Experimental Study of Stellar Reactions at CNS
|
|
- James McCoy
- 5 years ago
- Views:
Transcription
1 Experimental Study of Stellar Reactions at CNS Shigeru KUBONO ( 久保野茂 ) Center for Nuclear Study (CNS) University of Tokyo 1. Nucleosynthesis under Explosive Conditions + CNS-RIKEN AVF-Upgrade Project 2. Direct Study of the Stellar Reactions 3. High Resolution Spectroscopy for Proton Resonances 4. Scope
2 Nucleosynthesis Scenarios pp-chain M Proton X-burst H-burning Hot pp-chain αpprocess rpprocess CNO Cycle s-process Explosive Phenomena α- process Neutron Number 90 Th, 92 U r-process Unstable energies
3 Low Energy RI Beam Production
4 How to Produce RI Beams? Low Energy High Energy ISOL LLN none -based TRIUMF Method ORNL TRIAC, Not much developed! In-flight Notre Dame GSI, MSU Method ANL RIKEN, Beijing Lanzhou, CRIB/CNS GANIL
5 RI Beams by In-Flight Method RIB intensities reaction type 10 4 pps Resonant scattering w/thick target method eg. 22 Mg+p 10 6 pps Rearrangement reactions eg. (α,p), (α,n), (d,p), pps (p,γ), (α,γ),... Total system development; 1. Ion source 2. Accelerator 3. Beam transport 3. Production target 5. Separator
6 CNS Facilities at RIKEN (Under CNS-RIKEN joint venture) RIBF PA Another Facility in RIKEN AVF-BT Campus CRIB Ge Parallel processor system (Theory/Otsuka) CNS-BT AVF /HyperECR CSM AVF Upgrade Project
7 F1: Momentum Dispersive Focal Plane -MomentumSlit - Degrader (thin foil) Degrader Low-Energy in-flight RI Beam F1 RIB ~ pps at F3 ΔE/E ~ % Purity ~ % Q RI Beam 0 5 m Separator CRIB F0 Production target F0: Production Target Gas target with window foils Primary Beam (Low-Energy HI) F2 From RIKEN AVF Cyclotron F2:Achromatic Focal Plane Experimental setup Q Q Q Q B E Wien Filter System (under construction) Wien Filter F3 F3 From AVF
8 Beam Size of 14 O at F3 Wien Filter -> 100 % 14 O of > 10 6 aps Y (mm) ~ 7 x 6 mm 2 Without a degrader Small spot size Higher order correction X (mm) Smaller RI beam spot size!
9 7 Be Beam Production at CRIB 4-MeV 7 Be beam of 6x10 6 aps available! (w/ 0.5 pμa) More beam available! ( > 50 pμa) (Limited by the production target) 7 Be(p,γ) 8 B Reaction: ; Solar model, first generation stars
10 RIB Intensity to Be Reached at CRIB Production target Liq. N 2 cooling target Primary beam intensity SuperC. ECR/Tsukuba U. Upgrade the cyclotron Central region/ Dubna Z 10 8 pps direct measurement of (p,γ) reactions available N 105
11 Direct Study of the Stellar Reactions
12 Nuclear Reactions in the Sun - pp-chain High energy neutrino 8 B 8 Be+e + +ν Proton numbers Neutron numbers
13 8B Structure? Nuclear structure of 8B Solar Model First generation stars Supernovae
14 Elastic Resonant Scattering of p + A(RIB) (Thick target method) Y( E) = I( E) σ( E E+ Δ E/ 2 i E ΔE/ 2 ε( Ei ) ) de i I(E) : Number of beam particles ε(e) : Stopping cross sections
15 Q F0: Production Target Gas target with window foils Primary Beam (Low-Energy HI) 7 Be+p: Setup il) From RIKEN AVF Cyclotron F2:Achromatic Focal Plane Experimental setup 7 Li from AVF cyclotron Q Q Q Q B E F3 RI Beam Wien Filter System (under construction) Primary beam: 7 Li 3+, 61.9 MeV (8.76 MeV/u), ~100 pna. Production target: Hydrogen gas (0.67 mg/cm 2 ), 7 Li(p, n) 7 Be. Secondary beam: 7 Be 4+, 53.8 MeV (@ secondary target), 5 x 10 5 pps, 100% pure.
