Nuclear Data Center Network Who are we? What can we do for you? Victoria McLane 1,3 Naohiko Otuka 2,3 1 National Nuclear Data Center Brookhaven National Laboratory 2 Nuclear Data Center Japan Atomic Energy Research Institute 3 Nuclear Theory Group Hokkaido University Recent Advances in Astrophysics and Planetary Science, March 1-2, 2005, Sapporo, Japan

Nuclear Data for Astrophysics Nuclear data required for studies of:  Early universe – “Big Bang”,  Stellar physics:  novae, supernovae, Red giants,  Interstellar medium.

Nuclear Data for Astrophysics Codes for modeling these systems require massive amounts of nuclear data Reaction rates. Energy released in nuclear reactions. Structural properties of relevant nuclei.

Nuclear Data for Astrophysics Reaction rate: ‹σ·v› Cross section times ion velocity averaged over Maxwell-Bolzmann distribution of relative ion velocity. Basic data are cross sections and resonance parameters.

Nuclear Data for Astrophysics For many unstable nuclear no cross section data exist! Calculations rely on data from theoretical models. Experimental reaction data are used for refinement of theoretical models.

Nuclear Data for Astrophysics Reaction rates Coughlin and Fowler [1] NACRE [2] T. Raucher and F.-K. Thielemann [3] Goriely et al. Many others

Nuclear Data for Astrophysics Energy released in nuclear reactions Reaction Q-values Audi, Wapstra, Thibault [4]

Nuclear Data for Astrophysics Structural properties of nuclei Decay lifetime, Branching ratios, Separation energies: 1- and 2-particle, Level densities, Resonance parameters.

Nuclear Data for Astrophysics Astrophysical Computer Model Reaction rates Evaluated cross sections Measured cross sections Energy release Mass tables Nuclear structure NSDD Evaluated NSDD Measured NSDD

Nuclear Data for Astrophysics 1. G.R. Coughlin and W.A. Fowler, At. Data & Nucl. Data Tables, 40 (1988) C. Angulo et al., Nucl. Phys. A 656 (1999) T. Raucher and F.-K. Thielemann, At. Data & Nucl. Data Tables 79 (2001) A.H. Wapstra, G. Audi, and C. Thibault, Nucl. Phys. A 729 (2003): part I, page 129; part II, page 337.

Nuclear Data for Astrophysics Stellar nucleosynthesis: Hydrogen burning. Helium burning. Silicon burning. Each involve the need for data on many nuclear reactions.

Alpha-Induced Reactions Reactions involving alpha particles are important in the helium burning stage of stars, novae, and supernovae. They involve light to medium weight nuclei, up to Z=32, and center-of-mass energies up to about 20 MeV.

Alpha-Induced Reactions Buildup of 56 Ni in supernovae depends critically on the ( ,  ) and ( ,p) reactions on  -nuclei, the heaviest stable nuclide of them being 40 Ca. For more massive radioactive  - nuclei, 44 Ti, 48 Cr, 52 Fe, and 56 Ni, we must rely heavily on calculations, since there are few measurements.

Alpha-Induced Reactions A key element in our understanding of  -induced reactions is the  -nucleus potential. Most wide used potentials are McFadden-Satchler [1] and Arthur-Young [2]. Both are global potentials, i.e., expected to perform for a large number of nuclei, but perhaps not suitable for accurate calculations.

Alpha-Induced Reactions NNDC and CNPD, Sarov, along with ORNL, have been involved in a project to compile and evaluate alpha-induced nuclear reaction data. Objective: to derive alpha-nucleus potentials for use in model calculations.

Alpha-Induced Reactions Compilation of data completed. Evaluation of data.  Calculations using the code Empire [3] for both potentials and the code NON-SMOKER [4].

Alpha-Induced Reactions 1 st phase of project is nearing completion [5]. All data will be made available to the community.

Alpha-Induced Reactions 1. L. McFadden and G.R. Satchler, Nucl. Phys. 84,177 (1966). 2. E.D. Arthur and P.G. Young, LA-8626 [ENDF- 304], Los Alamos National Laboratory (1980). 3. M. Herman, p aper presented at Nuclear Data for Science & Technology, Sep. 26 – Oct. 1, 2004, Santa Fe, NM, USA, to be published. 4. T. Rauscher, F.K. Thielemann, At. Data & Nucl. Data Tables 75, 1 (2000).

Alpha-Induced Reactions 5. Papers presented at Nuclear Data for Science & Technology, Sep. 26 – Oct. 1, 2004, Santa Fe, NM, USA, to be published.  S.A.Dunaeva et al., paper 459.  A.G. Zvenigorodski et al., paper 460.

Nuclear Data for Astrophysics To explain occurrence of heavy elements Evolving from existing Fe group: s-process r-process rp-process

Nuclear Data for Astrophysics s-process: slow sequence of neutron absorption (Red giant) Z,A → Z,A+1 → Z,A+2 …… ↓ β - Z+1,A+1 → Z+1,A+2 → …… Knowledge of (n,γ) cross sections 1 to 100 keV.

