DOCSLIB.ORG

Nuclear Astrophysics and Low Energy Nuclear Physics Part 1: Nuclear Astrophysics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Nuclear Astrophysics and Low Energy Nuclear Physics Part 1: Nuclear Astrophysics BNL-113703-2017-JA White Paper on Nuclear Astrophysics and Low Energy Nuclear Physics Part 1: Nuclear Astrophysics Almudena Arconesa, Dan W. Bardayanb, Timothy C. Beers, Lee A. Bernstein, Jeffrey C. Blackmond, Bronson Messere, B. Alex Browng, Edward F. Browng, Carl R. Brunei, Art E. Champagne, Alessandro Chieffi, Aaron J. Couturem, Pawel Danielewicz, Roland Diehln, Mounib El-Eid, Jutta Escher, Brian D. Fields, Carla Frohlich, Falk Herwig, William Raphael Hix, Christian Iliadis, William G. Lynch, Gail C. McLaughlin, Bradley S. Meyer, Anthony Mezzacappa, Filomena Nunes, Brian W. O'Shea, Madappa Prakash, Boris Pritychenko, Sanjay Reddy, Ernst Rehm, Grigory Rogachev, Robert E. Rutledge, Hendrik Schatz, Michael S. Smith, Ingrid H. Stairs, Andrew W. Steiner, Tod E. Strohmayer, Frank X. Timmes, Dean M. Townsley, Michael Wiescher, Remco G. T. Zegers, Michael Zingale Submitted to Progress in Particle and Nuclear Physics March 21, 2017 National Nuclear Data Center Brookhaven National Laboratory U.S. Department of Energy Office of Science, Office of Nuclear Physics Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No. DE-SC0012704 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof or its contractors or subcontractors. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof. White Paper on Nuclear Astrophysics and Low Energy Nuclear Physics Part 1: Nuclear Astrophysics Almudena Arconesa,ag, Dan W. Bardayanb,ag, Timothy C. Beersb,ag, Lee A. Bernsteinc, Jeffrey C. Blackmond,ag, Bronson Messere,f, B. Alex Browng,h,ag, Edward F. Browng,h,ag, Carl R. Brunei,ag, Art E. Champagnej,k, Alessandro Chieffil, Aaron J. Couturem,ag, Pawel Danielewiczg,h, Roland Diehln,o,ag, Mounib El-Eidp, Jutta Escherc, Brian D. Fieldsq,ag, Carla Fr¨ohlichr,ag, Falk Herwigs,ag, William Raphael Hixf,1, Christian Iliadisj,k, William G. Lynchg,h,ag, Gail C. McLaughlinr,ag, Bradley S. Meyert, Anthony Mezzacappau,v, Filomena Nunesg,h,ag, Brian W. O'Sheah,ag, Madappa Prakashi,ag, Boris Pritychenkow, Sanjay Reddyx,ag, Ernst Rehmy,ag, Grigory Rogachevz, Robert E. Rutledgeaa,ag, Hendrik Schatzg,h,ag, Michael S. Smithf, Ingrid H. Stairsab, Andrew W. Steineru,ag, Tod E. Strohmayerac, Frank X. Timmesad,ag, Dean M. Townsleyae, Michael Wiescherb,ag, Remco G. T. Zegersg,h,ag, Michael Zingaleaf,ag aGSI Helmholtzzentrum f¨urSchwerionenforschung GmbH, D-64291 Darmstadt, Germany bDepartment of Physics and JINA Center for the Evolution of the Elements, University of Notre Dame, Notre Dame, IN 46556, USA cLawrence Livermore National Laboratory, Livermore, California 94551, USA dDepartment of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803, USA eNational Center for Computational Sciences, Oak Ridge National Laboratory Oak Ridge TN 37831-6008 USA fPhysics Division, Oak Ridge National Laboratory, Oak Ridge TN 37831-6354 USA gNational Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824 USA hDept. of Physics and Astronomy, Michigan State University, East Lansing, MI 48824 USA iDepartment of Physics and Astronomy, Ohio University, Athens, OH 45701, USA jUniversity of North Carolina at Chapel Hill, Chapel Hill, NC 27599-3255, USA kTriangle Universities Nuclear Laboratory, Durham, North Carolina 27708-0308, USA lINAF-IAPS, Via del Fosso del Cavaliere, 100, 00133 Roma, Italy mLos Alamos National Laboratory, Los Alamos, New Mexico 87545, USA nMax Planck Institut f¨urextraterrestrische Physik, D-85748 