16 Direct Measurement of the αp-process Reaction
17 High T rp-process (e.g. X-ray burst, SN) 14 O(α,p) 17 F
18 14 O(α,p) Stellar Reaction Both 6.15 and 6.29 important Transition to 17 F*(0.495) important Branching ~ 1/2
19 Astrophysical Reaction Rate 14 O+α 18 Ne * (7.05,(4+)) 17 F * +p New transitions enhance the reaction rate through the MeV level This implies the temperature at cross point of and 7.05-MeV curves reduced. B. Harss et al., PRC65 p (2002)
20 Proton Resonance Search for rp-process Nuclei
21 Early Stage of rp-process Breakout process from NeNa Cycle Production of 22 Na Studied recently.
22 Spectrum of 22 Mg+p Scattering C ounts / 35 k ev b in θlab 0 Ex: (inelastic) E (MeV) cm (elastic) 3.00 (inelastic) Mg(2 + 1 ) + p Expt. Calc. (inelastic) Calc. (elastic) E= x 3.13,3.29,3.00, E (MeV) cm
23 23 Al Level Scheme in 23 Al Present; 22 Mg+p + (7/2 ) + + (7/2,5/2 ) + + (7/2,5/2 ) (3/2 + ) Present 22 Mg+p 3.95(30) 3.26(30) 3.14(30) Shell-model + 7/2 3 3/2-1 5/2+ 3 3/2+ 3 7/2+ 2 1/2+ 2 3/2+ 2-1/ / / Mg( Li, He) 3.699(24) 3.204(21) 2.575(34) 1.773(35) 23 Al( γ, p) ; / ; Mg+p 0 + 5/ (20) (1/2 + ) 0 (5/2 + ) Al
24 Comparisons E x J π expt J π calc l Γ p,(p ) exp Γ p,(p ) cal 0.55 (1/2 + ) 1/ (3/2 + ) 3/ Good tool to study weak-coupled 32(5), 17(3) structure! 3.00 (3/2 +, 5/2 + ) 3/ * (7/2 +, 5/2 + ) 7/ (20) * (7/2 +, 5/2 + ) 5/ (20) * (7/2 + ) 7/ (20) 18 * Their widths are for the decay branches to the 1 st ex. state in 22 Mg. (Ex. energy in MeV and width in kev) 44
25 High-Resolution Spectrograph PA and the Activities
26 High-resolution magnetic spectrograph PA beams A target Focal Plane Det. (X1, X2, Y1,Y2 ΔE, E, TOF)
27 RILAC RIKEN Ring Cyclotron Beam Line for PA 120 MeV α Slit For high resolution mode. E2 PA
28 Elastic scattering at 10 degrees Target : Mylar (t~1.5um) Beam : 4 He 2+ (K.E.~120MeV) E Lab (α) = 120 MeV 12 C (g.s.) 16 O (g.s.) PA angle : 10 degrees PA slit : 0.1 msr Counts 12 C (1 st ) FWHM~ 40 kev Beam transportation : dispersion mode Beam slit width ~ 0.3 mm Relative momentum (ch)
29 (1.8-MeV γ by COMPTEL) New Astronomy by satellites and high resolution telescopes (like by SUBARU) =Observation of Isotopes (not elements) Mapping of 26 Al Gamma Rays Our Galaxy 25 Al(p,γ) 26 Si(3 +?) T 1/2 =0.74 My Galactic plane
30 Scope
31 RIBF Project at RIKEN CRIB 2 Linac 3 Ring Cyclotron 1 Ion Source Present facility 0 50 m 4 frc Highest-energy cyclotron Highest intensity RI beam factory r-process rp-process p-process 5... IRC CNS-SHARAQ Under construction (2006 first beam!) 6 SuperCond.RC (8000 tons)
32 Available RI Beams at RIBF RI Beam Intensity at the RI Beams Factory 100 Primary beam of 1 pµa is assumed. Calculated by Intensity II By Nakamura 82 Proton numbers Z 50 St able Unst able limit of Tachibana Production rate ~ 10-5 /s N Neutron numbers No. of particles per second 100 Nuclear Chart 1993 by Chiharu Tanihata (from Tanihata)
33 Subjects Understanding of the r-process: - Evolution of the Early Universe Cosmo-chronology, Mechanism of Supernovae Pathway Second, third peaks Details around the waiting points The time dependence - Mass (separation energy), Magicity, Half-life, resonances, fission process,..
34 Low-Energy RIB intensity to be reached at CRIB 10 8 pps direct measurement of (p,γ) reactions Beam size < 5 x 5 mm 2 Z Another Intensive facility at RIKEN N available
35 Major part of AVF operation will be available for CRIB (& PA) now on CNS-PAC ; early December, every year Catania, Hanoi, McMaster, Kyushu, RIKEN, Korea, Canberra, days ; 2006 Maybe more time in near future. on Nuclear Astrophysics, Nuclear Physics Material Science,... (or mail to KUBONO@cns.s.u-tokyo.ac.jp)
36 Summary 1. Small machine facility can produce low-energy RIB of 10 8 pps. 2. Direct approach with low-energy RIB for - primordial NS, rp-process, hot pp-chain, early stage of SN, r-process will be possible in near future. 3. The r-process nuclei with very short-half-lives can be investigated with SHARAQ at RIBF.
Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams
Hirschegg 06-1 Experimental Approach to Explosive Hydrogen Burning with Low-Energy RI Beams S. Kubono Center for Nuclear Study (CNS) University of Tokyo 1. Low Energy RI Beam Production 2. Proton Resonance
More informationStellar Evolution: what do we know?
