FRIB Physics Program Brad Sherrill Facility for Rare

FRIB Physics Program Brad Sherrill Facility for Rare Isotope Beams 26 June 2013

Outline § Development of a comprehensive model of atomic nuclei – How do we understand the structure and stability of atomic nuclei? § Understanding the origin of elements and modeling of extreme astrophysics environments § Use of atomic nuclei to test fundamental symmetries (e. g. in a search for CP violation) § Applied isotope science – new applications of isotopes RHIC Users Meeting June 2013, Slide 2

One of the Challenges – How many elements? Claims for up to Z=118, but much beyond requires theory – application of Density Functional Theory - P. Pyykkö: Phys. Chem. Phys. 13, 161 -168 (2011) “Half of chemistry is undiscovered. ” - Another view – above Z=122 all chemistry is the same due to relativistic effects - For stability of Z>120 see also Jachimowicz, Kowal, Skalski, PRC 83 (2011) RHIC Users Meeting June 2013, Slide 3

One of the Challenges – Origin Elemental Abundances in our Solar System § Stars are mostly made of hydrogen and helium, but each has a fairly unique pattern of other elements Asplund, M. , Grevesse, N. , Sauval, A. J. , Scott, P. : Annu. Rev. Astron. Astrophys. 47, 481 (2009) § The abundance of elements tell us about the history of events prior to the formation of our sun § The plot at the right shows the composition in the visible surface layer of the Sun (photosphere) § How were these elements created prior to the formation of the Sun? RHIC Users Meeting June 2013, Slide 4

Challenge: Nuclei from NN Interactions - How do we model atomic nuclei? QCD, but we need approximations Theory “Data” N. Ishii, S. Aoki, T. Hatsuda, Phys. Rev. Lett. 99, 022001 (2007) - Modern approaches to NN potentials include - QCD Inspired EFT - Epelbaum, Machleidt, … String Theory Inspired – Hashimoto … Lattice QCD – Detmold, Aoki … RHIC Users Meeting June 2013, Slide 5

Goal: Comprehensive Understanding of Nuclei § Two-nucleon, three-nucleon, etc. interactions are a foundation. What if they are imbedded in a nucleus? 12 C Nucleus § Are protons and neutrons in medium modified from their free structure? Maybe: EMC Effect and recent results from JLAB indicate yes § What affect does nucleon structure have on nuclear structure? § What other effects are present but unrecognized? RHIC Users Meeting June 2013, Slide 6

The Road Map: A Comprehensive Model of Atomic Nuclei § Step 1: Start from NN forces (ab initio theory) and study of light rare isotopes to determine the interactions of nucleons in nuclei and connect these to QCD by comparison to lattice calculations of NN, NNN forces, and couplings in EFT § Step 2: For mid-mass nuclei use configuration interaction models. The degrees of freedom and interactions must be determined from rare isotopes § Step 3: Use density functional theory, DFT, to connect to heavy nuclei. Rare isotopes help determine the form and parameters of the DFT. Rare isotopes play a key role at each step. RHIC Users Meeting June 2013, Slide 7

Theory Road Map: Comprehensive Model of Nuclear Structure and Reactions § Pictoral version of the Theory Road Map – Goal is a “standard model” for understanding nuclei Energy density functional Configuration interaction § Colors indicate the yields from FRIB. Access to a wide range and nuclei along the drip lines is critical Ab initio Continuum Relationship to QCD (LQCD) RHIC Users Meeting June 2013, Slide 8

Comparison of Calculated and Measured Binding Energies with NN models § Greens Function Monte Carlo techniques allow up to mass number 12 to be calculated § Blue 2 -body forces V 18 § S. Pieper B. Wiringa, et al. NN potential NN + NNN potential RHIC Users Meeting June 2013, Slide 9

New information from exotic isotopes S. Pieper B. Wiringa, et al. • Neutron rich nuclei were key in determining the isospin dependence of 3 body forces and the development of IL-2 R from UIX • New data on exotic nuclei continues to lead to refinements in the interactions NN + improved NNN potential Properties of exotic isotopes are essential in determining NN and NNN potentials RHIC Users Meeting June 2013, Slide 10

Current status of the GFMC calculations Carlson, Pieper, Wiringa, et al. RHIC Users Meeting June 2013, Slide 11

