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Arrowsmith-Kron G, Athanasakis-Kaklamanakis M, Au M, Ballof J, Berger R, Borschevsky A, Breier AA, Buchinger F, Budker D, Caldwell L, Charles C, Dattani N, de Groote RP, DeMille D, Dickel T, Dobaczewski J, Düllmann CE, Eliav E, Engel J, Fan M, Flambaum V, Flanagan KT, Gaiser AN, Garcia Ruiz RF, Gaul K, Giesen TF, Ginges JSM, Gottberg A, Gwinner G, Heinke R, Hoekstra S, Holt JD, Hutzler NR, Jayich A, Karthein J, Leach KG, Madison KW, Malbrunot-Ettenauer S, Miyagi T, Moore ID, Moroch S, Navratil P, Nazarewicz W, Neyens G, Norrgard EB, Nusgart N, Pašteka LF, N Petrov A, Plaß WR, Ready RA, Pascal Reiter M, Reponen M, Rothe S, Safronova MS, Scheidenerger C, Shindler A, Singh JT, Skripnikov LV, Titov AV, Udrescu SM, Wilkins SG, Yang X. Opportunities for fundamental physics research with radioactive molecules. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2024; 87:084301. [PMID: 38215499 DOI: 10.1088/1361-6633/ad1e39] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/10/2023] [Accepted: 01/12/2024] [Indexed: 01/14/2024]
Abstract
Molecules containing short-lived, radioactive nuclei are uniquely positioned to enable a wide range of scientific discoveries in the areas of fundamental symmetries, astrophysics, nuclear structure, and chemistry. Recent advances in the ability to create, cool, and control complex molecules down to the quantum level, along with recent and upcoming advances in radioactive species production at several facilities around the world, create a compelling opportunity to coordinate and combine these efforts to bring precision measurement and control to molecules containing extreme nuclei. In this manuscript, we review the scientific case for studying radioactive molecules, discuss recent atomic, molecular, nuclear, astrophysical, and chemical advances which provide the foundation for their study, describe the facilities where these species are and will be produced, and provide an outlook for the future of this nascent field.
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Affiliation(s)
- Gordon Arrowsmith-Kron
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI 48824, United States of America
| | - Michail Athanasakis-Kaklamanakis
- Experimental Physics Department, CERN, CH-1211 Geneva 23, Switzerland
- KU Leuven, Department of Physics and Astronomy, Instituut voor Kern- en Stralingsfysica, B-3001 Leuven, Belgium
| | - Mia Au
- CERN, Geneva, Switzerland
- Johannes Gutenberg-Universität Mainz, Mainz, Germany
| | - Jochen Ballof
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI 48824, United States of America
- Accelerator Systems Department, CERN, 1211 Geneva 23, Switzerland
| | - Robert Berger
- Fachbereich Chemie, Philipps-Universität Marburg, Hans-Meerwein-Straße 4, 35032 Marburg, Germany
| | - Anastasia Borschevsky
- Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Groningen, The Netherlands
| | - Alexander A Breier
- Institute of Physics, University of Kassel, Heinrich-Plett-Str. 40, 34132 Kassel, Germany
| | | | - Dmitry Budker
- Helmholtz-Institut, GSI Helmholtzzentrum fur Schwerionenforschung and Johannes Gutenberg University, Mainz 55128, Germany
- Department of Physics, University of California at Berkeley, Berkeley, CA 94720-7300, United States of America
| | - Luke Caldwell
- JILA, NIST and University of Colorado, Boulder, CO 80309, United States of America
- Department of Physics, University of Colorado, Boulder, CO 80309, United States of America
| | - Christopher Charles
- TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada
- University of Western Ontario, 1151 Richmond St. N., London, Ontario N6A 5B7, Canada
| | - Nike Dattani
- HPQC Labs, Waterloo, Ontario, Canada
- HPQC College, Waterloo, Ontario, Canada
| | - Ruben P de Groote
- Instituut voor Kern- en Stralingsfysica, KU Leuven, Leuven, Belgium
- Department of Physics, University of Jyväskylä, Jyväskylä, Finland
| | - David DeMille
- University of Chicago, Chicago, IL, United States of America
- Argonne National Laboratory, Lemont, IL, United States of America
| | - Timo Dickel
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- II. Physikalisches Institut, Justus-Liebig-Universität Gießen, 35392 Gießen, Germany
| | - Jacek Dobaczewski
- School of Physics, Engineering and Technology, University of York, Heslington, York YO10 5DD, United Kingdom
- Institute of Theoretical Physics, Faculty of Physics, University of Warsaw, ul. Pasteura 5, PL-02-093 Warsaw, Poland
| | - Christoph E Düllmann
- Department of Chemistry-TRIGA Site, Johannes Gutenberg University, Fritz-Strassmann-Weg 2, 55128 Mainz, Germany
- GSI Helmholtzzentrum für Schwerionenforschung, Planckstr. 1, 64291 Darmstadt, Germany
- Helmholtz Institute Mainz, Staudingerweg 18, 55128 Mainz, Germany
| | - Ephraim Eliav
- School of Chemistry, Tel Aviv University, Ramat Aviv, Tel Aviv 69978, Israel
| | - Jonathan Engel
- Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, United States of America
| | - Mingyu Fan
- Department of Physics, University of California, Santa Barbara, CA 93106, United States of America
| | | | - Kieran T Flanagan
- Photon Science Institute, Department of Physics and Astronomy, University of Manchester, Manchester M13 9PL, United Kingdom
| | - Alyssa N Gaiser
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI 48824, United States of America
| | - Ronald F Garcia Ruiz
- Massachusetts Institute of Technology, Cambridge, MA 02139, United States of America
| | - Konstantin Gaul
- Fachbereich Chemie, Philipps-Universität Marburg, Hans-Meerwein-Straße 4, 35032 Marburg, Germany
| | - Thomas F Giesen
- Institute of Physics, University of Kassel, Heinrich-Plett-Str. 40, 34132 Kassel, Germany
| | - Jacinda S M Ginges
- School of Mathematics and Physics, The University of Queensland, Brisbane QLD 4072, Australia
| | | | - Gerald Gwinner
- Department of Physics and Astronomy, University of Manitoba, Winnipeg, MB R3T 3M9, Canada
| | | | - Steven Hoekstra
- Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Groningen, The Netherlands
- Nikhef, National Institute for Subatomic Physics, Amsterdam, The Netherlands
| | - Jason D Holt
- TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada
- Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada
| | - Nicholas R Hutzler
- California Institute of Technology, Pasadena, CA 91125, United States of America
| | - Andrew Jayich
- Department of Physics, University of California, Santa Barbara, CA 93106, United States of America
| | - Jonas Karthein
- Massachusetts Institute of Technology, Cambridge, MA 02139, United States of America
| | - Kyle G Leach
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI 48824, United States of America
- Colorado School of Mines, Golden, CO 80401, United States of America
| | - Kirk W Madison
- Department of Physics and Astronomy, University of British Columbia, Vancouver, BC V6T1Z1, Canada
| | - Stephan Malbrunot-Ettenauer
- TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada
- Department of Physics, University of Toronto, 60 St. George St., Toronto, Ontario, Canada
| | | | - Iain D Moore
- Accelerator Laboratory, Department of Physics, University of Jyväskylä, Jyväskylä 40014, Finland
| | - Scott Moroch
- Massachusetts Institute of Technology, Cambridge, MA 02139, United States of America
| | - Petr Navratil
- TRIUMF, 4004 Wesbrook Mall, Vancouver, BC V6T 2A3, Canada
| | - Witold Nazarewicz
- Facility for Rare Isotope Beams and Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, United States of America
| | - Gerda Neyens
- KU Leuven, Department of Physics and Astronomy, Instituut voor Kern- en Stralingsfysica, B-3001 Leuven, Belgium
| | - Eric B Norrgard
- Sensor Science Division, National Institute of Standards and Technology, Gaithersburg, MD 20899, United States of America
| | - Nicholas Nusgart
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI 48824, United States of America
| | - Lukáš F Pašteka
- Van Swinderen Institute for Particle Physics and Gravity, University of Groningen, Groningen, The Netherlands
- Department of Physical and Theoretical Chemistry, Faculty of Natural Sciences, Comenius University, Bratislava, Slovakia
| | - Alexander N Petrov
- Petersburg Nuclear Physics Institute named by B.P. Konstantinov of National Research Center 'Kurchatov Institute' (NRC 'Kurchatov Institute'-PNPI), 1 Orlova roscha mcr., Gatchina 188300, Leningrad Region, Russia
- Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg 199034, Russia
