Discovery of Scandium, Titanium, Mercury, and Einsteinium Isotopes

Total Page:16

File Type:pdf, Size:1020Kb

Discovery of Scandium, Titanium, Mercury, and Einsteinium Isotopes Discovery of Scandium, Titanium, Mercury, and Einsteinium Isotopes D. Meierfrankenfeld, A. Bury, M. Thoennessen∗ National Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA Abstract Currently, twenty-three scandium, twenty-five titanium, forty mercury and seventeen einsteinium isotopes have been observed and the discovery of these isotopes is discussed here. For each isotope a brief synopsis of the first refereed publication, including the production and identification method, is presented. arXiv:1003.5128v2 [nucl-ex] 8 Sep 2010 ∗Corresponding author. Email address: [email protected] (M. Thoennessen) Preprint submitted to Atomic Data and Nuclear Data Tables October 25, 2018 Contents 1. Introduction . 4 2. Discovery of 39−61Sc.................................................................................... 4 2.1. 39Sc............................................................................................. 5 2.2. 40Sc............................................................................................. 6 2.3. 41Sc............................................................................................. 6 2.4. 42Sc............................................................................................. 6 2.5. 43Sc............................................................................................. 6 2.6. 44Sc............................................................................................. 7 2.7. 45Sc............................................................................................. 7 2.8. 46Sc............................................................................................. 7 2.9. 47Sc............................................................................................. 7 2.10. 48Sc............................................................................................. 8 2.11. 49Sc............................................................................................. 8 2.12. 50Sc............................................................................................. 8 2.13. 51Sc............................................................................................. 8 2.14. 52;53Sc........................................................................................... 9 2.15. 54;55Sc........................................................................................... 9 2.16. 56−58Sc.......................................................................................... 9 2.17. 59−61Sc.......................................................................................... 9 3. Discovery of 39−63Ti.................................................................................... 9 3.1. 39Ti............................................................................................. 11 3.2. 40Ti............................................................................................. 11 3.3. 41Ti............................................................................................. 11 3.4. 42Ti............................................................................................. 11 3.5. 43Ti............................................................................................. 12 3.6. 44Ti............................................................................................. 12 3.7. 45Ti............................................................................................. 12 3.8. 46;47Ti........................................................................................... 12 3.9. 48Ti............................................................................................. 12 3.10. 49;50Ti........................................................................................... 13 3.11. 51Ti............................................................................................. 13 3.12. 52Ti............................................................................................. 13 3.13. 53Ti............................................................................................. 13 3.14. 54;55Ti........................................................................................... 13 3.15. 56Ti............................................................................................. 14 3.16. 57Ti............................................................................................. 14 3.17. 58Ti............................................................................................. 14 3.18. 59−61Ti.......................................................................................... 14 3.19. 62;63Ti........................................................................................... 14 4. Discovery of 171−210Hg.................................................................................. 15 2 4.1. 171Hg............................................................................................ 16 4.2. 172;173Hg......................................................................................... 16 4.3. 174Hg............................................................................................ 16 4.4. 175;176Hg......................................................................................... 16 4.5. 177Hg............................................................................................ 17 4.6. 178Hg............................................................................................ 17 4.7. 179;180Hg......................................................................................... 17 4.8. 181Hg............................................................................................ 17 4.9. 182Hg............................................................................................ 18 4.10. 183;184Hg......................................................................................... 18 4.11. 185−187Hg........................................................................................ 18 4.12. 188Hg............................................................................................ 18 4.13. 189Hg............................................................................................ 18 4.14. 190Hg............................................................................................ 19 4.15. 191Hg............................................................................................ 19 4.16. 192;193Hg......................................................................................... 19 4.17. 194Hg............................................................................................ 19 4.18. 195Hg............................................................................................ 20 4.19. 196Hg............................................................................................ 20 4.20. 197Hg............................................................................................ 20 4.21. 198−201Hg........................................................................................ 20 4.22. 202Hg............................................................................................ 20 4.23. 203Hg............................................................................................ 20 4.24. 204Hg............................................................................................ 21 4.25. 205Hg............................................................................................ 21 4.26. 206Hg............................................................................................ 21 4.27. 207Hg............................................................................................ 21 4.28. 208Hg............................................................................................ 21 4.29. 209Hg............................................................................................ 22 4.30. 210Hg............................................................................................ 22 5. Discovery of the Element Einsteinium . 22 6. Discovery of 241−257Es.................................................................................. 23 6.1. 241Es............................................................................................ 23 6.2. 242Es............................................................................................ 23 6.3. 243;244Es......................................................................................... 25 6.4. 245Es............................................................................................ 25 6.5. 246Es............................................................................................ 25 6.6. 247Es............................................................................................ 25 6.7. 248Es............................................................................................ 26 6.8. 249−252Es ........................................................................................ 26 6.9. 253Es............................................................................................ 26 3 6.10. 254Es............................................................................................ 27 6.11. 255Es............................................................................................ 27 6.12. 256Es............................................................................................ 27 6.13.