Garching, Germany oExcellence Cluster Universe, D-85748 Garching, Germany pDepartment of Physics, American University of Beirut, Bliss St. 11-0236, 1107 2020 Beirut, Lebanon qDepartment of Astronomy, University of Illinois, Urbana, IL 61801, USA rDepartment of Physics, North Carolina State University, Raleigh, NC 27695-8202, USA sDepartment of Physics and Astronomy, University of Victoria, Victoria BC, Canada tDepartment of Physics and Astronomy, Clemson University, Clemson, SC, 29634-0978, USA uDepartment of Physics and Astronomy, University of Tennessee, Knoxville, TN 37996-1200 USA vJoint Institute for Computational Sciences, Oak Ridge National Laboratory Oak Ridge TN 37831-6173 USA wNational Nuclear Data Center, Brookhaven National Laboratory, Upton, NY 11973-5000, USA xInstitute for Nuclear Theory, University of Washington, Seattle, WA 98195 yPhysics Division, Argonne National Laboratory, Argonne IL 60439, USA zDepartment of Physics and Astronomy and Cyclotron Institute, Texas A&M University, College Station, TX 77843, USA aaDepartment of Physics, McGill University, 3600 rue University, Montreal, QC, Canada, H3A-2T8 abDept. of Physics and Astronomy, Univ. of British Columbia, Vancouver, BC V6T 1Z1, Canada acX-ray Astrophysics Laboratory, Astrophysics Science Division, NASA/GSFC, Greenbelt, MD 20771 adSchool of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1504, USA aeDepartment of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL, 35487-0324, USA afDepartment of Physics & Astronomy, Stony Brook University, Stony Brook, NY 11794-3800, USA agJoint Institute for Nuclear Astrophysics Center for the Evolution of the Elements, multi-institutional 1 Contents 1 Executive Summary Nuclear Astrophysics 5 2 Scientific Challenges in Nuclear Astrophysics 8 2.1 What is the Origin of the Elements? . 8 2.1.1 Origin of the Elements - Introduction for non experts . 8 2.1.2 Origin of the Elements - Current open questions . 10 2.1.3 Origin of the Elements - Context . 10 2.1.4 Origin of the Elements - Strategic Thrust 1: The Nuclear Physics of Element Synthesis and Model Validation . 12 2.1.5 Origin of the Elements - Strategic Thrust 2: Advancing models of individual nucleosynthesis processes . 14 2.1.6 Origin of the Elements - Strategic Thrust 3: Nucleosynthesis Yield Grids . 18 2.1.7 Origin of the Elements - Strategic Thrust 4: Observations of Ele- ment Production Signatures . 19 2.1.8 Origin of the Elements - Impact on other areas in nuclear astrophysics 20 2.2 How do stars work? . 20 2.2.1 Stars - Introduction for non experts . 20 2.2.2 Stars - Current open questions . 21 2.2.3 Stars - Context . 21 2.2.4 Stars - Strategic Thrust 1: Constraining the rates of nuclear reac- tions in stars . 23 2.2.5 Stars - Strategic Thrust 2: Fundamental Advances in Stellar Models 23 2.2.6 Stars - Strategic Thrust 3: Nucleosynthesis as validation tool . 26 2.2.7 Stars - Strategic Thrust 4: Solar Neutrinos . 27 2.2.8 Stars - Impact on other areas in nuclear astrophysics . 28 2.3 How do Core-Collapse Supernovae and Long Gamma Ray Bursts Explode? 29 2.3.1 CCSNe - Introduction for non experts . 29 2.3.2 CCSNe - Current open questions . 29 2.3.3 CCSNe - Context . 30 2.3.4 CCSNe - Strategic Thrust 1: Towards adequate 3D Models . 30 2.3.5 CCSNe - Strategic Thrust 2: Improved Nuclear Physics . 32 2.3.6 CCSNe - Strategic Thrust 3: More realistic progenitor models . 32 2.3.7 CCSNe - Strategic Thrust 4: Multi-messenger observations . 33 2.3.8 CCSNe - Impact on other areas in nuclear astrophysics . 35 2.4 Compact Object Binary Mergers and Short GRBs . 36 2.4.1 Compact Mergers - Introduction for non experts . 