Stellar Evolution: what do we know? New Tools - Astronomy satellite based observatories Hubble Space Telescope Compton Gamma-Ray Observatory Chandra X-Ray Observatory INTEGRAL ground based observatories
More informationHiRA: Science and Design Considerations
HiRA: Science and Design Considerations Scientific Program: Astrophysics: Transfer reactions Resonance spectroscopy Nuclear Structure: Inelastic scattering Transfer reactions Resonance spectroscopy Breakup
More informationThe Ring Branch. Nuclear Reactions at. Mass- and Lifetime Measurements. off Exotic Nuclei. Internal Targets. Electron and p. Experiments: Scattering
stochastic cooling Exotic nuclei from Super-FRS Degrader for fast slowing down The Ring Branch TOF Detector MCPs E anode ion B CR Electron cooler NESR secondary electrons Experiments: Mass- and Lifetime
More informationH/He burning reactions on unstable nuclei for Nuclear Astrophysics
H/He burning reactions on unstable nuclei for Nuclear Astrophysics PJ Woods University of Edinburgh H T O F E E U D N I I N V E B R U S I R T Y H G Explosive H/He burning in Binary Stars Isaac Newton,
More informationPresentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7
Presentation at the 10th RIBLL Collaboration Symposium, Beijing, 2017/1/7 Outline 1. Background 1.1 Decay for proton-rich nuclei 1.2 Astrophysical implications 2. Experiments 2.1 Introduction 2.2 Experimental
More informationStudy on explosive nuclear synthesis with low-energy RI beams at CRIB
Study on explosive nuclear synthesis with low-energy RI beams at CRIB : Hidetoshi Yamaguchi, Seiya Hayakawa, Lei Yang, Hideki Shimizu Nuclear Astrophysics Group, Center for Nuclear Study, Univ. of Tokyo
More informationScientific goal in Nuclear Astrophysics is to explore:
Nuclear Physics in Stars Michael Wiescher University of Notre Dame Joint Institute for Nuclear Astrophysics Scientific goal in Nuclear Astrophysics is to explore: Nuclear Signature in the Cosmos The Nuclear
More informationNuclear Physics using RadioIsotope Beams. T. Kobayashi (Tohoku Univ.)
Nuclear Physics using RadioIsotope Beams T. Kobayashi (Tohoku Univ.) Nucleus: two kinds of Fermions: proton & neutron size ~1fm strong interaction: ~known tightly bound system < several fm < 300 nucleons
More informationMagnetic Separator for light RIB production
Magnetic Separator for light RIB production Vandana Nanal 1,* 1 Deptartment of Nuclear and Atomic Physics, Tata Institute of Fundamental Research, Mumbai - 400005, INDIA. * email:vnanal@gmail.com A magnetic
More informationExperimental Nuclear Astrophysics: Lecture 3. Chris Wrede National Nuclear Physics Summer School June 20 th, 2018
: Lecture 3 Chris Wrede National Nuclear Physics Summer School June 20 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-induced reactions Lecture 3: What I do (indirect
More informationRole of clusters in nuclear astrophysics with Cluster Nucleosynthesis Diagram (CND)
Journal of Physics: Conference Series OPEN ACCESS Role of clusters in nuclear astrophysics with Cluster Nucleosynthesis Diagram (CND) To cite this article: S Kubono et al 2013 J. Phys.: Conf. Ser. 436
More informationWorldwide Direction on Nuclear Science and Application
Worldwide Direction on Nuclear Science and Application Thomas Glasmacher Michigan State University LINAC 16 28 th Linear Accelerator Conference East Lansing, MI, USA 25-30 September 2016 21 st Century
More information2. Acceleration Scheme
2. Acceleration Scheme Accelerators in the RIBF consist of three existing accelerators and three ring cyclotrons under construction. The existing accelerators are the RIKEN Linear Accelerator (RILAC),
More informationEVOLUTION OF SHELL STRUCTURE
EVOLUTION OF SHELL STRUCTURE W A RICHTER ITHEMBA LABS UNIVERSITY OF THE WESTERN CAPE Focus points: 1. Single-particle structure of nuclei 2. Elastic scattering 3. The Interface between Nuclear structure
More informationResearch at FSU, using RESOLUT facility Development of and research with two new detector-systems
Nuclear Astrophysics and Structure Research with Radioactive Beams Research at FSU, using RESOLUT facility Development of and research with two new detector-systems ResoNeut: Low-energy neutron detector-array