Recommended publications
  • Mass Independent Fractionation of Mercury Isotopes As Source Tracers in Sediments
    Available online at www.sciencedirect.com ScienceDirect Procedia Earth and Planetary Science 13 ( 2015 ) 151 – 157 11th Applied Isotope Geochemistry Conference, AIG-11 BRGM Mass Independent Fractionation of Mercury Isotopes as Source Tracers in Sediments Reshmi Dasa,b,* , William Landingb, Michael Bizimisc, Leroy Odomb, Jane Caffreyd aEarth Observatory of Singapore, 50 Nanyang Avenue, Singapore 639798, Singapore bFlorida State University, Tallahassee, Florida 32306, USA cUniversity of South Carolina, Columbia, South Carolina 29208, USA dUniversity of West Florida, Pensacola, Florida 32514, USA Abstract Since the discovery of isotopic fractionation of mercury in nature, mass dependent fractionation (MDF) and mass independent fractionation (MIF) of mercury isotopes are used as a tracer to understand the mercury cycle. MIF is a powerful tool in understanding the Hg transformations and reaction mechanisms. Here we look into the MIF of the two odd isotopes of mercury (199Hg and 201Hg) in sediment samples collected from lakes and springs of Florida, Lake Erie, and Yucatan Peninsula. The '199Hg and '201Hg of the sediments range from + 0.52‰ to -0.48‰. From the isotopic signature we interpret the possible source of Hg in the Yucatan Peninsula carbonate to be Hg(II) from the water column. Hg in the Florida lakes and spring sediments primarily comes from litterfall. Lake Erie appears to have an anthropogenic source. This study suggests that the MIF signature of Hg isotopes can be used to qualitatively determine the primary source(s) of Hg in sediments. © 2015 The Authors. Published by Elsevier B.V. This is an open access article under the CC BY-NC-ND license © 2015 The Authors.
    [Show full text]
  • Mass Fractionation Laws, Mass-Independent Effects, and Isotopic Anomalies Nicolas Dauphas and Edwin A
    EA44CH26-Dauphas ARI 10 June 2016 9:41 ANNUAL REVIEWS Further Click here to view this article's online features: • Download figures as PPT slides • Navigate linked references • Download citations Mass Fractionation Laws, • Explore related articles • Search keywords Mass-Independent Effects, and Isotopic Anomalies Nicolas Dauphas1,∗ and Edwin A. Schauble2 1Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, Chicago, Illinois 60637; email: [email protected] 2Department of Earth and Space Sciences, University of California, Los Angeles, California 90095 Annu. Rev. Earth Planet. Sci. 2016. 44:709–83 Keywords First published online as a Review in Advance on isotopes, fractionation, laws, NFS, nuclear, anomalies, nucleosynthesis, May 18, 2016 meteorites, planets The Annual Review of Earth and Planetary Sciences is online at earth.annualreviews.org Abstract This article’s doi: Isotopic variations usually follow mass-dependent fractionation, meaning 10.1146/annurev-earth-060115-012157 that the relative variations in isotopic ratios scale with the difference in Copyright c 2016 by Annual Reviews. mass of the isotopes involved (e.g., δ17O ≈ 0.5 × δ18O). In detail, how- All rights reserved ever, the mass dependence of isotopic variations is not always the same, ∗ Corresponding author and different natural processes can define distinct slopes in three-isotope diagrams. These variations are subtle, but improvements in analytical capa- Access provided by University of Chicago Libraries on 07/19/16. For personal use only. Annu. Rev. Earth Planet. Sci. 2016.44:709-783. Downloaded from www.annualreviews.org bilities now allow precise measurement of these effects and make it possi- ble to draw inferences about the natural processes that caused them (e.g., reaction kinetics versus equilibrium isotope exchange).