36 2.4.2 Compact Mergers - Current open questions . 36 2.4.3 Compact Mergers - Context . 37 2.4.4 Compact Mergers - Strategic Thrust 1: Advanced Models . 38 2.4.5 Compact Mergers - Strategic Thrust 2: Multi-messenger observations 38 2.4.6 Compact Mergers - Impact on other areas in nuclear astrophysics . 39 Preprint submitted to Elsevier December 8, 2016 2.5 Explosions of White Dwarfs . 39 2.5.1 White Dwarf Explosions - Introduction for non experts . 39 2.5.2 White Dwarf Explosions - Open questions . 39 2.5.3 White Dwarf Explosions - Context . 41 2.5.4 White Dwarf Explosions - Strategic Thrust1: Advancing the models 42 2.5.5 White Dwarf Explosions - Strategic Thrust2: Multi-wavelength observations . 45 2.5.6 White Dwarf Explosions - Strategic Thrust3: Pinning down the nuclear physics . 46 2.5.7 White Dwarf Explosions - Impact on other areas in nuclear astro- physics . 47 2.6 Neutron Stars . 47 2.6.1 Neutron Stars - Introduction for non experts . 47 2.6.2 Neutron Stars - Current Open Questions . 48 2.6.3 Neutron Stars - Context . 49 2.6.4 Neutron Stars - Strategic Thrust 1: Observations . 53 2.6.5 Neutron Stars - Strategic Thrust 2: Physics of Bursts and Crusts . 54 2.6.6 Neutron Star Strategic Thrust 3: The nuclear matter equation of state . 57 2.6.7 Neutron Stars - Strategic Thrust 4: Comprehensive models of ac- creting neutron stars . 58 2.6.8 Neutron Stars - Impact on core-collpase supernovae, neutron star mergers, and the r-process . 58 2.7 Big Bang Nucleosynthesis . 59 2.7.1 Big Bang - Introduction for non experts . 59 2.7.2 Big Bang - Current open questions . 59 2.7.3 Big Bang - Context . 59 2.7.4 Big Bang - Strategic Thrust 1: Improving BBN models .
Load more

Recommended publications
  • Nuclear Physics
    Nuclear Physics Overview One of the enduring mysteries of the universe is the nature of matter—what are its basic constituents and how do they interact to form the properties we observe? The largest contribution by far to the mass of the visible matter we are familiar with comes from protons and heavier nuclei. The mission of the Nuclear Physics (NP) program is to discover, explore, and understand all forms of nuclear matter. Although the fundamental particles that compose nuclear matter—quarks and gluons—are themselves relatively well understood, exactly how they interact and combine to form the different types of matter observed in the universe today and during its evolution remains largely unknown. Nuclear physicists seek to understand not just the familiar forms of matter we see around us, but also exotic forms such as those that existed in the first moments after the Big Bang and that exist today inside neutron stars, and to understand why matter takes on the specific forms now observed in nature. Nuclear physics addresses three broad, yet tightly interrelated, scientific thrusts: Quantum Chromodynamics (QCD); Nuclei and Nuclear Astrophysics; and Fundamental Symmetries: . QCD seeks to develop a complete understanding of how the fundamental particles that compose nuclear matter, the quarks and gluons, assemble themselves into composite nuclear particles such as protons and neutrons, how nuclear forces arise between these composite particles that lead to nuclei, and how novel forms of bulk, strongly interacting matter behave, such as the quark-gluon plasma that formed in the early universe. Nuclei and Nuclear Astrophysics seeks to understand how protons and neutrons combine to form atomic nuclei, including some now being observed for the first time, and how these nuclei have arisen during the 13.8 billion years since the birth of the cosmos.