More informationUtilization of Intense Rare Isotope Beam at KoRIA
KIAS Workshop Nuclear and Particle Physics in KoRIA and BSI Utilization of Intense Rare Isotope Beam at KoRIA 2011. 9. 17 Yong-Kyun Kim (Hanyang University) On behalf of KoRIA User Community 초신성의 관측 1
More informationnuclear states nuclear stability
nuclear states 1 nuclear stability 2 1 nuclear chart 3 nuclear reactions Important concepts: projectile (A) target (B) residual nuclei (C+D) q-value of a reaction Notations for the reaction B(A,C)D A+B
More informationHow Nature makes gold
How Nature makes gold The role of isotopes for the origin of the elements Karlheinz Langanke GSI Helmholtzzentrum Darmstadt AAAS Symposium, Vancouver, February 20, 2012 Signatures of Nucleosynthesis solar
More informationIntroduction to REX-ISOLDE concept and overview of (future) European projects
Introduction to REX-ISOLDE concept and overview of (future) European projects Thanks to: Y. Blumenfeld, P. Butler, M. Huyse, M. Lindroos, K. Riisager, P. Van Duppen Energetic Radioactive Beam Facilities
More informationReaction rates in the Laboratory
Reaction rates in the Laboratory Example I: 14 N(p,γ) 15 O slowest reaction in the CNO cycle Controls duration of hydrogen burning Determines main sequence turnoff glob. cluster ages stable target can
More informationProspects for Nuclear Astrophysics Experiments in Korea
The 7th BLTP JINR-APCTP Joint Workshop July 14-19, 2013 Prospects for Nuclear Astrophysics Experiments in Korea Kevin Insik Hahn Ewha Womans University Outline Introduction Nuclear Astrophysics in Korea
More informationHydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects. Catherine M. Deibel Louisiana State University
Hydrogen and Helium Burning in Type I X-ray Bursts: Experimental Results and Future Prospects Catherine M. Deibel Louisiana State University 8/29/14 CGS15 August 25 29, 2014 1 Click Type to I X-Ray edit
More informationGANIL / SPIRAL1 / SPIRAL2
Nuclear Structure, Reaction and Dynamics GANIL / SPIRAL1 / SPIRAL2 A huge discovery potential Exotic Nuclei Proton number Z Which force? 3-body, tensor, spin-orbit, Isospin dependence, Continuum coupling
More informationHigh-precision (p,t) reactions to determine reaction rates of explosive stellar processes Matić, Andrija
University of Groningen High-precision (p,t) reactions to determine reaction rates of explosive stellar processes Matić, Andrija IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's
More informationExperimental determination of astrophysical reaction rates with radioactive nuclear beams
Nuclear Physics A 693 (2001) 221 248 www.elsevier.com/locate/npe Experimental determination of astrophysical reaction rates with radioactive nuclear beams Shigeru Kubono Center for Nuclear Study, University
More informationProspects for Nuclear Astrophysics Experiments at KoRIA
September 24-25, 2009 HIM @ APCTP Prospects for Nuclear Astrophysics Experiments at KoRIA Insik Hahn Ewha Womans University Introduction KoRIA Nuclear Astrophysics Experimental Considerations Why radioactive
More informationNuclear Waiting Points and Double Peaked X-Ray Bursts
Nuclear Waiting Points and Double Peaked X-Ray Bursts WITH TODAY'S HONORARY CO-AUTHORSHIP: David Miles Kahl Department of Physics & Astronomy, McMaster University, 1280 Main Street West, ABB 248, Hamilton,
More informationNuclear Astrophysics with DRAGON at ISAC:
Nuclear Astrophysics with DRAGON at ISAC: The 21 Na(p, γ) 22 Mg reaction John M. D Auria for the DRAGON Collaboration Simon Fraser University Burnaby, British Columbia, Canada Abstract The DRAGON facility
More informationSpectroscopy of Single-Particle States in Oxygen Isotopes via (p, 2p) Reaction
Spectroscopy of Single-Particle States in Oxygen Isotopes via (p, 2p) Reaction Shoichiro KAWASE Center for Nuclear Study, the University of Tokyo (p,2p) reaction as a spectroscopic tool Simple reaction
More informationThe LUNA - MV project at the Gran Sasso Laboratory
The LUNA - MV project at the Gran Sasso Laboratory Roberto Menegazzo for the LUNA Collaboration 3ème Andromède Workshop - Orsay, 9 Juillet 2014 outlook LUNA: Why going underground to measure nuclear fusion
More informationResonance scattering and α- transfer reactions for nuclear astrophysics.