| | - Wolfgang R Plaß
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- II. Physikalisches Institut, Justus-Liebig-Universität Gießen, 35392 Gießen, Germany
| | - Roy A Ready
- Department of Physics, University of California, Santa Barbara, CA 93106, United States of America
| | - Moritz Pascal Reiter
- School of Physics & Astronomy, The University of Edinburgh, Peter Guthrie Tait Road, EH9 3FD Edinburgh, United Kingdom
| | - Mikael Reponen
- Accelerator Laboratory, Department of Physics, University of Jyväskylä, Jyväskylä 40014, Finland
| | | | - Marianna S Safronova
- Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, United States of America
- Joint Quantum Institute, National Institute of Standards and Technology and the University of Maryland, Gaithersburg, MD 20742, United States of America
| | - Christoph Scheidenerger
- GSI Helmholtzzentrum für Schwerionenforschung GmbH, 64291 Darmstadt, Germany
- II. Physikalisches Institut, Justus-Liebig-Universität Gießen, 35392 Gießen, Germany
- Helmholtz Forschungsakademie Hessen für FAIR (HFHF), Campus Gießen, Gießen, Germany
| | - Andrea Shindler
- Facility for Rare Isotope Beams & Physics Department, Michigan State University, East Lansing, MI 48824, United States of America
| | - Jaideep T Singh
- Facility for Rare Isotope Beams, Michigan State University, East Lansing, MI, United States of America
| | - Leonid V Skripnikov
- Petersburg Nuclear Physics Institute named by B.P. Konstantinov of National Research Center 'Kurchatov Institute' (NRC 'Kurchatov Institute'-PNPI), 1 Orlova roscha mcr., Gatchina 188300, Leningrad Region, Russia
- Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg 199034, Russia
| | - Anatoly V Titov
- Petersburg Nuclear Physics Institute named by B.P. Konstantinov of National Research Center 'Kurchatov Institute' (NRC 'Kurchatov Institute'-PNPI), 1 Orlova roscha mcr., Gatchina 188300, Leningrad Region, Russia
- Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg 199034, Russia
| | - Silviu-Marian Udrescu
- Massachusetts Institute of Technology, Cambridge, MA 02139, United States of America
| | - Shane G Wilkins
- Massachusetts Institute of Technology, Cambridge, MA 02139, United States of America
| | - Xiaofei Yang
- School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, People's Republic of China
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Brandt PC, Provornikova E, Bale SD, Cocoros A, DeMajistre R, Dialynas K, Elliott HA, Eriksson S, Fields B, Galli A, Hill ME, Horanyi M, Horbury T, Hunziker S, Kollmann P, Kinnison J, Fountain G, Krimigis SM, Kurth WS, Linsky J, Lisse CM, Mandt KE, Magnes W, McNutt RL, Miller J, Moebius E, Mostafavi P, Opher M, Paxton L, Plaschke F, Poppe AR, Roelof EC, Runyon K, Redfield S, Schwadron N, Sterken V, Swaczyna P, Szalay J, Turner D, Vannier H, Wimmer-Schweingruber R, Wurz P, Zirnstein EJ. Future Exploration of the Outer Heliosphere and Very Local Interstellar Medium by Interstellar Probe. SPACE SCIENCE REVIEWS 2023; 219:18. [PMID: 36874191 PMCID: PMC9974711 DOI: 10.1007/s11214-022-00943-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 05/20/2022] [Accepted: 12/07/2022] [Indexed: 06/18/2023]
Abstract
A detailed overview of the knowledge gaps in our understanding of the heliospheric interaction with the largely unexplored Very Local Interstellar Medium (VLISM) are provided along with predictions of with the scientific discoveries that await. The new measurements required to make progress in this expanding frontier of space physics are discussed and include in-situ plasma and pick-up ion measurements throughout the heliosheath, direct sampling of the VLISM properties such as elemental and isotopic composition, densities, flows, and temperatures of neutral gas, dust and plasma, and remote energetic neutral atom (ENA) and Lyman-alpha (LYA) imaging from vantage points that can uniquely discern the heliospheric shape and bring new information on the interaction with interstellar hydrogen. The implementation of a pragmatic Interstellar Probe mission with a nominal design life to reach 375 Astronomical Units (au) with likely operation out to 550 au are reported as a result of a 4-year NASA funded mission study.
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Affiliation(s)
- P. C. Brandt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - E. Provornikova
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - S. D. Bale
- University of California Berkeley, Berkeley, CA USA
| | - A. Cocoros
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - R. DeMajistre
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. Dialynas
- Office of Space Research and Technology, Academy of Athens, Athens, 10679 Greece
| | | | - S. Eriksson
- Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO USA
| | - B. Fields
- University of Illinois Urbana-Champaign, Urbana, IL USA
| | - A. Galli
- University of Bern, Bern, Switzerland
| | - M. E. Hill
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - M. Horanyi
- Laboratory for Atmospheric and Space Physics, University of Colorado at Boulder, Boulder, CO USA
| | | | | | - P. Kollmann
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - J. Kinnison
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - G. Fountain
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - S. M. Krimigis
- Office of Space Research and Technology, Academy of Athens, Athens, 10679 Greece
| | | | - J. Linsky
- University of Colorado Boulder, Boulder, CO USA
| | - C. M. Lisse
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. E. Mandt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - W. Magnes
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - R. L. McNutt
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | - E. Moebius
- University of New Hampshire, Durham, NH USA
| | - P. Mostafavi
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - M. Opher
- Boston University, Boston, MA USA
| | - L. Paxton
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - F. Plaschke
- Technical University Braunschweig, Braunschweig, Germany
| | - A. R. Poppe
- University of California Berkeley, Berkeley, CA USA
| | - E. C. Roelof
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | - K. Runyon
- Planetary Science Institute, Tucson, AZ USA
| | | | | | | | | | - J. Szalay
- Princeton University, Princeton, NJ USA
| | - D. Turner
- The Johns Hopkins University Applied Physics Laboratory, Laurel, MD USA
| | | | | | - P. Wurz
- University of Bern, Bern, Switzerland
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3
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The initial exploration for 26Al chronology in deep-sea ferromanganese crust. RADIATION DETECTION TECHNOLOGY AND METHODS 2023. [DOI: 10.1007/s41605-023-00386-0] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/24/2023]
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4
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Siraj A, Loeb A. The New Astronomical Frontier of Interstellar Objects. ASTROBIOLOGY 2022; 22:1459-1470. [PMID: 36475962 DOI: 10.1089/ast.2021.0189] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/17/2023]
Abstract
The upcoming commencement of the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST) will greatly enhance the discovery rate of interstellar objects (ISOs). 'Oumuamua and Borisov were the first two ISOs confirmed in the Solar System, although the first interstellar meteor was detected earlier. We explore the intriguing mass budget of ejected planetesimals implied by the detections of 'Oumuamua and Borisov and explore the expected abundance of ISOs as a function of size in the solar neighborhood. Specifically, we find that a significant fraction of stellar mass must go toward producing ISOs and that ISOs outnumber Solar System objects in the Oort cloud. We consider signatures of ISOs colliding with Earth, the Moon, and neutron stars, as well as the possibility of differentiating ISOs from Solar System objects in stellar occultation surveys, and we show that these methods are observationally feasible. We introduce a test for dynamical anisotropy that is capable of determining the typical ejection speed of ISOs from their parent stars. Finally, we predict a new population of dynamically distinct ISOs originating from stars in the Galactic halo. One of the two branches of the newly established Galileo Project1 seeks to learn more about the nature of ISOs like 'Oumuamua by performing new searches and designing follow-up observations.