    [Show full text]
  • The R-Process Nucleosynthesis and Related Challenges
    EPJ Web of Conferences 165, 01025 (2017) DOI: 10.1051/epjconf/201716501025 NPA8 2017 The r-process nucleosynthesis and related challenges Stephane Goriely1,, Andreas Bauswein2, Hans-Thomas Janka3, Oliver Just4, and Else Pllumbi3 1Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP 226, 1050 Brussels, Belgium 2Heidelberger Institut fr¨ Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany 3Max-Planck-Institut für Astrophysik, Postfach 1317, 85741 Garching, Germany 4Astrophysical Big Bang Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan Abstract. The rapid neutron-capture process, or r-process, is known to be of fundamental importance for explaining the origin of approximately half of the A > 60 stable nuclei observed in nature. Recently, special attention has been paid to neutron star (NS) mergers following the confirmation by hydrodynamic simulations that a non-negligible amount of matter can be ejected and by nucleosynthesis calculations combined with the predicted astrophysical event rate that such a site can account for the majority of r-material in our Galaxy. We show here that the combined contribution of both the dynamical (prompt) ejecta expelled during binary NS or NS-black hole (BH) mergers and the neutrino and viscously driven outflows generated during the post-merger remnant evolution of relic BH-torus systems can lead to the production of r-process elements from mass number A > 90 up to actinides. The corresponding abundance distribution is found to reproduce the∼ solar distribution extremely well. It can also account for the elemental distributions observed in low-metallicity stars. However, major uncertainties still affect our under- standing of the composition of the ejected matter.
    [Show full text]
  • Status and Perspectives of the Neutron Time-Of-Flight Facility N TOF at CERN
    Status and perspectives of the neutron time-of-flight facility n_TOF at CERN E. Chiaveri on behalf of the n_TOF Collaboration ([email protected]) Since the start of its operation in 2001, based on an idea of Prof. Carlo Rubbia[1], the neutron time-of-flight facility of CERN, n_TOF, has become one of the most forefront neutron facilities in the world for wide-energy spectrum neutron cross section measurements. Thanks to the combination of excellent neutron energy resolution and high instantaneous neutron flux available in the two experimental areas, the second of which has been constructed in 2014, n_TOF is providing a wealth of new data on neutron-induced reactions of interest for nuclear astrophysics, advanced nuclear technologies and medical applications. The unique features of the facility will continue to be exploited in the future, to perform challenging new measurements addressing the still open issues and long-standing quests in the field of neutron physics. In this document the main characteristics of the n_TOF facility and their relevance for neutron studies in the different areas of research will be outlined, addressing the possible future contribution of n_TOF in the fields of nuclear astrophysics, nuclear technologies and medical applications. In addition, the future perspectives of the facility will be described including the upgrade of the spallation target. 1 Introduction Neutron-induced reactions play a fundamental role for a number of research fields, from the origin of chemical elements in stars, to basic nuclear physics, to applications in advanced nuclear technology for energy, dosimetry, medicine and space science [1]. Thanks to the time-of-flight technique coupled with the characteristics of the CERN n_TOF beam-lines and neutron source, reaction cross-sections can be measured with a very high energy-resolution and in a broad neutron energy range from thermal up to GeV.
    [Show full text]
  • White Paper on Nuclear Astrophysics and Low Energy Nuclear Physics
    WHITE PAPER ON NUCLEAR ASTROPHYSICS AND LOW ENERGY NUCLEAR PHYSICS PART 1: NUCLEAR ASTROPHYSICS FEBRUARY 2016 NUCLEAR ASTROPHYSICS & LOW ENERGY NUCLEAR PHYSICS 1 Edited by: Hendrik Schatz and Michael Wiescher Layout and design: Erin O’Donnell, NSCL, Michigan State University Individual sections have been edited by the section conveners: Almudena Arcones, Dan Bardayan, Lee Bernstein, Jeffrey Blackmon, Edward Brown, Carl Brune, Art Champagne, Alessandro Chieffi, Aaron Couture, Roland Diehl, Jutta Escher, Brian Fields, Carla Froehlich, Falk Herwig, Raphael Hix, Christian Iliadis, Bill Lynch, Gail McLaughlin, Bronson Messer, Bradley Meyer, Filomena Nunes, Brian O'Shea, Madappa Prakash, Boris Pritychenko, Sanjay Reddy, Ernst Rehm, Grisha Rogachev, Bob Ruthledge, Michael Smith, Andrew Steiner, Tod Strohmayer, Frank Timmes, Remco Zegers, Mike Zingale NUCLEAR ASTROPHYSICS & LOW ENERGY NUCLEAR PHYSICS 2 ABSTRACT This white paper informs the nuclear astrophysics community and funding agencies about the scientific directions and priorities of the field and provides input from this community for the 2015 Nuclear Science Long Range Plan. It summarizes the outcome of the nuclear astrophysics town meeting that was held on August 21-23, 2014 in College Station at the campus of Texas A&M University in preparation of the NSAC Nuclear Science Long Range Plan. It also reflects the outcome of an earlier town meeting of the nuclear astrophysics community organized by the Joint Institute for Nuclear Astrophysics (JINA) on October 9- 10, 2012 Detroit, Michigan, with the purpose of developing a vision for nuclear astrophysics in light of the recent NRC decadal surveys in nuclear physics (NP2010) and astronomy (ASTRO2010). The white paper is furthermore informed by the town meeting of the Association of Research at University Nuclear Accelerators (ARUNA) that took place at the University of Notre Dame on June 12-13, 2014.