Resonance scattering and α- transfer reactions for nuclear astrophysics. Grigory Rogachev Outline Studying resonances using resonance scattering Studying resonances using transfer reactions Resonances
More informationAn Introduction to. Ion-Optics. Series of Five Lectures JINA, University of Notre Dame Sept. 30 Dec. 9, Georg P. Berg
An Introduction to Ion-Optics Series of Five Lectures JINA, University of Notre Dame Sept. 30 Dec. 9, 2005 Georg P. Berg 1 The Lecture Series 1 st Lecture: 9/30/05, 2:00 pm: Definitions, Formalism, Examples
More informationPerspectives on Nuclear Astrophysics
Perspectives on Nuclear Astrophysics and the role of DUSEL Nuclear Astrophysics is a broad field that needs facilities from 1keV-100GeV A low energy accelerator DIANA a DUSEL is a unique instrument for
More informationCapabilities at the National Superconducting Cyclotron Laboratory. Sean Liddick NDNCA workshop, May 26-29, 2015
Capabilities at the National Superconducting Cyclotron Laboratory Sean Liddick NDNCA workshop, May 26-29, 2015 NSCL and FRIB Laboratory NSCL is funded by the U.S. National Science Foundation to operate
More informationNuclear Astrophysics - I
Nuclear Astrophysics - I Carl Brune Ohio University, Athens Ohio Exotic Beam Summer School 2016 July 20, 2016 Astrophysics and Cosmology Observations Underlying Physics Electromagnetic Spectrum: radio,
More informationNSCL and Physics and Astronomy Department, Michigan State University Joint Institute for Nuclear Astrophysics
National Superconducting Cyclotron Laboratory An overview Ana D. Becerril NSCL and Physics and Astronomy Department, Michigan State University Joint Institute for Nuclear Astrophysics University of North
More informationThe Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae
The Origin of the Elements between Iron and the Actinides Probes for Red Giants and Supernovae I Outline of scenarios for neutron capture nucleosynthesis (Red Giants, Supernovae) and implications for laboratory
More informationThe Super-FRS Project at GSI
2 m A G A T A The Super-FRS Project at GSI FRS facility The concept of the new facility The Super-FRS and its branches Summary Martin Winkler for the Super-FRS working group CERN, 3.1.22 Energy Buncher
More informationNuclear Reactions Part III Grigory Rogachev
THE FLORIDA STATE UNIVERSITY National Superconducting Cyclotron Facility Nuclear Reactions Part III Grigory Rogachev Outline Introduction. Resonances in atomic nuclei Role of resonances in era of exotic
More informationDepartment of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA
Spin assignments of 22 Mg states through a 24 Mg(p,t) 22 Mg measurement, K. L. Jones, B. H. Moazen, S. T. Pittman Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996,
More informationDirect (α,p) Reaction Measurements with HELIOS and the study of 20 Ne(α,p) 23 Na
Direct (α,p) Reaction Measurements with HELIOS and the study of 20 Ne(α,p) 23 Na Jianping Lai, Daniel Santiago-Gonzalez Catherine M. Deibel Louisiana State University 9/13/16 INPC 2016 1 (α,p) Reactions
More informationNuclear Astrophysics II
Nuclear Astrophysics II Lecture 5 Fri. June 1, 2012 Prof. Shawn Bishop, Office 2013, Ex. 12437 shawn.bishop@ph.tum.de http://www.nucastro.ph.tum.de/ 1 Where to from here? We are now at a crossroads for
More informationRecoil Separators for Nuclear Astrophysics studies Manoel Couder
Recoil Separators for Nuclear Astrophysics studies Manoel Couder Institute for Structure and Nuclear Astrophysics University of Notre Dame Joint Institute for Nuclear Astrophysics Outline Nuclear astrophysics
More informationb delayed g decay measurements to probe thermonuclear astrophysical explosions
b delayed g decay measurements to probe thermonuclear astrophysical explosions Chris Wrede Michigan State University and NSCL for the NSCL E10034, E12028 & E14066 collaborations NIC XIII, Debrecen, Hungary
More informationExplosive Events in the Universe and H-Burning
Explosive Events in the Universe and H-Burning Jordi José Dept. Física i Enginyeria Nuclear, Univ. Politècnica de Catalunya (UPC), & Institut d Estudis Espacials de Catalunya (IEEC), Barcelona Nuclear
More informationTowards the Extremes of the Nuclear Landscape. Walter F. Henning - RIKEN Nishina Center
Towards the Extremes of the Nuclear Landscape Walter F. Henning - RIKEN Nishina Center Super heavies Proton drip line Unknown Territory Neutron drip line Super heavies Proton drip line Neutron drip line
More informationConstraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies
Constraining Astrophysical Reaction Rates with Transfer Reactions at Low and Intermediate Energies Christoph Langer (JINA/NSCL) INT Workshop: Reactions and Structure of Exotic Nuclei March 2015 1 Understanding
More information13 Synthesis of heavier elements. introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1
13 Synthesis of heavier elements introduc)on to Astrophysics, C. Bertulani, Texas A&M-Commerce 1 The triple α Reaction When hydrogen fusion ends, the core of a star collapses and the temperature can reach
More informationNuclear Physics Questions, Directions, Applications
Nuclear Physics Questions, Directions, Applications Science Questions & Goals of Nuclear Physics Implications of Nuclear Physics for other Fields Applications of Nuclear Physics in other Fields The Nuclear
More informationEvolution and nucleosynthesis prior to the AGB phase
Evolution and nucleosynthesis prior to the AGB phase Amanda Karakas Research School of Astronomy & Astrophysics Mount Stromlo Observatory Lecture Outline 1. Introduction to AGB stars, and the evolution
More informationC NS. Direct reactions of Borromean nuclei FM50. S. Shimoura CNS, University of Tokyo
C NS Direct reactions of Borromean nuclei S. Shimoura CNS, University of Tokyo FM50 Introduction 3N force in neutron-rich nuclei U1X IL2/4 B.E. Importance of T=3/2 3N force in the PRC 64 014001 (2001)
More informationProduction and Separation of Radioactive Beams. Mg and 20 Na with MARS
Production and Separation of Radioactive Beams 20 Mg and 20 Na with MARS Gopal Subedi, Colby College REU 2009, Cyclotron Institute, TAMU Advisor: Dr. Robert E. Tribble August 23, 2009 1 Overview Motivation
More informationAstrophysical Nucleosynthesis
R. D. Gehrz ASTRO 2001, Fall Semester 2018 1 RDG The Chemical Evolution of the Universe 2RDG 1 The Stellar Evolution Cycle 3 RDG a v a v X X V = v a + v X 4 RDG reaction rate r n n s cm ax a X r r ( E)
More informationASTRONOMY 220C ADVANCED STAGES OF STELLAR EVOLUTION AND NUCLEOSYNTHESIS. Spring, This is a one quarter course dealing chiefly with:
This is a one quarter course dealing chiefly with: ASTRONOMY 220C ADVANCED STAGES OF STELLAR EVOLUTION AND NUCLEOSYNTHESIS Spring, 2015 http://www.ucolick.org/~woosley a) Nuclear astrophysics and the relevant
More informationWhat Powers the Stars?