Nuclear Data for Astrophysics r-process: rapid sequence of neutron absorption (supernova explosion)? Z,A → Z,A+1 → Z,A+2 → Z,A+3…… “neutron drip line” ↓ β - rp-process: rapid sequence of proton absorption Z,A → Z+1,A+1 → Z+2,A+2 → Z+3,A+3…… “proton drip line” ↓ β +

Nuclear Data for Astrophysics These involve very many nuclear reactions. Needed from nuclear data community:  Basic measured data where possible.  Calculations where measurements not feasible.  Evaluations of cross section data.

Who Are We? Nuclear Reaction Data Centers  Coordinated by IAEA NDS.  Cooperate on compilation, exchange, and dissemination of nuclear reaction data.  All data are available on the World Wide Web, free of charge.

Who Are We? Member centers: Provide higher quality service at lower cost by:  avoiding duplication of compilation effort,  adopting common formats and procedures,  sharing programming resources. Provide customer services covering wide range of nuclear data.

Who Are We? More than 50 years experience in nuclear data! 1952: BNL Neutron Cross Section Compilation Group  1 st edition of BNL-325 published in : Sigma Center founded in U.S. at BNL.  SCISRS: 1 st computerized database of experimental nuclear reaction data established in 1964.

Who Are We? 1966: “4-Center Network” created.  Coordinated compilation of neutron reaction data on an international scale.  EXFOR adopted as official exchange format of “4-Center” Network. 1975: Charged-Particle and Photonuclear Data Center Network formed.

Who Are We? 1979: Nuclear Reaction Data Center Network created.  Merger of “4-Center” Network and Charged- Particle and Photonuclear Data Network.

Who Are We? Currently, 13 members centers. “Core” centers: provide complete services NNDC: US National Nuclear Data Center NDS: IAEA Nuclear Data Section NEADB: NEA Data Bank.

Who Are We? CHINA China Nuclear Data Center, China Institute of Atomic Energy, Beijing HUNGARY Cyclotron Applications Department, ATOMKI, Debrecen JAPAN Japan Atomic Energy Research Institute, Tokai Japan Charged Particle Reaction Data Group, Hokkaido KOREA Nuclear Data Evaluation Laboratory, Korea Atomic Energy Research Institute, Taejon

Who Are We? RUSSIA Center for Nuclear Data (CJD), Obninsk Center for Atomic & Nuclear Data, Kurchatov Institute, Moscow Center for Photonuclear Experiments Data, Moscow State University Nuclear Physics Data Center Center for Nuclear Physics Data, Russia Federal Nuclear Center – VNIIEF, Sarov UKRAINE Ukrainian Nuclear Data Center, SC Institute for Nuclear Research, Kiev

What Can We Do for You? Core centers provide easy access to:  Neutron, charged-particle, and photonuclear reaction data.  Nuclear structure and decay data.  Both experimental and evaluated.

What Can We Do for You? EXFOR/CSISRS Experimental Nuclear Reaction Data  Data for incident projectiles ≤1 GeV. New:  Data for incident projectiles >1 GeV.  Fundamental particles reactions.

What Can We Do for You? EXFOR/CSISRS References linked to abstracts for several journals. Links to evaluated data. 3 levels of retrieval: Basic, Extended, Expert Complete set of help file (dictionaries)

What Can We Do for You? EXFOR/CSISRS Data output: EXFOR or CFOR formats. Additional output formats will be developed for users as needs arise. Plots.

What Can We Do for You? ENDF Evaluated Nuclear Reaction Data Data output: as ENDF- formatted files, plots:  for multiple libraries;  with experimental data;  user has some control over format.

6 Li(n,t) 4 He experimental cross section data plotted with ENDF/B-VI curve using ZVView.

What Can We Do for You? NUDAT Nuclear Structure and Decay Data Level properties, Decay modes, Radiations. Output: Tables Plots.

What Can We Do for You? Bibliographic Database Nuclear Science References (NSR) Publications in low and intermediate energy nuclear physics (includes nuclear astrophysics). Data may be retrieved by author, nuclide, reaction,particle, subject, and other criteria. Links provided to experimental and evaluated nuclear structure and decay data. Links are provided to abstracts for several journals.

Additional Services National Nuclear Data Center Nuclear Structure and Decay Data Publication of Nuclear Data Sheets. Nuclear Wallet Cards. EMPIRE Code maintenance.

Additional Services Nuclear Energy Agency Data Bank Computer Program Services Collection and distribution of computer programs relevant to nuclear applications. CD-Rom distribution JANIS: evaluated and experimental data

IAEA Nuclear Data Section FENDL library for fusion applications. IAEA Photonuclear Data Library. Reference Input Parameter Library (RIPL) for theoretical calculations of nuclear reaction cross sections. Atomic and Molecular Data Evaluation and dissemination of atomic and molecular data for fusion and other plasma science & technology applications. Additional Services

Core centers US National Nuclear Data Center Brookhaven National Laboratory OECD-NEA Data Bank Issy-les-Moulineaux, France IAEA Nuclear Data Section Vienna, Austria

US National Nuclear Data Center

Japanese Centers Japan Atomic Energy Research Institute Nuclear Data Center, Tokai-mura Japan Charged-Particle Nuclear Reaction Data Group Hokkaido University, Sapporo

Japan Charged-Particle Reaction Group

Nuclear Reaction Data Centers Please contact us and let us know what we can do for you!

Acknowledgements Thank you to:  Michael Smith of Oak Ridge National Laboratory for contributing information on uses of nuclear data in astrophysics.  Goddard Space Flight Center, NASA for supernova clip.