    [Show full text]
  • R-Process: Observations, Theory, Experiment
    r-process: observations, theory, experiment H. Schatz Michigan State University National Superconducting Cyclotron Laboratory Joint Institute for Nuclear Astrophysics 1. Observations: do we need s,r,p-process and LEPP? 2. r-process (and LEPP?) models 3. r-process experiments SNR 0103-72.6 Credit: NASA/CXC/PSU/S.Park et al. Origin of the heavy elements in the solar system s-process: secondary • nuclei can be studied Æ reliable calculations • site identified • understood? Not quite … r-process: primary • most nuclei out of reach • site unknown p-process: secondary (except for νp-process) Æ Look for metal poor`stars (Pagel, Fig 6.8) To learn about the r-process Heavy elements in Metal Poor Halo Stars CS22892-052 (Sneden et al. 2003, Cowan) 2 1 + solar r CS 22892-052 ) H / X CS22892-052 ( g o red (K) giant oldl stars - formed before e located in halo Galaxyc was mixed n distance: 4.7 kpc theya preserve local d mass ~0.8 M_sol n pollutionu from individual b [Fe/H]= −3.0 nucleosynthesisa events [Dy/Fe]= +1.7 recall: element number[X/Y]=log(X/Y)-log(X/Y)solar What does it mean: for heavy r-process? For light r-process? • stellar abundances show r-process • process is not universal • process is universal • or second process exists (not visible in this star) Conclusions depend on s-process Look at residuals: Star – solar r Solar – s-process – p-process s-processSimmerer from Simmerer (Cowan et etal.) al. /Lodders (Cowan et al.) s-processTravaglio/Lodders from Travaglio et al. -0.50 -0.50 -1.00 -1.00 -1.50 -1.50 log e log e -2.00 -2.00 -2.50 -2.50 30 40 50 60 70 80 90 30 40 50 60 70 80 90 Element number Element number ÆÆNeedNeed reliable reliable s-process s-process (models (models and and nu nuclearclear data, data, incl.
    [Show full text]
  • Arxiv:1901.01410V3 [Astro-Ph.HE] 1 Feb 2021 Mental Information Is Available, and One Has to Rely Strongly on Theoretical Predictions for Nuclear Properties
    Origin of the heaviest elements: The rapid neutron-capture process John J. Cowan∗ HLD Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK 73019, USA Christopher Snedeny Department of Astronomy, University of Texas, 2515 Speedway, Austin, TX 78712-1205, USA James E. Lawlerz Physics Department, University of Wisconsin-Madison, 1150 University Avenue, Madison, WI 53706-1390, USA Ani Aprahamianx and Michael Wiescher{ Department of Physics and Joint Institute for Nuclear Astrophysics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, USA Karlheinz Langanke∗∗ GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany and Institut f¨urKernphysik (Theoriezentrum), Fachbereich Physik, Technische Universit¨atDarmstadt, Schlossgartenstraße 2, 64298 Darmstadt, Germany Gabriel Mart´ınez-Pinedoyy GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany; Institut f¨urKernphysik (Theoriezentrum), Fachbereich Physik, Technische Universit¨atDarmstadt, Schlossgartenstraße 2, 64298 Darmstadt, Germany; and Helmholtz Forschungsakademie Hessen f¨urFAIR, GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany Friedrich-Karl Thielemannzz Department of Physics, University of Basel, Klingelbergstrasse 82, 4056 Basel, Switzerland and GSI Helmholtzzentrum f¨urSchwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany (Dated: February 2, 2021) The production of about half of the heavy elements found in nature is assigned to a spe- cific astrophysical nucleosynthesis process: the rapid neutron capture process (r-process). Although this idea has been postulated more than six decades ago, the full understand- ing faces two types of uncertainties/open questions: (a) The nucleosynthesis path in the nuclear chart runs close to the neutron-drip line, where presently only limited experi- arXiv:1901.01410v3 [astro-ph.HE] 1 Feb 2021 mental information is available, and one has to rely strongly on theoretical predictions for nuclear properties.