What Powers the Stars? In brief, nuclear reactions. But why not chemical burning or gravitational contraction? Bright star Regulus (& Leo dwarf galaxy). Nuclear Energy. Basic Principle: conversion of mass
More informationtwo-proton radioactivity discovery of two-proton radioactivity experimental results with TPC s future studies
two-proton radioactivity discovery of two-proton radioactivity experimental results with TPC s future studies Bertram Blank CEN Bordeaux-Gradignan EPS European Nuclear Physics Conference 2009 Spring meeting
More informationProduction yields of light short lived isotopes at SARAF
Production yields of light short lived isotopes at SARAF Dan Berkovits, SOREQ NRC Michael Hass, The Weizmann Institute With much help from Sergey Vaintraub Talk content: Introduction Production yield calculation
More informationStellar Interior: Physical Processes
Physics Focus on Astrophysics Focus on Astrophysics Stellar Interior: Physical Processes D. Fluri, 29.01.2014 Content 1. Mechanical equilibrium: pressure gravity 2. Fusion: Main sequence stars: hydrogen
More informationFAIR. Reiner Krücken for the NUSTAR collaboration
NUSTAR @ FAIR Reiner Krücken for the NUSTAR collaboration Physik Department E12 Technische Universität München & Maier-Leibnitz-Laboratory for Nuclear and Particle Physics NUSTAR @ FAIR Nuclear Structure
More informationDecay Spectroscopy with EURICA in the region of 100 Sn
Decay Spectroscopy with EURICA in the region of 100 Sn Daniel Lubos for the EURICA RIBF09 collaboration Technische Universität München Jul 09, 2015 @ Science Day of RA G Excellence Cluster Origin and Structure
More informationSpectroscopy of light exotic nuclei using resonance scattering in inverse kinematics.
Spectroscopy of light exotic nuclei using resonance scattering in inverse kinematics. Grigory Rogachev RESOLUT: a new radioactive beam facility at FSU Solenoid 2 Magnetic Spectrograph Magnetic Spectrograph
More informationReview of ISOL-type Radioactive Beam Facilities
Review of ISOL-type Radioactive Beam Facilities, CERN Map of the nuclear landscape Outline The ISOL technique History and Geography Isotope Separation On-Line Existing facilities First generation facilities
More informationFuture RIB facilities
Future RIB facilities (RIB= radioactive ion beam / rare isotope beam) Reiner Krücken Physik Department E12 Technische Universität München Maier-Leibnitz Laboratory of TU München and LMU München for Nuclear-,
More informationRecent results at RIBF
Recent results at RIBF 1. Nuclear structure and astrophysics in-beam gamma & decay spectroscopy 2. New coming programs H. Sakurai RIKEN Nishina Center/Dept of Phys., Univ. of Tokyo RIKEN RI Beam Factory
More informationPlan for the Nuclear Symmetry Energy Measurements at RAON, LAMPS Facility
3 rd International Symposium on Nuclear Symmetry Energy (NuSYM13) NSCL/FRIB, East Lansing, Michigan, U.S.A. 22-26 July, 2013 Plan for the Nuclear Symmetry Energy Measurements at RAON, LAMPS Facility Byungsik
More informationHigh-resolution study of Gamow- Teller transitions in pf-shell nuclei. Tatsuya ADACHI
High-resolution study of Gamow- Teller transitions in pf-shell nuclei Tatsuya ADACHI Type II supernova Electron Capture (EC) & β decay Neutrino induced reaction A Z-1X N+1 daughter EC β A ZX N parent (A,Z)
More informationMeasurements of the 7 Be+n Big-Bang nucleosynthesis reactions at CRIB by the Trojan Horse method
Measurements of the Be+n Big-Bang nucleosynthesis reactions at CRIB by the Trojan Horse method S. Hayakawa 1, K. Abe 1, O. Beliuskina 1, S. M. Cha 2, K. Y. Chae 2, S. Cherubini 3,4, P. Figuera 3,4, Z.