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Affiliation(s)
- Amir Siraj
- Department of Astronomy, Harvard University, Cambridge, Massachusetts, USA
| | - Abraham Loeb
- Department of Astronomy, Harvard University, Cambridge, Massachusetts, USA
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5
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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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Heinitz S, Kajan I, Schumann D. How accurate are half-life data of long-lived radionuclides? RADIOCHIM ACTA 2022. [DOI: 10.1515/ract-2021-1135] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022]
Abstract
Abstract
We have consulted existing half-life data available in Nuclear Data Sheets for radionuclides with Z < 89 in the range between 30 and 108 years with emphasis on their uncertainty. Based on this dataset, we have highlighted the lack of reliable data by giving examples for nuclides relevant for astrophysical, environmental and nuclear research. It is shown that half-lives for a substantial number of nuclides require a re-determination since existing data are either based on one single measurement, are contradictory or are associated with uncertainties above 5%.
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Affiliation(s)
| | - Ivan Kajan
- Paul Scherrer Institute (PSI) , Villigen , Switzerland
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Koll D, Faestermann T, Korschinek G, Leya I, Merchel S, Wallner A. The Dyadic Radionuclide System 60Fe / 53Mn to Distinguish Interstellar from Interplanetary 60Fe. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202226011022] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The discovery of live 60Fe in a deep-sea crust with proposed interstellar origin followed by evidence for elevated interplanetary 3He in the same crust raised the question on how to unambiguously identify the true production site of the identified 60Fe. Here, we show the implementation of the dyadic radionuclide system 60Fe / 53Mn to serve as a tool for the identification of surplus interstellar 60Fe over interplanetary production. The recent updates in experimental 60Fe and 53Mn data from iron meteorites as well as in production rate models confirm the validity and robustness of this dyadic system for future applications.
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Boschini MJ, Della Torre S, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. The Discovery of a Low-energy Excess in Cosmic-Ray Iron: Evidence of the Past Supernova Activity in the Local Bubble. THE ASTROPHYSICAL JOURNAL 2021; 913:5. [PMID: 34646050 PMCID: PMC8506974 DOI: 10.3847/1538-4357/abf11c] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Since its launch, the Alpha Magnetic Spectrometer-02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species ( p ¯ , e ±, and nuclei, 1H-8O, 10Ne, 12Mg, 14Si) which resulted in a number of breakthroughs. One of the latest long-awaited surprises is the spectrum of 26Fe just published by AMS-02. Because of the large fragmentation cross section and large ionization energy losses, most of CR iron at low energies is local and may harbor some features associated with relatively recent supernova (SN) activity in the solar neighborhood. Our analysis of the new AMS-02 results, together with Voyager 1 and ACE-CRIS data, reveals an unexpected bump in the iron spectrum and in the Fe/He, Fe/O, and Fe/Si ratios at 1-2 GV, while a similar feature in the spectra of He, O, and Si and in their ratios is absent, hinting at a local source of low-energy CRs. The found excess extends the recent discoveries of radioactive 60Fe deposits in terrestrial and lunar samples and in CRs. We provide an updated local interstellar spectrum (LIS) of iron in the energy range from 1 MeV nucleon-1 to ~10 TeV nucleon-1. Our calculations employ the GALPROP-HELMOD framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei Z ⩽ 28.
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Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
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Wallner A, Froehlich MB, Hotchkis MAC, Kinoshita N, Paul M, Martschini M, Pavetich S, Tims SG, Kivel N, Schumann D, Honda M, Matsuzaki H, Yamagata T. 60Fe and 244Pu deposited on Earth constrain the r-process yields of recent nearby supernovae. Science 2021; 372:742-745. [PMID: 33986180 DOI: 10.1126/science.aax3972] [Citation(s) in RCA: 21] [Impact Index Per Article: 7.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/21/2019] [Accepted: 04/12/2021] [Indexed: 11/02/2022]
Abstract
Half of the chemical elements heavier than iron are produced by the rapid neutron capture process (r-process). The sites and yields of this process are disputed, with candidates including some types of supernovae (SNe) and mergers of neutron stars. We search for two isotopic signatures in a sample of Pacific Ocean crust-iron-60 (60Fe) (half-life, 2.6 million years), which is predominantly produced in massive stars and ejected in supernova explosions, and plutonium-244 (244Pu) (half-life, 80.6 million years), which is produced solely in r-process events. We detect two distinct influxes of 60Fe to Earth in the last 10 million years and accompanying lower quantities of 244Pu. The 244Pu/60Fe influx ratios are similar for both events. The 244Pu influx is lower than expected if SNe dominate r-process nucleosynthesis, which implies some contribution from other sources.
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Affiliation(s)
- A Wallner
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia. .,Helmholtz-Zentrum Dresden-Rossendorf, Institute of Ion Beam Physics and Materials Research, 01328 Dresden, Germany
| | - M B Froehlich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - M A C Hotchkis
- Australian Nuclear Science and Technology Organisation, Lucas Heights, NSW 2234, Australia
| | - N Kinoshita
- Institute of Technology, Shimizu Corporation, Tokyo 135-8530, Japan
| | - M Paul
- Racah Institute of Physics, The Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - M Martschini
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - S Pavetich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - S G Tims
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - N Kivel
- Laboratory of Radiochemistry, Department for Nuclear Energy and Safety, Paul Scherrer Institute, 5232 Villigen, Switzerland
| | - D Schumann
- Laboratory of Radiochemistry, Department for Nuclear Energy and Safety, Paul Scherrer Institute, 5232 Villigen, Switzerland
| | - M Honda
- Graduate School of Pure and Applied Sciences, University of Tsukuba, Ibaraki 305-8577, Japan
| | - H Matsuzaki
- Micro Analysis Laboratory, Tandem Accelerator, The University Museum, The University of Tokyo, Tokyo 113-0032, Japan
| | - T Yamagata
- Micro Analysis Laboratory, Tandem Accelerator, The University Museum, The University of Tokyo, Tokyo 113-0032, Japan
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10
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Malkov MA, Moskalenko IV. The TeV Cosmic-Ray Bump: A Message from the Epsilon Indi or Epsilon Eridani Star? THE ASTROPHYSICAL JOURNAL 2021; 911:151. [PMID: 34646049 PMCID: PMC8506973 DOI: 10.3847/1538-4357/abe855] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/13/2023]
Abstract
A recently observed bump in the cosmic-ray (CR) spectrum from 0.3 to 30 TV is likely caused by a stellar bow shock that reaccelerates preexisting CRs, which further propagate to the Sun along the magnetic field lines. Along their way, these particles generate an Iroshnikov-Kraichnan (I-K) turbulence that controls their propagation and sustains the bump. Ad hoc fitting of the bump shape requires six adjustable parameters. Our model requires none, merely depending on three physical unknowns that we constrain using the fit. These are the shock Mach number, M, its size, l ⊥, and the distance to it, ζ obs. Altogether, they define the bump rigidity R 0. With M ≈ 1.5-1.6 and R 0 ≈ 4.4 TV, the model fits the data with ≈0.08% accuracy. The fit critically requires the I-K spectrum predicted by the model and rules out the alternatives. These attributes of the fit make an accidental agreement highly unlikely. In turn, the R 0 and M derived from the fit impose the distance-size relation on the shock:ζ obs ( pc ) ~ 10 2 l ⊥ ( pc ) . For sufficiently large bow shocks, l ⊥ = 10-3-10-2 pc, we find the distance of ζ obs = 3-10 pc. Three promising stars in this range are the Scholz's Star at 6.8 pc, Epsilon Indi at 3.6 pc, and Epsilon Eridani at 3.2 pc. Based on their current positions and velocities, we propose that Epsilon Indi and Epsilon Eridani can produce the observed spectral bump. Moreover, Epsilon Eridani's position is only ~6°.7 off of the magnetic field direction in the solar neighborhood, which also changes the CR arrival direction distribution. Given the proximity of these stars, the bump appearance may change in a relatively short time.
