Nuclear Astrophysics
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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. -
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. -
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. -
Grant Proposals, 1991-1999
Grant Proposals, 1991-1999 Finding aid prepared by Smithsonian Institution Archives Smithsonian Institution Archives Washington, D.C. Contact us at [email protected] Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Descriptive Entry.............................................................................................................. 1 Names and Subjects ...................................................................................................... 1 Container Listing ............................................................................................................. 2 Grant Proposals https://siarchives.si.edu/collections/siris_arc_251859 Collection Overview Repository: Smithsonian Institution Archives, Washington, D.C., [email protected] Title: Grant Proposals Identifier: Accession 99-171 Date: 1991-1999 Extent: 17 cu. ft. (17 record storage boxes) Creator:: Smithsonian Astrophysical Observatory. Contracts and Procurement Office Language: English Administrative Information Prefered Citation Smithsonian Institution Archives, Accession 99-171, Smithsonian Astrophysical Observatory, Contracts and Procurement Office, Grant Proposals Descriptive Entry This accession consists of records documenting Smithsonian Astrophysical Observatory projects and activities. Materials include proposals, correspondence, progress -
Report of Contributions
Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB). -
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. -
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. -
![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](https://docslib.b-cdn.net/cover/8159/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-508159.webp)
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. -
Massive Amounts of Cold Dust in Small Magellanic Cloud Remnant 1E
Massive Amounts of Cold Dust in Small Magellanic Cloud Supernova Remnant 1E 0102-7219 M. B. Wong1,2, I. De Looze2,3, M. J. Barlow2 Washington University in St. Louis School of Medicine, 660 S. Euclid Ave, St. Louis MO, 63110 Dept. of Physics & Astronomy, University College London, Gower St., London WC1E 6BT, UK Sterrenkundig Observatorium, Ghent University, Krijgslaan 281 - S9, 9000 Gent, Belgium Results Abstract Currently, the primary source of interstellar dust is a subject of debate as models relying on Shown below are the results of dust models for various Mg Silicate grain species. Depending on the evolved asymptotic giant branch stars fail to produce sufficient dust in the appropriate timescale. composition, total dust masses range from 0.001 – 0.01Msun and in each case has a prominent cold However, core collapse supernovae (CCSNe) have a much shorter lifecycle and are a plausible dust component. Though it was performed, carbon grain based fits were poor, as would be expected alternative for dust production in early Universe galaxies. Estimates suggest that each SNR would for an oxygen rich remnant such as 1E 0102, and are not included below. need to generate 0.1-1Msun of interstellar grains if CCSNe are indeed the major sources of dust in high redshift galaxies1,2. Numerous reports exist for warm dust masses several orders of Mg0.7SiO2.7 magnitude below this 0.1-1Msun range, but some recent studies incorporating longer wavelength data show large masses of low temperature dust from remnants such as CasA3 and the Crab4 Nebula. Here, using data from Spitzer Space Telescope’s MIPS instrument with PACS and SPIRE data from Herschel Space Observatory, we detected massive amounts of cold dust in E0102, a 1000 year old Figure 2: Dust mass for the warm oxygen rich remnant at a distance of 62.1kpc in the Small Magellanic Cloud (SMC). -
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. -
16Th HEAD Meeting Session Table of Contents
16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113 -
Nd AAS Meeting Abstracts
nd AAS Meeting Abstracts 101 – Kavli Foundation Lectureship: The Outreach Kepler Mission: Exoplanets and Astrophysics Search for Habitable Worlds 200 – SPD Harvey Prize Lecture: Modeling 301 – Bridging Laboratory and Astrophysics: 102 – Bridging Laboratory and Astrophysics: Solar Eruptions: Where Do We Stand? Planetary Atoms 201 – Astronomy Education & Public 302 – Extrasolar Planets & Tools 103 – Cosmology and Associated Topics Outreach 303 – Outer Limits of the Milky Way III: 104 – University of Arizona Astronomy Club 202 – Bridging Laboratory and Astrophysics: Mapping Galactic Structure in Stars and Dust 105 – WIYN Observatory - Building on the Dust and Ices 304 – Stars, Cool Dwarfs, and Brown Dwarfs Past, Looking to the Future: Groundbreaking 203 – Outer Limits of the Milky Way I: 305 – Recent Advances in Our Understanding Science and Education Overview and Theories of Galactic Structure of Star Formation 106 – SPD Hale Prize Lecture: Twisting and 204 – WIYN Observatory - Building on the 308 – Bridging Laboratory and Astrophysics: Writhing with George Ellery Hale Past, Looking to the Future: Partnerships Nuclear 108 – Astronomy Education: Where Are We 205 – The Atacama Large 309 – Galaxies and AGN II Now and Where Are We Going? Millimeter/submillimeter Array: A New 310 – Young Stellar Objects, Star Formation 109 – Bridging Laboratory and Astrophysics: Window on the Universe and Star Clusters Molecules 208 – Galaxies and AGN I 311 – Curiosity on Mars: The Latest Results 110 – Interstellar Medium, Dust, Etc. 209 – Supernovae and Neutron