More informationDetector Array for Low Intensity radiation. DALI and DALI2. S.Takeuchi, T.Motobayashi. Heavy Ion Nuclear Physics Laboratory, RIKEN
Detector Array for Low Intensity radiation DALI and DALI2 S.Takeuchi, T.Motobayashi Heavy Ion Nuclear Physics Laboratory, RIKEN H.Murakami, K.Demichi, H.Hasegawa, Y.Togano Department of Physics, Rikkyo
More informationDecay properties of neutron-rich nuclei on the r-process path
Nuclear science frontier explored by ultra-high power lasers, Feb. 03 Osaka Decay properties of neutron-rich nuclei on the r-process path Shunji NISHIMURA ( RIKEN Nishina Center / NAOJ) Nuclear Parameters
More informationDIANA A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY
DIANA D. Leitner for the DIANA collaboration Michigan State University PAC 2011 New York, April 2011 A NEXT GENERATION DEEP UNDERGROUND ACCELERATOR FACILITY Outline of the Talk Why underground? Brief science
More informationReaction measurements on and with radioactive isotopes for nuclear astrophysics
Reaction measurements on and with radioactive isotopes for nuclear astrophysics René Reifarth GSI Darmstadt/University of Frankfurt NUCL Symposium: Radiochemistry at the Facility for Rare Isotope Beams
More informationFrom the Midwest to the World the Joint Institute for Nuclear Astrophysics Hendrik Schatz Michigan State University
From the Midwest to the World the Joint Institute for Nuclear Astrophysics Hendrik Schatz Michigan State University 15 Years of Nuclear Astrophysics with JINA It started all at Notre Dame National and
More informationNuclear Astrophysics
Nuclear Astrophysics III: Nucleosynthesis beyond iron Karlheinz Langanke GSI & TU Darmstadt Tokyo, November 18, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics Tokyo, November 18, 2008
More informationNuclear Astrophysics
Nuclear Astrophysics I. Stellar burning Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics Aarhus, October 6-10, 2008 1 / 32
More informationNuclear astrophysics of the s- and r-process
Nuclear astrophysics of the s- and r-process René Reifarth Goethe University Frankfurt Ecole Joliot Curie School on Neutrons and Nuclei Frejus, France, Sep-28 Oct-3 2014 Nucleosynthesis tales from the
More informationNuclear Physics at RIBF
Nuclear Physics at RIBF 1. Facility Overview 2. Nuclear structure & astrophysics Highlights and on-going programs 3. Toward Island-of-Stability 4. Summary H. Sakurai RIKEN Nishina Center/Dept of Phys.,
More informationJINA. Address open questions by working on the nuclear physics and the astrophysics
JINA goals Astrophysics Nuclear Physics JINA Address open questions by working on the nuclear physics and the astrophysics JINA workshop goals Interesting problems Ready to be addressed Unknowns ready
More informationStudy of Neutron-Proton Correlation & 3N-Force in 12 C
Study of Neutron-Proton Correlation & 3N-Force in C Outline: 1. Interesting physics on np-correlations in C 2. Probe: Two-nucleon knockout reaction Partial cross section and P // measurements 3. Experimental
More informationThe origin of heavy elements in the solar system
The origin of heavy elements in the solar system (Pagel, Fig 6.8) each process contribution is a mix of many events! 1 Heavy elements in Metal Poor Halo Stars recall: [X/Y]=log(X/Y)-log(X/Y) solar CS22892-052
More informationStudying Neutron-Induced Reactions for Basic Science and Societal Applications
Studying Neutron-Induced Reactions for Basic Science and Societal Applications Correlations in Hadronic and Partonic Interactions 2018 A. Couture Yerevan, Armenia 28 September 2018 Operated by Los Alamos
More informationHigh Resolution Spectroscopy in Nuclear Astrophysics. Joachim Görres University of Notre Dame & JINA
High Resolution Spectroscopy in Nuclear Astrophysics Joachim Görres University of Notre Dame & JINA Nuclear Astrophysics Studies at RCNP Osaka Notre Dame Groningen Started in 2002 (Georg @ RCNP) with a
More informationX-RAY BURSTS AND PROTON CAPTURES CLOSE TO THE DRIPLINE. The hydrogen-rich accreted envelopes of neutron stars in binary systems are
1 X-RAY BURSTS AND ROTON CATURES CLOSE TO THE DRILINE T. Rauscher 1, F. Rembges 1, H. Schatz 2, M. Wiescher 3, F.-K. Thielemann 1 The hydrogen-rich accreted envelopes of neutron stars in binary systems
More informationIn the Beginning. After about three minutes the temperature had cooled even further, so that neutrons were able to combine with 1 H to form 2 H;
In the Beginning Obviously, before we can have any geochemistry we need some elements to react with one another. The most commonly held scientific view for the origin of the universe is the "Big Bang"