    [Show full text]
  • Mercury Stable Isotopes As Tracers in the Environment: Applications to Aquatic and Natural Gas Systems
    Mercury Stable Isotopes as Tracers in the Environment: Applications to Aquatic and Natural Gas Systems by Spencer J. Washburn A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Earth and Environmental Sciences) in the University of Michigan 2018 Doctoral Committee: Professor Joel D. Blum, Chair Professor G. Allen Burton Associate Professor Rose M. Cory Professor Kyger C. Lohmann Spencer J. Washburn [email protected] ORCID iD: 0000-0002-6176-8297 © Spencer J. Washburn 2018 Acknowledgements First I would like to thank my wife Kalli for her unwavering support, keen assistance, and timely encouragement over the last five years. I would like to extend my sincere gratitude and many thanks to my advisor, Dr. Joel Blum, for his patience, guidance, and encouragement throughout my entire time at the University of Michigan. His mentorship has been an invaluable part of my PhD experience. I would like to thank all of my co-authors, who have been the source of excellent scientific discourse and support. I would also like to thank my dissertation committee members, who have provided guidance throughout this process. I would like to thank Marcus Johnson, who has been a wonderful source of technical advice and laboratory assistance. I would like to thank the other graduate students who have been members of the BEIGL lab group - Patrick Donovan, Sae Yun Kwon, Laura Motta Medina, and Aaron Kurz - for all of the discussions and friendship over the last 5 years. I would also like to thank the other members of the BEIGL lab group during my tenure, particularly Laura Sherman, Jamie Gleason, and Jason Demers.
    [Show full text]
  • Stable Isotope Separation in Calutrons
    Printed ill tho llnitzd Statss ot 4mcm 4vailsble frurii Nations' Technical Information Service U S :3ep?rtmelli uf Commerce 5285 Port 4oyal Cosd Spririizflald Viryinis 22161 NTlS ptwiodes P~III~~Copy ,498, Microfiche P,C1 I his rcpoti \*!is prspxed as an account of >,dSi-k sponsored by a3 agsncy of the United Sraies Governr;,ent. Neither thc !J nited Skiics i<n.~cti $IK~: nor any agency th2reof. no? any of thzir employoes, (ciakc?.Aijy ivarranty, express or irripiled, or assunias any legal liability or responsibility for ihe accuracy. compleienass, or usefulness of any inforriraiton. ;p ius, product, or process disclosed, or represents that its usewould not infr privately o-v?d ilghts Rcferencc herein to ai-y specific commercial product, process, or service by trade nziile, Zi'adei*lark, manufacturer, or otherwise, does not necsssarily constitute or imply its enduisemcat, recorn,n faVOiii-,g by ille United States(;ovc;riiiie!ii 01- any Zgency thereof Th opinions of auiihols cxp:essed here:!: d~ ~iui neccssarily statc or refisc?!host of the United Sta?ezGovernmer:?or any ngcncy therccf. ____ ___________... ..... .____ ORNL/TM-10356 OPERATIONS DIVISION STABLE ISOTOPE SEPARATION IN CALUTRONS: FORTY YEARS OF PRODUCTION AND DISTRIBUTION W. A. Bell J. G. Tracy Date Published: November 1987 Prepared by the OAK RIDGE NATIONAL LABORATORY Oak Ridge, Tennessee 37831 operated by MARTIN MARIETTA ENERGY SYSTEMS, INC. for the U.S. DEPARTMENT OF ENERGY under Contract No. DE-AC05-840R21400 iti CONTENTS Page ACKNOWLEDGMENTS ................................................. iv I. INTRODUCTION .............................................. 1 11. PROGRAM EVOLUTION ......................................... 1 111. RESEARCH AND DEVELOPMENT .................................. 5 IV. CHEMISTRY ................................................. 8 V.
    [Show full text]
  • 197(M)Hg with High Specific Activity for Imaging and Therapy
    Theranostic mercury: 197(m)Hg with high specific activity for imaging and therapy DISSERTATION zur Erlangung des akademischen Grades Doctor rerum naturalium (Dr. rer. nat.) vorgelegt der Fakultät Mathematik und Naturwissenschaften der Technischen Universität Dresden von Master of Science Chao Wang Born on 07. September 1988 in Harbin, PR China Submitted on: 14.09.2018 Date of defense:13.11.2018 Die Dissertation wurde in der Zeit von September 2014 bis September 2018 am Helmholtz-Zentrum Dresden-Rossendorf im Institut für Radiopharmazeutische Krebsforschung angefertigt. Reviewers: Prof. Dr. Jörg Steinbach (TU Dresden, HZDR) Prof. Dr. Gerd Wunderlich (TU Dresden) Table of Contents 1 Introduction and aim of the work .................................................................... 1 1.1 Introduction ........................................................................................................... 1 1.2 Aims of the Thesis ................................................................................................ 6 1.2.1 Major tasks of this work .................................................................................... 6 2 Theoretical background and literature survey .............................................. 9 2.1 Theranostics .......................................................................................................... 9 2.1.1 General ............................................................................................................. 9 2.1.2 Modalities for diagnostic: PET and SPECT ..................................................