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Affiliation(s)
- Mikhail A Malkov
- Department of Physics and CASS, University of California, San Diego, La Jolla, CA 92093, USA
| | - Igor V Moskalenko
- Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
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11
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Crawford IA, Joy KH, Pasckert JH, Hiesinger H. The lunar surface as a recorder of astrophysical processes. PHILOSOPHICAL TRANSACTIONS. SERIES A, MATHEMATICAL, PHYSICAL, AND ENGINEERING SCIENCES 2021; 379:20190562. [PMID: 33222641 PMCID: PMC7739904 DOI: 10.1098/rsta.2019.0562] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 08/13/2020] [Indexed: 06/11/2023]
Abstract
The lunar surface has been exposed to the space environment for billions of years and during this time has accumulated records of a wide range of astrophysical phenomena. These include solar wind particles and the cosmogenic products of solar particle events which preserve a record of the past evolution of the Sun, and cosmogenic nuclides produced by high-energy galactic cosmic rays which potentially record the galactic environment of the Solar System through time. The lunar surface may also have accreted material from the local interstellar medium, including supernova ejecta and material from interstellar clouds encountered by the Solar System in the past. Owing to the Moon's relatively low level of geological activity, absence of an atmosphere, and, for much of its history, lack of a magnetic field, the lunar surface is ideally suited to collect these astronomical records. Moreover, the Moon exhibits geological processes able to bury and thus both preserve and 'time-stamp' these records, although gaining access to them is likely to require a significant scientific infrastructure on the lunar surface. This article is part of a discussion meeting issue 'Astronomy from the Moon: the next decades'.
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Affiliation(s)
- Ian A. Crawford
- Department of Earth and Planetary Sciences, Birkbeck College, University of London, Malet Street, London WC1E 7HX, UK
- Centre for Planetary Sciences at UCL/Birkbeck, Gower Street, London WC1E 6BT, UK
| | - Katherine H. Joy
- Department of Earth and Environmental Sciences, The University of Manchester, Oxford Road, M13 9PL Manchester, UK
| | - Jan H. Pasckert
- Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
| | - Harald Hiesinger
- Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Straße 10, 48149 Münster, Germany
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12
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Venkataramani V. Iron Homeostasis and Metabolism: Two Sides of a Coin. ADVANCES IN EXPERIMENTAL MEDICINE AND BIOLOGY 2021; 1301:25-40. [PMID: 34370286 DOI: 10.1007/978-3-030-62026-4_3] [Citation(s) in RCA: 28] [Impact Index Per Article: 9.3] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 02/07/2023]
Abstract
Iron is an ancient, essential and versatile transition metal found in almost all living organisms on Earth. This fundamental trace element is used in the synthesis of heme and iron-sulfur (Fe-S) containing proteins and other vital cofactors that are involved in respiration, redox reactions, catalysis, DNA synthesis and transcription. At the same time, the ability of iron to cycle between its oxidized, ferric (Fe3+) and its reduced, ferrous (Fe2+) state contributes to the production of free radicals that can damage biomolecules, including proteins, lipids and DNA. In particular, the regulated non-apoptotic cell death ferroptosis is driven by Fe2+-dependent lipid peroxidation that can be prevented by iron chelation or genetic inhibition of cellular iron uptake. Therefore, iron homeostasis must be tightly regulated to avoid iron toxicity. This review provides an overview of the origin and chemistry of iron that makes it suitable for a variety of biological functions and addresses how organisms evolved various strategies, including their scavenging and antioxidant machinery, to manage redox-associated drawbacks. Finally, key mechanisms of iron metabolism are highlighted in human diseases and model organisms, underlining the perils of dysfunctional iron handlings.
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Affiliation(s)
- Vivek Venkataramani
- Institute of Pathology, University Medical Center Göttingen (UMG), Göttingen, Germany.
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13
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Wallner A, Feige J, Fifield LK, Froehlich MB, Golser R, Hotchkis MAC, Koll D, Leckenby G, Martschini M, Merchel S, Panjkov S, Pavetich S, Rugel G, Tims SG. 60Fe deposition during the late Pleistocene and the Holocene echoes past supernova activity. Proc Natl Acad Sci U S A 2020; 117:21873-21879. [PMID: 32839339 PMCID: PMC7486756 DOI: 10.1073/pnas.1916769117] [Citation(s) in RCA: 9] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Nuclides synthesized in massive stars are ejected into space via stellar winds and supernova explosions. The solar system (SS) moves through the interstellar medium and collects these nucleosynthesis products. One such product is 60Fe, a radionuclide with a half-life of 2.6 My that is predominantly produced in massive stars and ejected in supernova explosions. Extraterrestrial 60Fe has been found on Earth, suggesting close-by supernova explosions ∼2 to 3 and ∼6 Ma. Here, we report on the detection of a continuous interstellar 60Fe influx on Earth over the past ∼33,000 y. This time period coincides with passage of our SS through such interstellar clouds, which have a significantly larger particle density compared to the local average interstellar medium embedding our SS for the past few million years. The interstellar 60Fe was extracted from five deep-sea sediment samples and accelerator mass spectrometry was used for single-atom counting. The low number of 19 detected atoms indicates a continued but low influx of interstellar 60Fe. The measured 60Fe time profile over the 33 ky, obtained with a time resolution of about ±9 ky, does not seem to reflect any large changes in the interstellar particle density during Earth's passage through local interstellar clouds, which could be expected if the local cloud represented an isolated remnant of the most recent supernova ejecta that traversed the Earth ∼2 to 3 Ma. The identified 60Fe influx may signal a late echo of some million-year-old supernovae with the 60Fe-bearing dust particles still permeating the interstellar medium.
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Affiliation(s)
- A Wallner
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia;
- Institute of Ion Beam Physics and Materials Research, Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
| | - J Feige
- Isotope Physics, Faculty of Physics, Vienna Environmental Research Accelerator Laboratory, University of Vienna, 1090 Vienna, Austria
- Zentrum für Astronomie und Astrophysik, Technische Universität Berlin, 10623 Berlin, Germany
| | - L K Fifield
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - M B Froehlich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - R Golser
- Isotope Physics, Faculty of Physics, Vienna Environmental Research Accelerator Laboratory, University of Vienna, 1090 Vienna, Austria
| | - M A C Hotchkis
- Centre for Accelerator Science, Australian Nuclear Science and Technology Organisation, Lucas Heights, NSW 2234, Australia
| | - D Koll
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - G Leckenby
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - M Martschini
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
- Isotope Physics, Faculty of Physics, Vienna Environmental Research Accelerator Laboratory, University of Vienna, 1090 Vienna, Austria
| | - S Merchel
- Institute of Ion Beam Physics and Materials Research, Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
| | - S Panjkov
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - S Pavetich
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
| | - G Rugel
- Institute of Ion Beam Physics and Materials Research, Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
| | - S G Tims
- Department of Nuclear Physics, Research School of Physics, Australian National University, Canberra, ACT 2601, Australia
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14
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Fujimoto Y, Krumholz MR, Inutsuka SI. Distribution and kinematics of 26Al in the Galactic disc. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2020; 497:2442-2454. [PMID: 32792749 PMCID: PMC7410101 DOI: 10.1093/mnras/staa2125] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/03/2020] [Revised: 07/01/2020] [Accepted: 07/09/2020] [Indexed: 06/11/2023]
Abstract
26Al is a short-lived radioactive isotope thought to be injected into the interstellar medium (ISM) by massive stellar winds and supernovae (SNe). However, all-sky maps of 26Al emission show a distribution with a much larger scale height and faster rotation speed than either massive stars or the cold ISM. We investigate the origin of this discrepancy using an N-body + hydrodynamics simulation of a Milky-Way-like galaxy, self-consistently including self-gravity, star formation, stellar feedback, and 26Al production. We find no evidence that the Milky Way's spiral structure explains the 26Al anomaly. Stars and the 26Al bubbles they produce form along spiral arms, but, because our simulation produces material arms that arise spontaneously rather than propagating arms forced by an external potential, star formation occurs at arm centres rather than leading edges. As a result, we find a scale height and rotation speed for 26Al similar to that of the cold ISM. However, we also show that a synthetic 26Al emission map produced for a possible Solar position at the edge of a large 26Al bubble recovers many of the major qualitative features of the observed 26Al sky. This suggests that the observed anomalous 26Al distribution is the product of foreground emission from the 26Al produced by a nearby, recent SN.