Application of GFMC technique to reactions of nuclei important to BB Nucleosynthesis § Resonance states in 5 He (n+4 He) K. Nollett, et al, PRL 2007; motivated by BBN modeling RHIC Users Meeting June 2013, Slide 12

Importance of 3 N forces § Big Bang Nucleosynthesis: Calculate all key reactions § Neutron star masses Gandolfi et al. , PRC 85, 032801 (2012) Nazarewicz et al. § Half-life of 14 C (Maris, Navratil et al. PRL), structure of calcium isotopes (Wienholtz et al. Nature), etc. RHIC Users Meeting June 2013, Slide 13

Construct NN Potentials: EFT based on QCD Symmetries – “Chiral” § Use the features of the pion in constructing an effective theory Cut-off parameter Λ ≅ 500 Me. V Contact interactions have constants that are fit to experiment Picture from E. Epelbaum Effective Field Theory, EFT, based on QCD Symmetries (Weinberg, Epelbaum , Furnstahl, Machleidt, van Kolck, Navrátil, … ) RHIC Users Meeting June 2013, Slide 14

Standard Shell Model § Mayer and Jensen Nobel prize in 1963 “"for their discoveries concerning nuclear shell structure" Magic Numbers N l 2 potential Spin-Orbit picture Niels Walet RHIC Users Meeting June 2013, Slide 15

Stability of Magic Nuclei Harder to excite RHIC Users Meeting June 2013, Slide 16

Stability of Magic Nuclei 20 protons Harder to excite 16 protons 14 protons RHIC Users Meeting June 2013, Slide 17

Surprise: Changing Magic Numbers Harder to excite Reason: A tensor force that depends on angular momentum and isospin (Otsuka et al. ) RHIC Users Meeting June 2013, Slide 18

Step 3: Density Functional Theory § Widely used in Chemistry– based on Hohenberg-Kohn (Phy Rev 136) § Relies on the variation concept where observables are treated as variational parameters, e. g. local density ρ(r) and its derivative § We don’t know the correct form for nuclei. Example: Skyrme functional § Use rare isotopes to test functional forms, determine parameters, provide insight N. Schunck, Exotic Beam Summer School 2012 for improvements RHIC Users Meeting June 2013, Slide 19

Prediction of the limits of the nuclear landscape J. Erler et al. , Nature 486, 509 (2012) 265 stable isotopes, 3100 observed, more like 2000 “known”, 6900(600) possible RHIC Users Meeting June 2013, Slide 20

Weakly bound isotopes have unique features “Normal” “Halo” Tanihata PRL 1985 “Skin” Tanihata PLB 1992 220 Rn 11 Li 80 Ni New Science: Pairing in low-density material, new tests of nuclear models, open quantum system, interaction with continuum states - Efimov States - Reactions see e. g. H. -W. Hammer and L. Platter, Ann. Rev. Nucl. Part. Sci. 60, 207 (2010) RHIC Users Meeting June 2013, Slide 21

Weakly Bound Nuclei are Open Quantum Systems Dobaczewski et al. , Prog. Part. Nucl. Phys. 59, 432 (2007) W Nazarewicz RHIC Users Meeting June 2013, Slide 22

The Origin of the Elements § One of 11 Science Questions for the 21 st century § How were the elements from iron to uranium made? • Where and how does the rprocess occur? RHIC Users Meeting June 2013, Slide 23

New data on elemental abundances: Surveys and Large Aperture Telescopes § The measurement of elemental abundances is at the forefront of astronomy using large telescopes § Large mirrors enable high resolution spectroscopic studies in a short time (Subaru, Hubble, LBT, Keck, …) § Surveys provide large data sets (SDSS-III, RAVE, LAMOST, Sky. Mapper, LSST…) § Future missions: JWST - “is specifically designed for discovering and understanding the formation of the first stars and galaxies, measuring the geometry of the Universe and the distribution of dark matter, investigating the evolution of galaxies and the production of elements by stars, and the process of star and planet formation. ” Hubble Space SUBARU RHIC Users Meeting June 2013, Slide 24

Simulation of Solar System Abundances Timmes, Woosley, Weaver Astro. Journal 1995 Parameters: • Supernovae type Ia and II • Number (77 supernovae with Ms 11 -40 Msun) • Progenitor mass distributions • Age of the galaxy • … Results: • SN rate 1/3 comes from type Ia • They reproduce measured 7 Li abundance metalicity vs. time etc. Success ! ? Note above A=72 we can’t model RHIC Users Meeting June 2013, Slide 25