    [Show full text]
  • Assessment of International Reference Materials for Isotope-Ratio Analysis (IUPAC Technical Report)1
    DOI 10.1515/pac-2013-1023 Pure Appl. Chem. 2014; 86(3): 425–467 IUPAC Technical Report Willi A. Brand*, Tyler B. Coplen, Jochen Vogl, Martin Rosner and Thomas Prohaska Assessment of international reference materials for isotope-ratio analysis (IUPAC Technical Report)1 Abstract: Since the early 1950s, the number of international measurement standards for anchoring stable isotope delta scales has mushroomed from 3 to more than 30, expanding to more than 25 chemical elements. With the development of new instrumentation, along with new and improved measurement procedures for studying naturally occurring isotopic abundance variations in natural and technical samples, the number of internationally distributed, secondary isotopic reference materials with a specified delta value has blossomed in the last six decades to more than 150 materials. More than half of these isotopic reference materials were produced for isotope-delta measurements of seven elements: H, Li, B, C, N, O, and S. The number of isotopic reference materials for other, heavier elements has grown considerably over the last decade. Nevertheless, even primary international measurement standards for isotope-delta measurements are still needed for some elements, including Mg, Fe, Te, Sb, Mo, and Ge. It is recommended that authors publish the delta values of internationally distributed, secondary isotopic reference materials that were used for anchoring their meas- urement results to the respective primary stable isotope scale. Keywords: delta notation; delta values; geochemistry; inductively coupled plasma (ICP) mass spectrometry; isotopes; IUPAC Inorganic Chemistry Division; mass spectrometry; reference materials. 1Sponsoring body: IUPAC Inorganic Chemistry Division: see more details on p. 458. *Corresponding author: Willi A.
    [Show full text]
  • Isotopic Composition and Fractionation of Mercury in Great
    Environ. Sci. Technol. 2010, 44, 7764–7770 prises more than 90% of the Hg in ambient air (3, 4). It has Isotopic Composition and low solubility in water and consequently can be transported Fractionation of Mercury in Great long distances in the atmosphere without being deposited (2, 4). In contrast, RGM and Hgp are much more reactive and Lakes Precipitation and Ambient Air deposit readily, either close to sources (5) or upon oxidation of Hg0 during atmospheric transport (2, 4). Given that Hg is ,† † a local, regional, and global pollutant, identifying the LYNNE E. GRATZ,* GERALD J. KEELER, transport pathways, chemical transformations, and deposi- JOEL D. BLUM,‡ AND tion mechanisms that Hg undergoes in the atmosphere can LAURA S. SHERMAN‡ be challenging. Air Quality Laboratory, 1415 Washington Heights, SPH I Mercury stable isotope geochemistry is a growing field Tower, and Department of Geological Sciences, used to examine Hg biogeochemical cycling. Mercury has 1100 N. University Ave., University of Michigan, Ann Arbor, Michigan 48109 seven stable isotopes (196, 198, 199, 200, 201, 202, and 204 amu), active redox chemistry, and an ability to form covalent bonds. It also commonly transforms between the solid, Received February 3, 2010. Revised manuscript received aqueous, and gas phases. Mass-dependent fractionation September 8, 2010. Accepted September 9, 2010. (MDF) of Hg has been observed experimentally during microbial reduction (6, 7) and dark abiotic aqueous reduction (8). MDF is also observed in natural materials, including - Atmospheric deposition is a primary pathway by which hydrothermal emissions (9 11) and terrestrial and marine sediments (12, 13). mercury (Hg) enters terrestrial and aquatic ecosystems; Recent studies demonstrate that mass-independent frac- however, the chemical and meteorological processes that Hg tionation (MIF) of Hg isotopes can occur in natural systems.
