chronology of the Solar System. SOLAR SYSTEM 2009:771-788. [DOI: 10.1007/978-3-540-88055-4_35] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/02/2023]
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13
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Srinivasan G, Whitehouse MJ, Weber I, Yamaguchi A. The Crystallization Age of Eucrite Zircon. Science 2007; 317:345-7. [PMID: 17641194 DOI: 10.1126/science.1140264] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Eucrites are a group of meteorites that represent the first planetary igneous activity following metal-silicate differentiation on an early planetesimal, similar to Asteroid 4 Vesta, and, thus, help date geophysical processes occurring on such bodies in the early solar system. Using the short-lived radionuclide (182)Hf as a relative chronometer, we demonstrate that eucrite zircon crystallized quickly within 6.8 million years of metal-silicate differentiation. This implies that mantle differentiation on the eucrite parent body occurred during a period when internal heat from the decay of (26)Al and (60)Fe was still available. Later metamorphism of eucrites took place at least 8.9 million years after the zircons crystallized and was likely caused by heating from impacts, or by burial under hot material excavated by impacts, rather than from lava flows. Thus, the timing of eucrite formation and of mantle differentiation is constrained.
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Affiliation(s)
- G Srinivasan
- Department of Geology, University of Toronto, Toronto, ON, Canada, M5S 3B1.
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14
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Ke Y, Solomatov VS. Early transient superplumes and the origin of the Martian crustal dichotomy. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002631] [Citation(s) in RCA: 40] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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15
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Bottke WF, Nesvorný D, Grimm RE, Morbidelli A, O'Brien DP. Iron meteorites as remnants of planetesimals formed in the terrestrial planet region. Nature 2006; 439:821-4. [PMID: 16482151 DOI: 10.1038/nature04536] [Citation(s) in RCA: 219] [Impact Index Per Article: 12.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/14/2005] [Accepted: 12/12/2005] [Indexed: 11/09/2022]
Abstract
Iron meteorites are core fragments from differentiated and subsequently disrupted planetesimals. The parent bodies are usually assumed to have formed in the main asteroid belt, which is the source of most meteorites. Observational evidence, however, does not indicate that differentiated bodies or their fragments were ever common there. This view is also difficult to reconcile with the fact that the parent bodies of iron meteorites were as small as 20 km in diameter and that they formed 1-2 Myr earlier than the parent bodies of the ordinary chondrites. Here we show that the iron-meteorite parent bodies most probably formed in the terrestrial planet region. Fast accretion times there allowed small planetesimals to melt early in Solar System history by the decay of short-lived radionuclides (such as 26Al, 60Fe). The protoplanets emerging from this population not only induced collisional evolution among the remaining planetesimals but also scattered some of the survivors into the main belt, where they stayed for billions of years before escaping via a combination of collisions, Yarkovsky thermal forces, and resonances. We predict that some asteroids are main-belt interlopers (such as (4) Vesta). A select few may even be remnants of the long-lost precursor material that formed the Earth.
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Affiliation(s)
- William F Bottke
- Southwest Research Institute, 1050 Walnut St, Suite 400, Boulder, Colorado 80302, USA.
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17
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Bizzarro M, Baker JA, Haack H. Mg isotope evidence for contemporaneous formation of chondrules and refractory inclusions. Nature 2004; 431:275-8. [PMID: 15372023 DOI: 10.1038/nature02882] [Citation(s) in RCA: 197] [Impact Index Per Article: 9.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/21/2004] [Accepted: 07/21/2004] [Indexed: 11/09/2022]
Abstract
Primitive or undifferentiated meteorites (chondrites) date back to the origin of the Solar System, and thus preserve a record of the physical and chemical processes that occurred during the earliest evolution of the accretion disk surrounding the young Sun. The oldest Solar System materials present within these meteorites are millimetre- to centimetre-sized calcium-aluminium-rich inclusions (CAIs) and ferromagnesian silicate spherules (chondrules), which probably originated by thermal processing of pre-existing nebula solids. Chondrules are currently believed to have formed approximately 2-3 million years (Myr) after CAIs (refs 5-10)--a timescale inconsistent with the dynamical lifespan of small particles in the early Solar System. Here, we report the presence of excess (26)Mg resulting from in situ decay of the short-lived (26)Al nuclide in CAIs and chondrules from the Allende meteorite. Six CAIs define an isochron corresponding to an initial (26)Al/(27)Al ratio of (5.25 +/- 0.10) x 10(-5), and individual model ages with uncertainties as low as +/- 30,000 years, suggesting that these objects possibly formed over a period as short as 50,000 years. In contrast, the chondrules record a range of initial (26)Al/(27)Al ratios from (5.66 +/- 0.80) to (1.36 +/- 0.52) x 10(-5), indicating that Allende chondrule formation began contemporaneously with the formation of CAIs, and continued for at least 1.4 Myr. Chondrule formation processes recorded by Allende and other chondrites may have persisted for at least 2-3 Myr in the young Solar System.
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Affiliation(s)
- Jamie Gilmour
- Department of Earth Sciences, University of Manchester, Manchester M13 9PL, UK.
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Kleine T, Münker C, Mezger K, Palme H. Rapid accretion and early core formation on asteroids and the terrestrial planets from Hf-W chronometry. Nature 2002; 418:952-5. [PMID: 12198541 DOI: 10.1038/nature00982] [Citation(s) in RCA: 86] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/27/2022]
Abstract
The timescales and mechanisms for the formation and chemical differentiation of the planets can be quantified using the radioactive decay of short-lived isotopes. Of these, the (182)Hf-to-(182)W decay is ideally suited for dating core formation in planetary bodies. In an earlier study, the W isotope composition of the Earth's mantle was used to infer that core formation was late (> or = 60 million years after the beginning of the Solar System) and that accretion was a protracted process. The correct interpretation of Hf-W data depends, however, on accurate knowledge of the initial abundance of (182)Hf in the Solar System and the W isotope composition of chondritic meteorites. Here we report Hf-W data for carbonaceous and H chondrite meteorites that lead to timescales of accretion and core formation significantly different from those calculated previously. The revised ages for Vesta, Mars and Earth indicate rapid accretion, and show that the timescale for core formation decreases with decreasing size of the planet. We conclude that core formation in the terrestrial planets and the formation of the Moon must have occurred during the first approximately 30 million years of the life of the Solar System.
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Affiliation(s)
- T Kleine
- Institut für Mineralogie, Universität Münster, Corrensstrasse 24, D-48149 Münster, Germany.
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