Neutron-capture process leading to elements heavier than iron § E. M. Burbidge, G. R. Burbidge, W. A. Fowler, and F. Hoyle. (1957). "Synthesis of the Elements in Stars". Rev Mod Phy 29: 547, must be an r-process (10% of gold from s-process) § Rapid neutron capture process, r-process • Fast, few second duration • Neutron density of 1020 -28 n/cm 3 • Runs out to where (n, γ) and (γ, n) are similar in rate • Adds 30 -40 neutrons • Site unknown Reaction path βAZ (γ , n) fission … (n, γ) RHIC Users Meeting June 2013, Slide 26

Advances in Theoretical Astrophysics § We now have several robust, self-consistent r-process models; to test them against observations, we need nuclear data Neutrino Driven Wind Hoffman et al. 2008 10 Winteler et al. 2012 1 40 Neutron Star Mergers 80 Mass number 100 MHD Supernova Jets abundance Korobkin et al. 2012 60 Mass number RHIC Users Meeting June 2013, Slide 27

Uncertainty between models and nuclear properties 101 Astrophysics Hot bubble Classical model Same nuclear physics Abundance 100 Nuclear physics ETFSI-Q masses ETFSI-1 masses Same (classical) r-process model 10 -1 10 -2 10 -3 10 -4 Freiburghaus et al. 1999 Mass number H. Schatz RHIC Users Meeting June 2013, Slide 28

New Facilities will Enable the Needed Breakthrough in Nuclear Physics Different key-regions probe different model aspects when compared to observations N=126 N=82 Critical region probes: Main r-process parameters Production of actinides Critical region: Disentangle r-processes Critical region probes: r-process freezeout behavior (Mumpower et al. 2012) Critical region probes: Neutrino fluence Critical region probes: Main r-process parameters H Schatz RHIC Users Meeting June 2013 , Slide 29

New Facilities will Enable the Needed Breakthrough in Nuclear Physics Different key-regions probe different model aspects when compared to observations FRIB reach for T 1/2, masses, and β-delayed neutron emission (Overlap with applications!) N=126 N=82 Critical region probes: Main r-process parameters Production of actinides Critical region: Disentangle r-processes Critical region probes: r-process freezeout behavior (Mumpower et al. 2012) Critical region probes: Neutrino fluence Critical region probes: Main r-process parameters H Schatz RHIC Users Meeting June 2013 , Slide 30

Stellar Hydrogen Explosions: Common (100/day) and Not Understood www 4. nau. edu § Open questions • Neutron star size • Short burst intervals • Multiple peaked bursts • Nature of superbursts • Ejected mass (Nucleosynthesis) • Observable gamma emitters • Why such a variety • Path to Ia supernovae RHIC Users Meeting June 2013, Slide 31

Making Sense of X-ray Burst Observations § Need nuclear data on rare isotopes to create reliable model templates to analyze observations Amthor, Cyburt et al. 2012 Galloway et al. GS 1826 -24 Burst profiles depend on nuclear rates With accurate model templates Redshift variation ~5000 widely varying bursts Zamfir et al. 2012 • • • Absolute peak flux, distance H/He composition Redshift + color correction (distance and anisotropy independent) neutron star size RHIC Users Meeting June 2013, Slide 32

FRIB Reach for Novae and X-ray burst reaction rate studies 10>10 109 -10 108 -9 107 -8 106 -7 105 -6 104 -5 102 -4 rp-process direct (p, g) direct (p, a) or (a, p) transfer key reaction rates can be indirectly measured including 72 Kr waiting point (p, p), some transfer most reaction rates up to ~Sr can be directly measured All reaction rates up to ~Ti can be directly measured RHIC Users Meeting June 2013, Slide 33

Rare Isotope Crusts of Accreting Neutron Stars KS 1731 -260 (Chandra) Cackett et al. 2006 (Chandra, XMM-Newton) § Nuclear reactions in the crust set thermal properties (e. g. cooling) § Can be directly observed in transients § Directly affects superburst ignition Understanding of crust reactions offers possibility to constrain neutron star properties (core composition, neutrino emission…) H. Schatz RHIC Users Meeting June 2013, Slide 34

Where do Neutrons Drip? Known mass Dripline known FRIB reach: dripline up to A~100 + mass measurements + EC rates via charge exchange K. -Y. Lau, M. Beard, P. Shternin, et al. , to be published RHIC Users Meeting June 2013, Slide 35