    [Show full text]
  • Experimental Searches for Rare Alpha and Beta Decays
    Experimental searches for rare alpha and beta decays P. Belli1;2;a, R. Bernabei1;2, F.A. Danevich3, A. Incicchitti4;5, and V.I. Tretyak3 1 Dip. Fisica, Universit`adi Roma \Tor Vergata", I-00133 Rome, Italy 2 INFN sezione Roma \Tor Vergata", I-00133 Rome, Italy 3 Institute for Nuclear Research, 03028 Kyiv, Ukraine 4 Dip. Fisica, Universit`adi Roma \La Sapienza", I-00185 Rome, Italy 5 INFN sezione Roma, I-00185 Rome, Italy Abstract. The current status of the experimental searches for rare alpha and beta decays is reviewed. Several interesting observations of alpha and beta decays, previously unseen due to their large half-lives (1015 − 1020 yr), have been achieved during the last years thanks to the improvements in the experimental techniques and to the underground locations of experiments that allows to suppress backgrounds. In particular, the list includes first observations of alpha decays of 151Eu, 180W (both to the ground state of the daughter nuclei), 190Pt (to excited state of the daughter nucleus), 209Bi (to the ground and excited 209 19 states of the daughter nucleus). The isotope Bi has the longest known half-life of T1=2 ≈ 10 yr relatively 115 115 to alpha decay. The beta decay of In to the first excited state of Sn (Eexc = 497:334 keV), recently observed for the first time, has the Qβ value of only (147 ± 10) eV, which is the lowest Qβ value known to-date. Searches and investigations of other rare alpha and beta decays (48Ca, 50V, 96Zr, 113Cd, 123Te, 178m2Hf, 180mTa and others) are also discussed.
    [Show full text]
  • Uptake, Efflux, and Toxicity of Inorganic and Methyl Mercury in the Endothelial Cells (EA.Hy926)
    www.nature.com/scientificreports OPEN Uptake, efux, and toxicity of inorganic and methyl mercury in the endothelial cells (EA.hy926) Songnian Liu, Martin Tsz-Ki Tsui✉, Elizabeth Lee, Josh Fowler & Zhenquan Jia✉ Cardiovascular disease (CVD) is the major cause of morbidity, mortality, and health care costs in the United States, and possibly around the world. Among the various risk factors of CVD, environmental and dietary exposures to mercury (Hg), a highly toxic metal traditionally regarded as a neurotoxin, has been recently suggested as a potential contributor towards human atherosclerotic development. In this study, we investigated the toxicity, type of cell death, dose-dependent uptake, and efux of inorganic HgII (as HgCl2) and methylmercury or MeHg (as CH3HgCl) in EA.hy926 endothelial cells, as these two forms of Hg are often reported to be present in human blood among the general populations (~20–30% as HgII and ~70–80% as MeHg). Our results showed that HgII is more toxic than MeHg to the endothelial cells, owing to the higher uptake into the cytoplasm and perhaps importantly lower efux of HgII by the cells, thus the “net” accumulation by the endothelial cells is higher for HgII than MeHg when exposed to the same Hg levels in the media. Furthermore, both HgII and MeHg were found to induce apoptotic and necrotic cell death. This study has important implications for the contributions of these two common Hg species to the development of atherosclerosis, an important process leading to CVD. Cardiovascular disease (CVDs) is the leading cause of morbidity, mortality, and health care costs in the United States.
    [Show full text]
  • The Chemical Compositions of the 2 New Hgmn Stars HD 30085 and HD
    Draft version August 15, 2019 A Preprint typeset using L TEX style AASTeX6 v. 1.0 THE CHEMICAL COMPOSITIONS OF THE 2 NEW HGMN STARS HD 30085 AND HD 30963. COMPARISON TO χ LUPI A, ν CAP AND HD 174567 R. Monier1 LESIA, UMR 8109, Observatoire de Paris et Universit´ePierre et Marie Curie Sorbonne Universit´es, place J. Janssen, Meudon, France. E.Griffin2 Dominion Astrophysical Observatory, 5071 West Saanich Road, Victoria, BC, V9E 2E7, Canada M. Gebran3 Department of Physics and Astronomy, Notre Dame University-Louaize, PO Box 72, Zouk Mikael, Lebanon. T. Kılıc¸oglu˘ 4 Department of Astronomy and Space Sciences, Faculty of Science, Ankara University, 06100, Turkey. T.Merle5 Institut d’Astronomie et d’Astrophysique, Universit´eLibre de Bruxelles, CP 226, Boulevard du Triomphe, 1050 Brussels, Belgium F. Royer6 GEPI, Observatoire de Paris, place J. Janssen, Meudon, France. ABSTRACT We report on a detailed abundance study of the fairly bright slow rotators HD 30085 (A0 IV), HD 30963 (B9 III) and HD 174567 (A0 V), hitherto reported as normal stars and the sharp-lined χ Lupi A (B9 IV HgMn). In the spectra of HD 30085, HD 30963, the Hg II line at 3984 A˚ line is conspicuous and numerous lines of silicon, manganese, chromium, titanium, iron, strontium, yttrium and zirconium appear to be strong absorbers. A comparison of the mean spectra of HD 30085 and HD 30963 with a grid of synthetic spectra for selected unblended lines having reliable updated atomic data reveals large overabundances of phosphorus, titanium, chromium, manganese, strontium, yttrium, and zirconium, barium, platinum and mercury and underabundances of helium, magnesium, scandium, arXiv:1908.05023v1 [astro-ph.SR] 14 Aug 2019 nickel.