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Affiliation(s)
- Yusuke Fujimoto
- Earth and Planets Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road, NW, Washington, DC 20015, USA
| | - Mark R Krumholz
- Research School of Astronomy and Astrophysics, Australian National University, Canberra, 2611 ACT, Australia
- ARC Centre of Excellence for Astronomy in Three Dimensions (ASTRO-3D), Canberra, 2611 ACT, Australia
| | - Shu-ichiro Inutsuka
- Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8602, Japan
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15
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Korschinek G, Faestermann T, Poutivtsev M, Arazi A, Knie K, Rugel G, Wallner A. Supernova-Produced ^{53}Mn on Earth. PHYSICAL REVIEW LETTERS 2020; 125:031101. [PMID: 32745435 DOI: 10.1103/physrevlett.125.031101] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/16/2019] [Revised: 04/13/2020] [Accepted: 06/18/2020] [Indexed: 06/11/2023]
Abstract
For the time period from 1.5 to 4 Myr before the present we found in deep ocean ferromanganese crusts a ^{53}Mn excess concentration in terms of ^{53}Mn/Mn of about 4×10^{-14} over that expected for cosmogenic production. We conclude that this ^{53}Mn is of supernova origin because it is detected in the same time window, about 2.5 Myr ago, where ^{60}Fe has been found earlier. This overabundance confirms the supernova origin of that ^{60}Fe. For the first time, supernova-formed ^{53}Mn has been detected and it is the second positively identified radioisotope from the same supernova. The ratio ^{53}Mn/^{60}Fe of about 14 is consistent with that expected for a SN with a 11-25 M_{⊙} progenitor mass and solar metallicity.
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Affiliation(s)
- G Korschinek
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - T Faestermann
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - M Poutivtsev
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - A Arazi
- Laboratorio TANDAR, Comisión Nacional de Energía Atómica, Av. Gral. Paz 1499, B1650KNA San Martín, Argentina
- Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET), Av. Rivadavia 1917, C1033AAJ Buenos Aires, Argentina
| | - K Knie
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - G Rugel
- Physik-Department, Technische Universität München, 85748 Garching, Germany
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
| | - A Wallner
- Physik-Department, Technische Universität München, 85748 Garching, Germany
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
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16
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Bouyahiaoui M, Kachelrieß M, Semikoz D. High-energy neutrinos from cosmic ray interactions in the local bubble. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.101.123023] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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17
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Martschini M, Lachner J, Merchel S, Priller A, Steier P, Wallner A, Wieser A, Golser R. The quest for AMS of 182Hf – why poor gas gives pure beams. EPJ WEB OF CONFERENCES 2020. [DOI: 10.1051/epjconf/202023202003] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
The long-lived radioisotope 182Hf (T1/2 = 8.9 Ma) is of high astrophysical interest as its potential abundance in environmental archives would provide insight into recent r-process nucleosynthesis in the vicinity of our solar system. Despite substantial efforts, it could not be measured at natural abundances with conventional AMS so far due to strong isobaric interference from stable 182W. Equally important is an increase in ion source efficiency for the anions of interest.
The new Ion Laser InterAction Mass Spectrometry (ILIAMS) technique at VERA tackles the problem of elemental selectivity in AMS with a novel approach. It achieves near-complete suppression of isobar contaminants via selective laser photodetachment of decelerated anion beams in a gas-filled radio-frequency quadrupole (RFQ) ion cooler. The technique exploits differences in electron affinities (EA) within elemental or molecular isobaric systems neutralizing anions with EAs smaller than the photon energy. Alternatively, these differences in EA can also facilitate anion separation via chemical reactions with the buffer gas.
We present first results with this approach on AMS-detection of 182Hf. With He +O2 mixtures as buffer gas in the RFQ, suppression of 182WF5− vs 180HfF 5− by >105 has been demonstrated. Mass analysis of the ejected anion beam identified the formation of oxyfluorides as an important reaction channel. The overall Hf-detection efficiency at VERA presently is 1.4% and the W-corrected blank value is 182Hf/180Hf = (3.4 ± 2.1)×10−14. In addition, a survey of different sample materials for highest negative ion yields of HfF 5− with Cs-sputtering has been conducted.
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18
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Koll D, Faestermann T, Korschinek G, Wallner A. Origin of Recent Interstellar 60Fe on Earth. EPJ WEB OF CONFERENCES 2020. [DOI: 10.1051/epjconf/202023202001] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
Over the last 20 years, evidence for a 2 Myr old supernova 60Fe influx onto Earth was provided by several authors. For the first time, independent investigations of samples from two different geological archives yielded conclusive data for a further, much younger 60Fe influx onto Earth. The origin of this influx is currently unclear because of the limited data available, the lack of consistent astrophysical models and a gap in the data between 50 kyr and 1 Myr. Possible astrophysical scenarios will be discussed with respect to the different influx patterns from different sources and a measurement to close the gap will be proposed.
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19
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Stuchbery AE. The Heavy Ion Accelerator Facility: Research Achievements and Aspirations. EPJ WEB OF CONFERENCES 2020. [DOI: 10.1051/epjconf/202023201001] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
An overview of Australia’s Heavy Ion Accelerator Facility (HIAF) is presented, including a survey of the accelerator infrastructure and its capabilities, as well as the beam-line instrumentation. Some recent research achievements are highlighted. Accelerator upgrades and instrumentation developments in progress are described, along with some aspirations for the longer-term development of the Facility and its associated research programs.
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20
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Kirsebom OS, Jones S, Strömberg DF, Martínez-Pinedo G, Langanke K, Röpke FK, Brown BA, Eronen T, Fynbo HOU, Hukkanen M, Idini A, Jokinen A, Kankainen A, Kostensalo J, Moore I, Möller H, Ohlmann ST, Penttilä H, Riisager K, Rinta-Antila S, Srivastava PC, Suhonen J, Trzaska WH, Äystö J. Discovery of an Exceptionally Strong β-Decay Transition of ^{20}F and Implications for the Fate of Intermediate-Mass Stars. PHYSICAL REVIEW LETTERS 2019; 123:262701. [PMID: 31951442 DOI: 10.1103/physrevlett.123.262701] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/22/2019] [Revised: 08/15/2019] [Indexed: 06/10/2023]
Abstract
A significant fraction of stars between 7 and 11 solar masses are thought to become supernovae, but the explosion mechanism is unclear. The answer depends critically on the rate of electron capture on ^{20}Ne in the degenerate oxygen-neon stellar core. However, because of the unknown strength of the transition between the ground states of ^{20}Ne and ^{20}F, it has not previously been possible to fully constrain the rate. By measuring the transition, we establish that its strength is exceptionally large and that it enhances the capture rate by several orders of magnitude. This has a decisive impact on the evolution of the core, increasing the likelihood that the star is (partially) disrupted by a thermonuclear explosion rather than collapsing to form a neutron star. Importantly, our measurement resolves the last remaining nuclear physics uncertainty in the final evolution of degenerate oxygen-neon stellar cores, allowing future studies to address the critical role of convection, which at present is poorly understood.