Are the fundamental interactions that are basic to the structure of matter fully understood? • Angular correlations in β-decay and search for scalar currents o o Adopted from Savard et al. Mass scale for new particle comparable with LHC 6 He and 18 Ne at 1012/s • Electric Dipole Moments o 225 Ra, 223 Rn, 229 Pa (10, 000 x more sensitive than 199 Hg; 229 Pa > 1010/s) e • Anapole moment in Fr atoms o γ Understanding of weak interactions in nuclei (francium isotopes; 1010/s) • Unitarity of CKM matrix 212 Fr Z Vud by super allowed Fermi decay o Probe the validity of nuclear corrections o RHIC Users Meeting June 2013, Slide 36

Rare Isotopes For Society § FRIB offers fast development of 1000 s of isotopes (via harvesting) § Isotopes for medical research • Examples: 47 Sc, 62 Zn, 64 Cu, 67 Cu, 68 Ge, 149 Tb, 153 Gd, 168 Ho, 177 Lu, 188 Re, 211 At, 212 Bi, 213 Bi, 223 Ra (DOE Isotope Workshop) • -emitters 149 Tb, 211 At: potential treatment of metastatic cancer • Cancer therapy of hypoxic tumors based on 67 Cu treatment/64 Cu dosimetery § Reaction rates important for stockpile stewardship and nuclear forensics • • Determination of extremely high neutron fluxes by activation analysis Rare isotope samples for (n, g), (n, n’), (n, 2 n), (n, f) e. g. 88, 89 Zr More difficult cases studied via surrogate reactions (d, p), (3 He, xn) … We can produce quantities of separated fission products for tests of detection techniques § Tracers for Marine Studies (32 Si), Condensed Matter (8 Li), industrial tracers (7 Be, 210 Pb, 137 Cs, etc. ), … § Data for advance reactor design and destruction of nuclear waste RHIC Users Meeting June 2013, Slide 37

Summary § We are entering a new era in nuclei physics when we can produce and study key rare isotopes: § Development of a standard model for nuclei • What are the heaviest elements possible? • What is the origin of the nuclear force in QCD and EW • In 15 years we might know the answer § Foundation for astrophysical modeling • With new rare isotopes we will be able to better model stellar processes • We will have the ability to understand the history of a star (or meteorite) • Modeling of neutron stars, novae, supernovae will be on a more solid footing § Search for symmetry violations, e. g. atomic EDMs • enhanced sensitivity from FRIB will allow most of the interesting EDM scales to be covered RHIC Users Meeting June 2013, Slide 38

Major US Project – Facility for Rare Isotope Beams, FRIB § Funded by DOE Office of Science – 2020 completion § Key Feature is 400 k. W beam power (5 x 1013 238 U/s) § Separation of isotopes in-flight • Fast development time for any isotope • Suited for all elements and short half-lives RHIC Users Meeting June 2013, Slide 39

New Insight from Mass Model Comparison to Data HFB-14: Hartree-Fock-Bogoliubov w/delta pairing force S. Goriely, M. Samyn, J. M. Pearson, Phys. Rev. C 75 (2007) 064312 J. Duflo, A. P. Zuker, Phys. Rev. C 52 (1995) R 23 Model Based MEHFB 14 –Shell MEAME 2003 MEDZmass – ME–AME 2003 ME = (Actual A u) x 931. 5 Me. V/u u = atomic mass unit (931. 5 Me. V) Less bound than data More bound than data www. nuclear masses. org RHIC Users Meeting June 2013, Slide 40

“Ab Initio” start with NN forces § Approach: Construct NN potentials based on neutron and proton scattering data and properties of light nuclei (Bonn, Reid, Illinois AV 18, Nijmegen, etc. ) § More recent approach is to construct the potentials some more fundamental theory • QCD Inspired EFT • String Theory Inspired – Hashimoto et al • Lattice QCD N. Ishii, S. Aoki, and T. Hatsuda, Phys. Rev. Lett. 99, 022001 (2007) RHIC Users Meeting June 2013, Slide 41

Configuration Interaction Models § The interaction of nuclei create a “mean field”. We think of nucleon moving in this potential. 12 C § Shell Model is the most common in nuclear science § Solve the equation HΨ=EΨ § Introduce a basis (usually harmonic oscillator) and solve the matrix equation § Can assume inert closed cores for certain nuclei (e. g. N=Z=20) § No core shell model does not make this assumption § All shell models use effective operators (interactions depend on model space RHIC Users Meeting June 2013, Slide 42