    [Show full text]
  • C. R. Webster and R. N. Zare, "Photochemical Isotope Separation of Hg-196 by Reaction with Hydrogen Halides
    1302 J. Phys. Chem. 1981, 85, 1302-1305 Photochemical Isotope Separation of Hg-196 by Reaction with Hydrogen Halides Christopher R. Webster and Richard N. Zare” Department of Chemlstry, Stanford Unlverslty, Stanford, California 04305 (Received: November 28, 1980; In Flnal Form: February 11, 198 1) The rarest of the naturally occurring isotopes of mercury, lSHg (0.146% abundance), has been photochemically separated by reaction with hydrogen halides as scavengers of the excited Hg(3P1) atoms. A separation of 2-3 mg/h of enriched calomel product is achieved by using a monoisotopic lamp as an excitation source. The product contains 22 f 8% of the l=He in the feedstock. For the HC1 reaction the enrichment factor is 4.2, for HBr 1.4, while for HI no enrichmeit is found. Introduction Separation Apparatus Mercury occurs naturally as a mixture of seven isotopes Figure 1 shows a diagram of the photochemical sepa- of which the lightest, l%Hg, has an abundance of only ration apparatus, and Figure 2 details the reaction cell and 0.146%. The separation of Hg-196 from natural mercury the mercury lamp which are at the heart of the experiment. has practical application in the preparation, through nu- The flow system is constructed mainly in borosilicate glass, clear reaction, of radioactive Hg-197, a y emitter used for with the reaction cell and the inner jackets made from cerebral blood-flow measurement and brain-scanning with quartz to allow transmission of ultraviolet radiation. scintillation detection techniques.l To date, the highest Calibrated flowmeters (Matheson) allow controlled enrichments and yields of the isotopes of mercury have amounts of the hydrogen halide (HC1, HBr, or HI) gas to resulted from photochemical separation, that is, monoi- be mixed with a fractional amount of l,&butadiene and sotopic 63P1-61S0 excitation at 253.7 nm followed by passed through the reaction cell illuminated by 253.7-nm chemical reaction to form a stable, separable product.2 radiation.
    [Show full text]
  • Discovery of the Mercury Isotopes
    Preprint submitted to ATOMIC DATA AND NUCLEAR DATA TABLES August 1, 2009 Discovery of the Mercury Isotopes D. MEIERFRANKENFELD and M. THOENNESSEN ∗ National Superconducting Cyclotron Laboratory and Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA Forty mercury isotopes have so far been observed; the discovery of these isotopes is discussed. For each isotope a brief summary of the first refereed publication, including the production and identification method, is presented. ∗ Corresponding author. Email address: [email protected] (M. Thoennessen). CONTENTS 1 Introduction . 2 2 Discovery of 171−210Hg ............................................................. 2 3 Summary......................................................................... 10 EXPLANATION OF TABLE . 13 TABLE I. Discovery of Mercury Isotopes . 14 REFERENCES FOR TABLE . 16 1. INTRODUCTION The discovery of the mercury isotopes is discussed as part of the series of the discovery of iso- topes which began with the cerium isotopes in 2009 [1]. The purpose of this series is to document and summarize the discovery of the isotopes. Guidelines for assigning credit for discovery are (1) clear identification, either through decay-curves and relationships to other known isotopes, particle or g-ray spectra, or unique mass and Z-identification, and (2) publication of the discovery in a refereed jour- nal. The authors and year of the first publication, the laboratory where the isotopes were produced as well as the production and identification methods are discussed. When appropriate, references to con- ference proceedings, internal reports, and theses are included. When a discovery includes a half-life measurement the measured value is compared to the currently adopted value taken from the NUBASE evaluation [2] which is based on the ENSDF database [3].
    [Show full text]