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Affiliation(s)
- O S Kirsebom
- Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, Denmark
- Institute for Big Data Analytics, Dalhousie University, Halifax, Nova Scotia B3H 4R2, Canada
| | - S Jones
- Computational Physics (XCP) Division, Los Alamos National Laboratory, New Mexico 87545, USA
- Heidelberger Institut für Theoretische Studien, D-69118 Heidelberg, Germany
| | - D F Strömberg
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany
| | - G Martínez-Pinedo
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany
| | - K Langanke
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany
| | - F K Röpke
- Heidelberger Institut für Theoretische Studien, D-69118 Heidelberg, Germany
- Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, D-69120 Heidelberg, Germany
| | - B A Brown
- National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, Michigan 48824, USA
| | - T Eronen
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - H O U Fynbo
- Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, Denmark
| | - M Hukkanen
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - A Idini
- Division of Mathematical Physics, Department of Physics, LTH, Lund University, P.O. Box 118, S-22100 Lund, Sweden
| | - A Jokinen
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - A Kankainen
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - J Kostensalo
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - I Moore
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - H Möller
- Institut für Kernphysik (Theoriezentrum), Technische Universität Darmstadt, D-64289 Darmstadt, Germany
- GSI Helmholtzzentrum für Schwerionenforschung, D-64291 Darmstadt, Germany
| | - S T Ohlmann
- Heidelberger Institut für Theoretische Studien, D-69118 Heidelberg, Germany
- Max Planck Computing and Data Facility, D-85748 Garching, Germany
| | - H Penttilä
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - K Riisager
- Department of Physics and Astronomy, Aarhus University, DK-8000 Aarhus C, Denmark
| | - S Rinta-Antila
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - P C Srivastava
- Department of Physics, Indian Institute of Technology, Roorkee 247667, India
| | - J Suhonen
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - W H Trzaska
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
| | - J Äystö
- Department of Physics, University of Jyväskylä, P.O. Box 35, FI-40014 University of Jyväskylä, Finland
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21
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Koll D, Korschinek G, Faestermann T, Gómez-Guzmán JM, Kipfstuhl S, Merchel S, Welch JM. Interstellar ^{60}Fe in Antarctica. PHYSICAL REVIEW LETTERS 2019; 123:072701. [PMID: 31491090 DOI: 10.1103/physrevlett.123.072701] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/28/2019] [Revised: 05/23/2019] [Indexed: 06/10/2023]
Abstract
Earth is constantly bombarded with extraterrestrial dust containing invaluable information about extraterrestrial processes, such as structure formation by stellar explosions or nucleosynthesis, which could be traced back by long-lived radionuclides. Here, we report the very first detection of a recent ^{60}Fe influx onto Earth by analyzing 500 kg of snow from Antarctica by accelerator mass spectrometry. By the measurement of the cosmogenically produced radionuclide ^{53}Mn, an atomic ratio of ^{60}Fe/^{53}Mn=0.017 was found, significantly above cosmogenic production. After elimination of possible terrestrial sources, such as global fallout, the excess of ^{60}Fe could only be attributed to interstellar ^{60}Fe which might originate from the solar neighborhood.
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Affiliation(s)
- Dominik Koll
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - Gunther Korschinek
- Physik-Department, Technische Universität München, 85748 Garching, Germany
- Excellence Cluster Universe, 85748 Garching, Germany
| | - Thomas Faestermann
- Physik-Department, Technische Universität München, 85748 Garching, Germany
- Excellence Cluster Universe, 85748 Garching, Germany
| | - J M Gómez-Guzmán
- Physik-Department, Technische Universität München, 85748 Garching, Germany
| | - Sepp Kipfstuhl
- Alfred-Wegener-Institut, Helmholtz-Zentrum für Polar- und Meeresforschung, 27568 Bremerhaven, Germany
| | - Silke Merchel
- Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany
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22
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Schumann D, Kivel N, Dressler R. Production and characterization of 60Fe standards for accelerator mass spectrometry. PLoS One 2019; 14:e0219039. [PMID: 31251777 PMCID: PMC6599215 DOI: 10.1371/journal.pone.0219039] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/11/2019] [Accepted: 06/16/2019] [Indexed: 11/19/2022] Open
Abstract
Accelerator Mass Spectrometry (AMS) is one of the most sensitive analysis techniques to measure long-lived radionuclides, reaching detection limits for isotopic ratios down to 10-15-10-16 in special cases. Its application portfolio covers nearly every field of environmental research, considering processes in the atmosphere, biosphere, hydrosphere, cryosphere, lithosphere and the cosmosphere. Normally, AMS measures the content of isotopes in comparison to a validated standard. However, in some cases like for example 60Fe, well characterized standard materials are difficult to produce due to the extreme rareness of the isotope. We report here on the manufacturing of a set of 60Fe standards, obtained by processing irradiated copper from a beam dump of the high-power proton accelerator (HIPA) at the Paul Scherrer Institute (PSI). The isotopic ratios of the standards have been adjusted via a dilution series of a master solution, isotopic content of which has been characterized by Multi Collector-Inductively Coupled Plasma-Mass Spectrometry (MC-ICP-MS). In total, we produced three samples with isotopic ratios of 1.037(6)·10-8, 1.125(7)·10-10 and 1.234 (7)·10-12, respectively. The latter had already been applied in three pioneering AMS studies investigating the remaining signal of injected matter of nearby super novae explosions in sediment archives.
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Affiliation(s)
- Dorothea Schumann
- Paul Scherrer Institute Villigen, Department for Nuclear Energy and Safety, Villigen PSI, Switzerland
- * E-mail:
| | - Niko Kivel
- Paul Scherrer Institute Villigen, Division Large Research Facilities, Villigen PSI, Switzerland
| | - Rugard Dressler
- Paul Scherrer Institute Villigen, Department for Nuclear Energy and Safety, Villigen PSI, Switzerland
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Melott AL, Marinho F, Paulucci L. Hypothesis: Muon Radiation Dose and Marine Megafaunal Extinction at the End-Pliocene Supernova. ASTROBIOLOGY 2019; 19:825-830. [PMID: 30481053 DOI: 10.1089/ast.2018.1902] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Abstract] [Key Words] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
Considerable data and analysis support the detection of one or more supernovae (SNe) at a distance of about 50 pc, ∼2.6 million years ago. This is possibly related to the extinction event around that time and is a member of a series of explosions that formed the Local Bubble in the interstellar medium. We build on previous work, and propagate the muon flux from SN-initiated cosmic rays from the surface to the depths of the ocean. We find that the radiation dose from the muons will exceed the total present surface dose from all sources at depths up to 1 km and will persist for at least the lifetime of marine megafauna. It is reasonable to hypothesize that this increase in radiation load may have contributed to a newly documented marine megafaunal extinction at that time.
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Affiliation(s)
- Adrian L Melott
- 1 Department of Physics and Astronomy, University of Kansas, Lawrence, Kansas
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Feige J, Wallner A, Altmeyer R, Fifield LK, Golser R, Merchel S, Rugel G, Steier P, Tims SG, Winkler SR. Limits on Supernova-Associated ^{60}Fe/^{26}Al Nucleosynthesis Ratios from Accelerator Mass Spectrometry Measurements of Deep-Sea Sediments. PHYSICAL REVIEW LETTERS 2018; 121:221103. [PMID: 30547642 DOI: 10.1103/physrevlett.121.221103] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/25/2018] [Revised: 09/20/2018] [Indexed: 06/09/2023]
Abstract
We searched for the presence of ^{26}Al in deep-sea sediments as a signature of supernova influx. Our data show an exponential dependence of ^{26}Al with the sample age that is fully compatible with radioactive decay of terrigenic ^{26}Al. The same set of samples demonstrated a clear supernova ^{60}Fe signal between 1.7 and 3.2 Myr ago. Combining our ^{26}Al data with the recently reported ^{60}Fe data results in a lower limit of 0.18_{-0.08}^{+0.15} for the local interstellar ^{60}Fe/^{26}Al isotope ratio. It compares to most of the ratios deduced from nucleosynthesis models and is within the range of the observed average galactic ^{60}Fe/^{26}Al flux ratio of (0.15±0.05).