    [Show full text]
  • Highlights and Discoveries from the Chandra X-Ray Observatory1
    Highlights and Discoveries from the Chandra X-ray Observatory1 H Tananbaum1, M C Weisskopf2, W Tucker1, B Wilkes1 and P Edmonds1 1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138. 2 NASA/Marshall Space Flight Center, ZP12, 320 Sparkman Drive, Huntsville, AL 35805. Abstract. Within 40 years of the detection of the first extrasolar X-ray source in 1962, NASA’s Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond X-ray images with 100-200 eV energy resolution for energies in the range 0.08<E<10 keV, locating X-ray sources to high precision, detecting extremely faint sources, and obtaining high resolution spectra of selected cosmic phenomena. The extended Chandra mission provides a long observing baseline with stable and well-calibrated instruments, enabling temporal studies over time-scales from milliseconds to years. In this report we present a selection of highlights that illustrate how observations using Chandra, sometimes alone, but often in conjunction with other telescopes, have deepened, and in some instances revolutionized, our understanding of topics as diverse as protoplanetary nebulae; massive stars; supernova explosions; pulsar wind nebulae; the superfluid interior of neutron stars; accretion flows around black holes; the growth of supermassive black holes and their role in the regulation of star formation and growth of galaxies; impacts of collisions, mergers, and feedback on growth and evolution of groups and clusters of galaxies; and properties of dark matter and dark energy.
    [Show full text]
  • Investigations of Nuclear Decay Half-Lives Relevant to Nuclear Astrophysics
    DE TTK 1949 Investigations of nuclear decay half-lives relevant to nuclear astrophysics PhD Thesis Egyetemi doktori (PhD) ´ertekez´es J´anos Farkas Supervisor / T´emavezet˝o Dr. Zsolt F¨ul¨op University of Debrecen PhD School in Physics Debreceni Egyetem Term´eszettudom´anyi Doktori Tan´acs Fizikai Tudom´anyok Doktori Iskol´aja Debrecen 2011 Prepared at the University of Debrecen PhD School in Physics and the Institute of Nuclear Research of the Hungarian Academy of Sciences (ATOMKI) K´esz¨ult a Debreceni Egyetem Fizikai Tudom´anyok Doktori Iskol´aj´anak magfizikai programja keret´eben a Magyar Tudom´anyos Akad´emia Atommagkutat´o Int´ezet´eben (ATOMKI) Ezen ´ertekez´est a Debreceni Egyetem Term´eszettudom´anyi Doktori Tan´acs Fizikai Tudom´anyok Doktori Iskol´aja magfizika programja keret´eben k´esz´ıtettem a Debreceni Egyetem term´eszettudom´anyi doktori (PhD) fokozat´anak elnyer´ese c´elj´ab´ol. Debrecen, 2011. Farkas J´anos Tan´us´ıtom, hogy Farkas J´anos doktorjel¨olt a 2010/11-es tan´evben a fent megnevezett doktori iskola magfizika programj´anak keret´eben ir´any´ıt´asommal v´egezte munk´aj´at. Az ´ertekez´esben foglalt eredm´e- nyekhez a jel¨olt ¨on´all´oalkot´otev´ekenys´eg´evel meghat´aroz´oan hozz´a- j´arult. Az ´ertekez´es elfogad´as´at javaslom. Debrecen, 2011. Dr. F¨ul¨op Zsolt t´emavezet˝o Investigations of nuclear decay half-lives relevant to nuclear astrophysics Ertekez´es´ a doktori (PhD) fokozat megszerz´ese ´erdek´eben a fizika tudom´any´agban ´Irta: Farkas J´anos, okleveles fizikus ´es programtervez˝omatematikus K´esz¨ult a Debreceni Egyetem Fizikai Tudom´anyok Doktori Iskol´aja magfizika programja keret´eben T´emavezet˝o: Dr.