More informationPrimer: Nuclear reactions in Stellar Burning
Primer: Nuclear reactions in Stellar Burning Michael Wiescher University of Notre Dame The difficulty with low temperature reaction rates CNO reactions in massive main sequence stars He burning reactions
More informationACCELERATOR MASS SPECTROMETRY; from tracing oceans to nuclear astrophysics. Philippe Collon, University of Notre Dame
ACCELERATOR MASS SPECTROMETRY; from tracing oceans to nuclear astrophysics Philippe Collon, University of Notre Dame A short introduction to JINA JINA: Joint Institute for Nuclear Astrophysics Abundance
More informationExperimental Initiatives in Nuclear Astrophysics
Experimental Initiatives in Nuclear Astrophysics Carl Brune Astrophysics: H and He burning, S process Facilities: neutron and gamma beams, underground accelerators, ICF plasmas Joint DNP Town Meetings
More informationO.Tarasov@Euroschool2013.JINR.RU 1 Nuclide discovery project from Michael Thoennessen http://www.nscl.msu.edu/~thoennes/isotopes/ Discovery papers Table of top 1000 (co)authors Table of top 250 first authors
More informationConceptos generales de astrofísica
Tema 14 Conceptos generales de astrofísica Asignatura de Física Nuclear Curso académico 2009/2010 Universidad de Santiago de Compostela 1 1. Nuclear Astrophysic s domain Nuclear Astrophysics is a relatively
More informationSUMMARY. Novae phenomenon see (J.Jose talk) Why is 18 F important? State of knowledge of 18 F(p,a) reaction. What can we learn from the THM study
SUMMARY Novae phenomenon see (J.Jose talk) Why is F important? State of knowledge of F(p,a) reaction What can we learn from the THM study Classical Nova The companion star transfers matter onto the white
More informationPhysics with Exotic Nuclei
Physics with Exotic Nuclei Hans-Jürgen Wollersheim NUclear STructure, Astrophysics and Reaction Outline Projectile Fragmentation A Route to Exotic Nuclei Fragmentation Cross Sections Nuclear Reaction Rates
More informationPhysics opportunities with the AT-TPC. D. Bazin NSCL/MSU at ReA
Physics opportunities with the AT-TPC D. Bazin NSCL/MSU at ReA Reaction studies at ReA Radioactive beams are used in inverse kinematics Target is now the (usually light) probe nucleus Scattered particles
More informationII. 5. Study for NaI(Tl) and Scintillation Fiber with 80 MeV Proton Beam Toward ESPRI Experiment at NIRS-HIMAC, RIKEN-RIBF
CYRIC Annual Report 2005 II. 5. Study for NaI(Tl) and Scintillation Fiber with 80 MeV Proton Beam Toward ESPRI Experiment at NIRS-HIMAC, RIKEN-RIBF Zenihiro J. 1, Matsuda Y. 2, Sakaguchi H. 3, Takeda H.
More informationin2p , version 1-28 Nov 2008
Author manuscript, published in "Japanese French Symposium - New paradigms in Nuclear Physics, Paris : France (28)" DOI : 1.1142/S21831391444 November 23, 28 21:1 WSPC/INSTRUCTION FILE oliveira International
More informationNeutron induced reactions & nuclear cosmo-chronology. chronology. A Mengoni IAEA Vienna/CERN, Geneva
Neutron induced reactions & nuclear cosmo-chronology chronology A Mengoni IAEA Vienna/CERN, Geneva Ages Cosmological way based on the Hubble time definition ( expansion age ) Astronomical way based on
More informationExotic Beam Summer School: Accelerators and Beams
Exotic Beam Summer School: Accelerators and Beams 26 July, 2011 Bradley M. Sherrill FRIB Chief Scientist Brad Sherrill EBSS July 2011, Slide 1 Slid 1! Accelerators are used to produce important isotopes
More informationFigure 2.11 from page 152 of Exploring the Heart of Ma2er
Nuclear Astrophysics The aim of nuclear astrophysics is to understand those nuclear reacbons that shape much of the nature of the visible universe. Nuclear fusion is the engine of stars; it produces the
More informationProduction and decay studies of 261 Rf, 262. Db, 265 Sg, and 266 Bh for superheavy element chemistry at RIKEN GARIS
Production and decay studies of 261 Rf, 262 Db, 265 Sg, and 266 Bh for superheavy element chemistry at RIKEN GARIS RIKEN Nishina Center Hiromitsu Haba for RIKEN SHE Chemistry Collaboration CONTENTS 1.
More informationExperimental Nuclear Astrophysics: Lecture 1. Chris Wrede National Nuclear Physics Summer School June 19 th, 2018
: Lecture 1 Chris Wrede National Nuclear Physics Summer School June 19 th, 2018 Outline Lecture 1: Introduction & charged-particle reactions Lecture 2: Neutron-capture reactions Lecture 3: What I do (indirect
More informationSunday Monday Thursday. Friday
Nuclear Structure III experiment Sunday Monday Thursday Low-lying excited states Collectivity and the single-particle degrees of freedom Collectivity studied in Coulomb excitation Direct reactions to study
More information