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Affiliation(s)
- Jenny Feige
- Technische Universität Berlin, Department of Astronomy and Astrophysics, Hardenbergstr. 36, 10623 Berlin, Germany
- University of Vienna, Faculty of Physics-Isotope Research and Nuclear Physics, VERA Laboratory, Währingerstr. 17, 1090 Vienna, Austria
| | - Anton Wallner
- The Australian National University, Department of Nuclear Physics, Canberra ACT 2601, Australia
| | - Randolf Altmeyer
- Humboldt-Universität zu Berlin, Department of Mathematics, Unter den Linden 6, 10099 Berlin, Germany
| | - L Keith Fifield
- The Australian National University, Department of Nuclear Physics, Canberra ACT 2601, Australia
| | - Robin Golser
- University of Vienna, Faculty of Physics-Isotope Research and Nuclear Physics, VERA Laboratory, Währingerstr. 17, 1090 Vienna, Austria
| | - Silke Merchel
- Helmholtz-Zentrum Dresden-Rossendorf, Helmholtz Institute Freiberg for Resource Technology, Bautzner Landstr. 400, 01328 Dresden, Germany
| | - Georg Rugel
- Helmholtz-Zentrum Dresden-Rossendorf, Helmholtz Institute Freiberg for Resource Technology, Bautzner Landstr. 400, 01328 Dresden, Germany
| | - Peter Steier
- University of Vienna, Faculty of Physics-Isotope Research and Nuclear Physics, VERA Laboratory, Währingerstr. 17, 1090 Vienna, Austria
| | - Stephen G Tims
- The Australian National University, Department of Nuclear Physics, Canberra ACT 2601, Australia
| | - Stephan R Winkler
- University of Vienna, Faculty of Physics-Isotope Research and Nuclear Physics, VERA Laboratory, Währingerstr. 17, 1090 Vienna, Austria
- iThemba LABS-Laboratory for Accelerator Based Science, Somerset West 7129, South Africa
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Rodrigues D, Negri AE, Balpardo C, Arazi A, Faestermann T, Fernandez Niello JO, Fimiani L, Gómez Guzmán JM, Hain K, Korschinek G, Ludwig P, Marti GV. Assessment of 53Mn deposition on Earth via accelerator mass spectrometry. Appl Radiat Isot 2018; 140:342-346. [PMID: 30138816 DOI: 10.1016/j.apradiso.2018.08.001] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/02/2017] [Revised: 07/30/2018] [Accepted: 08/02/2018] [Indexed: 11/19/2022]
Abstract
The 53Mn flux onto Earth is a quantity relevant for different extraterrestrial and astrophysical questions. It is a proxy for related fluxes, such as supernova-produced material or interplanetary dust particles. In this work, we performed a first attempt to assess the 53Mn flux by measuring the 53Mn/10Be isotopic ratio in a 1400 L sample of molten Antarctic snow by AMS (Accelerator Mass Spectrometry). Using the 10Be production rate in the atmosphere, an upper limit of 5.5 × 103 atoms cm-2 yr-1 was estimated for the deposition of extraterrestrial 53Mn. This result is compatible with one of the two discrepant values existing in the literature.
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Affiliation(s)
- Darío Rodrigues
- Comisión Nacional de Energía Atómica, Av. Gral. Paz 1499, BKNA1650 San Martín, Argentina; CONICET, Av. Rivadavia 1917, C1033AAJ Buenos Aires, Argentina; Departamento de Física, FCEyN, UBA and IFIBA, Conicet, Pabellón 1, Ciudad Universitaria, 1428 Buenos Aires, Argentina.
| | - Agustín E Negri
- CONICET, Av. Rivadavia 1917, C1033AAJ Buenos Aires, Argentina; Instituto de Investigación e Ingeniería Ambiental, Universidad Nacional de San Martín, 25 de Mayo y Francia, San Martín, B1650BWA Buenos Aires, Argentina
| | - Christian Balpardo
- Laboratorio de Metrología de Radioisótopos, Centro Atómico Ezeiza, Comisión Nacional de Energía Atómica, Pbro. González y Aragón 15, Ezeiza, B1802AYA Buenos Aires, Argentina
| | - Andrés Arazi
- Comisión Nacional de Energía Atómica, Av. Gral. Paz 1499, BKNA1650 San Martín, Argentina; CONICET, Av. Rivadavia 1917, C1033AAJ Buenos Aires, Argentina
| | - Thomas Faestermann
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - Jorge O Fernandez Niello
- Comisión Nacional de Energía Atómica, Av. Gral. Paz 1499, BKNA1650 San Martín, Argentina; CONICET, Av. Rivadavia 1917, C1033AAJ Buenos Aires, Argentina; Instituto de Investigación e Ingeniería Ambiental, Universidad Nacional de San Martín, 25 de Mayo y Francia, San Martín, B1650BWA Buenos Aires, Argentina
| | - Leticia Fimiani
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - José Manuel Gómez Guzmán
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - Karin Hain
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - Gunther Korschinek
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - Peter Ludwig
- Technische Universität München, Fakultät für Physik, James-Franck-Straße 1, 85748 Garching, Germany
| | - Guillermo V Marti
- Comisión Nacional de Energía Atómica, Av. Gral. Paz 1499, BKNA1650 San Martín, Argentina
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Thomas BC. Photobiological Effects at Earth's Surface Following a 50 pc Supernova. ASTROBIOLOGY 2018; 18:481-490. [PMID: 29283671 PMCID: PMC5962913 DOI: 10.1089/ast.2017.1730] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/28/2017] [Accepted: 10/26/2017] [Indexed: 05/27/2023]
Abstract
We investigated the potential biological impacts at Earth's surface of stratospheric O3 depletion caused by nearby supernovae known to have occurred about 2.5 and 8 million years ago at about 50 pc distance. New and previously published atmospheric chemistry modeling results were combined with radiative transfer modeling to determine changes in surface-level solar irradiance and biological responses. We find that UVB irradiance is increased by a factor of 1.1 to 2.8, with large variation in latitude, and seasonally at high-latitude regions. Changes in UVA and PAR (visible light) are much smaller. DNA damage (in vitro) is increased by factors similar to UVB, while other biological impacts (erythema, skin cancer, cataracts, marine phytoplankton photosynthesis inhibition, and plant damage) are increased by smaller amounts. We conclude that biological impacts due to increased UV irradiance in this SN case are not mass-extinction level but might be expected to contribute to changes in species abundances; this result fits well with species turnover observed around the Pliocene-Pleistocene boundary. Key Words: UV radiation-Supernovae-Ozone-Radiative transfer. Astrobiology 18, 481-490.
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Affiliation(s)
- Brian C Thomas
- Department of Physics and Astronomy, Washburn University , Topeka, Kansas
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Affiliation(s)
- Günther Dollinger
- Universität der Bundeswehr, München, and Excellence Cluster “Munich-Centre for Advanced Photonics”
| | - Thomas Faestermann
- Physik Department, Technische Universität, München, and Excellence Cluster “Origin and Structure of the Universe”
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A Way Out of the Bubble Trouble?—Upon Reconstructing the Origin of the Local Bubble and Loop I via Radioisotopic Signatures on Earth. GALAXIES 2018. [DOI: 10.3390/galaxies6010026] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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Hammache F. Transfer reactions for nuclear astrophysics. EPJ WEB OF CONFERENCES 2018. [DOI: 10.1051/epjconf/201818401009] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
Direct measurements of cross sections at stellar energies are very challenging - if at all possible. This is essentially due to the very low cross-sections of the reactions of interest (especially when it involves charged particles), and/or to the radioactive nature of many key nuclei. Direct measurements with charged particles are often performed at higher energies and then extrapolated down to stellar energies using R-matrix calculations. However, these extrapolations are delicate because of the possible existence of unobserved low-energy or sub-threshold resonances. In order to bypass the difficulties related to direct measurements, indirect methods such as transfer reactions are used. These experiments are usually performed at higher energies and their conditions are relatively less stringent than in direct measurements. However, these methods rely on theoretical models for which the input parameters may be an important source of systematic uncer-tainties and thus need to be determined carefully. In this manuscript, a short overview on the difficulties related to direct measurements will be given as well as a description of thetransfer reaction method and the theoretical concept behind. Finally, the method will be illustrated through two recent performed studies.
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Schumann D, Dressler R, Maugeri EA, Heinitz S. Isotope production and target preparation for nuclear astrophysics data. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201714603005] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
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Melott AL, Thomas BC, Kachelrieß M, Semikoz DV, Overholt AC. A Supernova at 50 pc: Effects on the Earth's Atmosphere and Biota. THE ASTROPHYSICAL JOURNAL 2017; 840:105. [PMID: 30034016 PMCID: PMC6052450 DOI: 10.3847/1538-4357/aa6c57] [Citation(s) in RCA: 32] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/30/2022]
Abstract
Recent 60Fe results have suggested that the estimated distances of supernovae in the last few million years should be reduced from ∼100 to ∼50 pc. Two events or series of events are suggested, one about 2.7 million years to 1.7 million years ago, and another about 6.5-8.7 million years ago. We ask what effects such supernovae are expected to have on the terrestrial atmosphere and biota. Assuming that the Local Bubble was formed before the event being considered, and that the supernova and the Earth were both inside a weak, disordered magnetic field at that time, TeV-PeV cosmic rays (CRs) at Earth will increase by a factor of a few hundred. Tropospheric ionization will increase proportionately, and the overall muon radiation load on terrestrial organisms will increase by a factor of ∼150. All return to pre-burst levels within 10 kyr. In the case of an ordered magnetic field, effects depend strongly on the field orientation. The upper bound in this case is with a largely coherent field aligned along the line of sight to the supernova, in which case, TeV-PeV CR flux increases are ∼104; in the case of a transverse field they are below current levels. We suggest a substantial increase in the extended effects of supernovae on Earth and in the "lethal distance" estimate; though more work is needed. This paper is an explicit follow-up to Thomas et al. We also provide more detail on the computational procedures used in both works.