    [Show full text]
  • Second AGILE Catalogue of Gamma-Ray Sources?
    A&A 627, A13 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834143 & c ESO 2019 Astrophysics Second AGILE catalogue of gamma-ray sources? A. Bulgarelli1, V. Fioretti1, N. Parmiggiani1, F. Verrecchia2,3, C. Pittori2,3, F. Lucarelli2,3, M. Tavani4,5,6,7 , A. Aboudan7,12, M. Cardillo4, A. Giuliani8, P. W. Cattaneo9, A. W. Chen15, G. Piano4, A. Rappoldi9, L. Baroncelli7, A. Argan4, L. A. Antonelli3, I. Donnarumma4,16, F. Gianotti1, P. Giommi16, M. Giusti4,5, F. Longo13,14, A. Pellizzoni10, M. Pilia10, M. Trifoglio1, A. Trois10, S. Vercellone11, and A. Zoli1 1 INAF-OAS Bologna, Via Gobetti 93/3, 40129 Bologna, Italy e-mail: [email protected] 2 ASI Space Science Data Center (SSDC), Via del Politecnico snc, 00133 Roma, Italy 3 INAF-Osservatorio Astronomico di Roma, Via di Frascati 33, 00078 Monte Porzio Catone, Italy 4 INAF-IAPS Roma, Via del Fosso del Cavaliere 100, 00133 Roma, Italy 5 Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy 6 INFN Roma Tor Vergata, Via della Ricerca Scientifica 1, 00133 Roma, Italy 7 Consorzio Interuniversitario Fisica Spaziale (CIFS), Villa Gualino - v.le Settimio Severo 63, 10133 Torino, Italy 8 INAF–IASF Milano, Via E. Bassini 15, 20133 Milano, Italy 9 INFN Pavia, Via Bassi 6, 27100 Pavia, Italy 10 INAF–Osservatorio Astronomico di Cagliari, Via della Scienza 5, 09047 Selargius, CA, Italy 11 INAF–Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, LC, Italy 12 CISAS, University of Padova, Padova, Italy 13 Dipartimento di Fisica, University of Trieste, Via Valerio 2, 34127 Trieste, Italy 14 INFN, sezione di Trieste, Via Valerio 2, 34127 Trieste, Italy 15 School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, Braamfontein stateJohannesburg 2050, South Africa 16 ASI, Via del Politecnico snc, 00133 Roma, Italy Received 27 August 2018 / Accepted 12 March 2019 ABSTRACT Aims.
    [Show full text]
  • Sodium and Potassium Signatures Of
    Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets Apurva Oza, Robert Johnson, Emmanuel Lellouch, Carl Schmidt, Nick Schneider, Chenliang Huang, Diana Gamborino, Andrea Gebek, Aurelien Wyttenbach, Brice-Olivier Demory, et al. To cite this version: Apurva Oza, Robert Johnson, Emmanuel Lellouch, Carl Schmidt, Nick Schneider, et al.. Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets. The Astro- physical Journal, American Astronomical Society, 2019, 885 (2), pp.168. 10.3847/1538-4357/ab40cc. hal-02417964 HAL Id: hal-02417964 https://hal.sorbonne-universite.fr/hal-02417964 Submitted on 18 Dec 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astrophysical Journal, 885:168 (19pp), 2019 November 10 https://doi.org/10.3847/1538-4357/ab40cc © 2019. The American Astronomical Society. Sodium and Potassium Signatures of Volcanic Satellites Orbiting Close-in Gas Giant Exoplanets Apurva V. Oza1 , Robert E. Johnson2,3 , Emmanuel Lellouch4 , Carl Schmidt5 , Nick Schneider6 , Chenliang Huang7 , Diana Gamborino1 , Andrea Gebek1,8 , Aurelien Wyttenbach9 , Brice-Olivier Demory10 , Christoph Mordasini1 , Prabal Saxena11, David Dubois12 , Arielle Moullet12, and Nicolas Thomas1 1 Physikalisches Institut, Universität Bern, Bern, Switzerland; [email protected] 2 Engineering Physics, University of Virginia, Charlottesville, VA 22903, USA 3 Physics, New York University, 4 Washington Place, New York, NY 10003, USA 4 LESIA–Observatoire de Paris, CNRS, UPMC Univ.