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Affiliation(s)
- A L Melott
- Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA
| | - B C Thomas
- Department of Physics and Astronomy, Washburn University, Topeka, KS 66621, USA
| | | | - D V Semikoz
- APC, Universite Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, 119 F-75205 Paris, France
- National Research Nuclear University "MEPHI" (Moscow Engineering Physics Institute), Kashirskoe Highway 31, M4, 115409, Russia
| | - A C Overholt
- Department of Science and Mathematics, MidAmerica Nazarene University, Olathe, KS 66062, USA
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Rehm KE. The Influence of Nuclear Reactions and Nuclear Structure in Astrophysics. EPJ WEB OF CONFERENCES 2017. [DOI: 10.1051/epjconf/201716300048] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Melott AL. A Possible Role for Stochastic Astrophysical Ionizing Radiation Events in the Systematic Disparity between Molecular and Fossil Dates. ASTROBIOLOGY 2017; 17:87-90. [PMID: 28026990 DOI: 10.1089/ast.2016.1527] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/06/2023]
Abstract
Major discrepancies have been noted for some time between fossil ages and molecular divergence dates for a variety of taxa. Recently, systematic trends within avian clades have been uncovered. The trends show that the disparity is much larger for mitochondrial DNA than for nuclear DNA, also that it is larger for crown fossil dates than stem fossil dates. It has been argued that this pattern is largely inconsistent with incompleteness of the fossil record as the principal driver of the disparity. A case is presented that, given the expected mutations from a fluctuating background of astrophysical radiation from such sources as supernovae, the rate of molecular clocks is variable and should increase back to a few million years, before returning to the long-term average rate. This is a possible explanation for the disparity. One test of this hypothesis is to look for an acceleration of molecular clocks at 2 to 2.5 Ma due to one or more moderately nearby supernovae known to have happened at that time. Another is to look for reduced disparity in benthic organisms of the deep ocean. In addition, due to the importance of highly penetrating muon irradiation, the disparity should be magnified for megafauna. Key Words: Extreme events in Earth history-Molecular clock-Radiation physics-Evolution. Astrobiology 17, 87-90.
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Affiliation(s)
- Adrian L Melott
- Department of Physics and Astronomy, University of Kansas , Lawrence, Kansas
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Time-resolved 2-million-year-old supernova activity discovered in Earth's microfossil record. Proc Natl Acad Sci U S A 2016; 113:9232-7. [PMID: 27503888 DOI: 10.1073/pnas.1601040113] [Citation(s) in RCA: 59] [Impact Index Per Article: 7.4] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022] Open
Abstract
Massive stars ([Formula: see text]), which terminate their evolution as core-collapse supernovae, are theoretically predicted to eject [Formula: see text] of the radioisotope (60)Fe (half-life 2.61 Ma). If such an event occurs sufficiently close to our solar system, traces of the supernova debris could be deposited on Earth. Herein, we report a time-resolved (60)Fe signal residing, at least partially, in a biogenic reservoir. Using accelerator mass spectrometry, this signal was found through the direct detection of live (60)Fe atoms contained within secondary iron oxides, among which are magnetofossils, the fossilized chains of magnetite crystals produced by magnetotactic bacteria. The magnetofossils were chemically extracted from two Pacific Ocean sediment drill cores. Our results show that the (60)Fe signal onset occurs around 2.6 Ma to 2.8 Ma, near the lower Pleistocene boundary, terminates around 1.7 Ma, and peaks at about 2.2 Ma.
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Thomas BC, Engler EE, Kachelrieß M, Melott AL, Overholt AC, Semikoz DV. TERRESTRIAL EFFECTS OF NEARBY SUPERNOVAE IN THE EARLY PLEISTOCENE. THE ASTROPHYSICAL JOURNAL. LETTERS 2016; 826:L3. [PMID: 30034771 PMCID: PMC6052446 DOI: 10.3847/2041-8205/826/1/l3] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
Recent results have strongly confirmed that multiple supernovae happened at distances of ∼100 pc, consisting of two main events: one at 1.7-3.2 million years ago, and the other at 6.5-8.7 million years ago. These events are said to be responsible for excavating the Local Bubble in the interstellar medium and depositing 60Fe on Earth and the Moon. Other events are indicated by effects in the local cosmic ray (CR) spectrum. Given this updated and refined picture, we ask whether such supernovae are expected to have had substantial effects on the terrestrial atmosphere and biota. In a first look at the most probable cases, combining photon and CR effects, we find that a supernova at 100 pc can have only a small effect on terrestrial organisms from visible light and that chemical changes such as ozone depletion are weak. However, tropospheric ionization right down to the ground, due to the penetration of ⩾TeV CRs, will increase by nearly an order of magnitude for thousands of years, and irradiation by muons on the ground and in the upper ocean will increase twentyfold, which will approximately triple the overall radiation load on terrestrial organisms. Such irradiation has been linked to possible changes in climate and increased cancer and mutation rates. This may be related to a minor mass extinction around the Pliocene-Pleistocene boundary, and further research on the effects is needed.
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Affiliation(s)
- B C Thomas
- Department of Physics and Astronomy, Washburn University, Topeka, KS 66621, USA
| | - E E Engler
- Department of Physics and Astronomy, Washburn University, Topeka, KS 66621, USA
| | | | - A L Melott
- Department of Physics and Astronomy, University of Kansas, Lawrence, KS 66045, USA
| | - A C Overholt
- Department of Science and Mathematics, MidAmerica Nazarene University, Olathe, KS 66062, USA
| | - D V Semikoz
- APC, Universite Paris Diderot, CNRS/IN2P3, CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cite, F-119 75205 Paris, France
- National Research Nuclear University "MEPHI" (Moscow Engineering Physics Institute), Kashirskoe Highway 31, Moscow, 115409, Russia
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Binns WR, Israel MH, Christian ER, Cummings AC, de Nolfo GA, Lave KA, Leske RA, Mewaldt RA, Stone EC, von Rosenvinge TT, Wiedenbeck ME. Observation of the ⁶⁰Fe nucleosynthesis-clock isotope in galactic cosmic rays. Science 2016; 352:677-80. [PMID: 27103666 DOI: 10.1126/science.aad6004] [Citation(s) in RCA: 80] [Impact Index Per Article: 10.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 11/03/2015] [Accepted: 03/18/2016] [Indexed: 11/02/2022]
Abstract
Iron-60 ((60)Fe) is a radioactive isotope in cosmic rays that serves as a clock to infer an upper limit on the time between nucleosynthesis and acceleration. We have used the ACE-CRIS instrument to collect 3.55 × 10(5) iron nuclei, with energies ~195 to ~500 mega-electron volts per nucleon, of which we identify 15 (60)Fe nuclei. The (60)Fe/(56)Fe source ratio is (7.5 ± 2.9) × 10(-5) The detection of supernova-produced (60)Fe in cosmic rays implies that the time required for acceleration and transport to Earth does not greatly exceed the (60)Fe half-life of 2.6 million years and that the (60)Fe source distance does not greatly exceed the distance cosmic rays can diffuse over this time, ⪍1 kiloparsec. A natural place for (60)Fe origin is in nearby clusters of massive stars.
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Affiliation(s)
- W R Binns
- Washington University, St. Louis, MO 63130, USA.
| | - M H Israel
- Washington University, St. Louis, MO 63130, USA.
| | - E R Christian
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - A C Cummings
- California Institute of Technology, Pasadena, CA 91125, USA
| | - G A de Nolfo
- NASA/Goddard Space Flight Center, Greenbelt, MD 20771, USA
| | - K A Lave
- Washington University, St. Louis, MO 63130, USA
| | - R A Leske
- California Institute of Technology, Pasadena, CA 91125, USA
| | - R A Mewaldt
- California Institute of Technology, Pasadena, CA 91125, USA
| | - E C Stone
- California Institute of Technology, Pasadena, CA 91125, USA
| | | | - M E Wiedenbeck
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA
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