    [Show full text]
  • Low-Energy Nuclear Physics Part 2: Low-Energy Nuclear Physics
    BNL-113453-2017-JA White paper on nuclear astrophysics and low-energy nuclear physics Part 2: Low-energy nuclear physics Mark A. Riley, Charlotte Elster, Joe Carlson, Michael P. Carpenter, Richard Casten, Paul Fallon, Alexandra Gade, Carl Gross, Gaute Hagen, Anna C. Hayes, Douglas W. Higinbotham, Calvin R. Howell, Charles J. Horowitz, Kate L. Jones, Filip G. Kondev, Suzanne Lapi, Augusto Macchiavelli, Elizabeth A. McCutchen, Joe Natowitz, Witold Nazarewicz, Thomas Papenbrock, Sanjay Reddy, Martin J. Savage, Guy Savard, Bradley M. Sherrill, Lee G. Sobotka, Mark A. Stoyer, M. Betty Tsang, Kai Vetter, Ingo Wiedenhoever, Alan H. Wuosmaa, Sherry Yennello Submitted to Progress in Particle and Nuclear Physics January 13, 2017 National Nuclear Data Center Brookhaven National Laboratory U.S. Department of Energy USDOE Office of Science (SC), Nuclear Physics (NP) (SC-26) Notice: This manuscript has been authored by employees of Brookhaven Science Associates, LLC under Contract No.DE-SC0012704 with the U.S. Department of Energy. The publisher by accepting the manuscript for publication acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency thereof, nor any of their employees, nor any of their contractors, subcontractors, or their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or any third party’s use or the results of such use of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights.
    [Show full text]
  • Annual Report 2019
    Annual Report 2019 IRAM Annual Report 2019 Published by IRAM © 2020 Director of publication Karl-Friedrich Schuster Edited by Cathy Berjaud, Frédéric Gueth With contributions from: Sébastien Blanchet, Edwige Chapillon, Antonio Córdoba, Isabelle Delaunay, Paolo Della Bosca, Eduard Driessen, Bertrand Gautier, Olivier Gentaz, Bastien Lefranc, Santiago Navarro, Roberto Neri, Juan Peñalver, Jérôme Pety, Francesco Pierfederici, Christophe Risacher, Miguel Sánchez Portal, Murielle Serlet, Karl-Friedrich Schuster, Karin Zacher Contents Introduction 4 Highlights of research with the IRAM telescopes 6 30-meter telescope 18 NOEMA 25 Grenoble headquarters 33 Frontend Group 33 Backend Group 37 Superconducting Devices Group 39 Mechanical Group 41 Computer Group 44 Science Software 45 IRAM ARC Node 47 Outreach 47 Personnel & Finance 50 Annexes 54 Telescope schedules 54 Publications 74 Committees 94 4 Introduction This annual report has been edited during complicated times of the corona virus epidemy but this should not distract us from looking back on 2019 which was thoroughly positive for IRAM although at the same time not without new challenges. The year 2019 was rich of important events and scientific results. In fact, NOEMA and powerful new instruments at the 30-meter telescope produce so much high-quality data that we are clearly entering in a new phase of how science is done with the IRAM facilities. At the same time IRAM users have started now to fully embrace the possibilities which are available through large programs and their significant impact on all fields of millimetre wave astronomy. The required infrastructure to treat the very important data flows which are generated through large programs and the ever-increasing performance of the IRAM instruments is now reaching a mature status with the direct optical fibre connections from the observatories to the Granada office and the Grenoble headquarter, the upgraded infrastructure in data storage and computing and finally the very significant advances in data reduction software.
    [Show full text]