“No Core” Shell Model § Use ab initio interactions derived by some means like EFT or fits to NN scattering in a shell model § Diagonalize in a large basis of many-body states From A. Poves, International School on Exotic Beams, Santiago de Compostela, September 4 -11 2010 (see also J Vary, etc. ) RHIC Users Meeting June 2013, Slide 43

FRIB Reach For Crust Processes • Interesting set of reactions leading to proton-rich material converted to neutron-rich material Known mass Electron capture rates Mass measurements Drip line established Haensel & Zdunik Astro Journ 1990, 2003, 2008 Gupta et al. Astro Journ 2006 H. Schatz RHIC Users Meeting June 2013, Slide 44

There a number of nucleosynthesis processes that must be modeled § Big Bang Nucleosynthesis § pp-chain § CNO cycle Sample reaction paths § triple alpha § Helium, C, O, Ne, Si burning (α, γ) § s-process (p, γ) § r-process β(α, p) § rp-process § νp – process AZ (n, 2 n) (n, γ) § p – process § α - process § fission recycling β+ , (n, p) § Cosmic ray spallation (γ, p) § pyconuclear fusion fission Black - FRIB critical for modeling RHIC Users Meeting June 2013, Slide 45

How many isotopes might exist? § Estimated Possible: Erler, Birge, Kortelainen, Nazarewicz, Olsen, Stoitsov, Nature 486, 509– 512 (28 June 2012) , based on a study of EDF models § “Known” defined as isotopes with at least one excited state known (1900 isotopes from NNDC database) § Represents what is possible now RHIC Users Meeting June 2013, Slide 46

The Number of Isotopes Available for Study at FRIB (next generation facilities) § Estimated Possible: Erler, Birge, Kortelainen, Nazarewicz, Olsen, Stoitsov, Nature 486, 509– 512 (28 June 2012) , based on a study of EDF models § “Known” defined as isotopes with at least one excited state known (1900 isotopes from NNDC database) § For Z<90 FRIB is predicted to make > 80% of all possible isotopes RHIC Users Meeting June 2013, Slide 47

A Vision “It is in my view that continued development and application of radioactive beam techniques could bring the most exciting results in laboratory astrophysics in the next decade” Nobel Laureate Willy Fowler, 1984 RHIC Users Meeting June 2013, Slide 48

Unusual Isotopes to Test Fundamental Symmetries – Electric Dipole Moment Search A Electric Dipole Moment, EDM, • Violates CP symmetry • Large value would be evidence for physics beyond the standard model • Possible explanation for matter dominance over antimatter Wolfgang Korsch RHIC Users Meeting June 2013, Slide 49

EDM Searches in Three Sectors § Best current limit in nuclei is from WC Griffiths et al. PRL 102, 101601 (2009) d (e-cm) < 3. 1 x 10 -29 Nucleons (n, p) Quark EDM Nuclei (Hg, Ra, Rn) Quark Chromo-EDM Electron in paramagnetic molecules (Yb. F, Th. O) Electron EDM Physics beyond the Standard Model: SUSY, etc. § Rare isotopes offer the chance for enhanced sensitivity § Current efforts: • 223 Rn • • TRIUMF: E 929 Spokespersons T. Chupp (Univ of Michigan), C. Svensson (Guelph) 225 Ra Argonne National Laboratory: Z-T Lu 225 Ra at TRIμP at KVI Z-T Liu, Univ. of Chicago RHIC Users Meeting June 2013, Slide 50

Example: EDM of 225 Ra Enhanced 225 Ra: I=½ t 1/2 = 15 d • Closely spaced parity doublet – Haxton & Henley (1983) • Large intrinsic Schiff moment due to octupole deformation – Auerbach, Flambaum & Spevak (1996) • Relativistic atomic structure (225 Ra / 199 Hg ~ 3) – Dzuba, Flambaum, Ginges, Kozlov (2002) Parity doublet |a |b Enhancement Factor: EDM (225 Ra) / EDM (199 Hg) Skyrme Model - = (| - |b )/ 2 55 ke. V Isoscalar Isovector Isotensor SIII 300 4000 700 Sk. M* 300 2000 500 LP Gaffney et al. Nature 1998000 SLy 4 497 (2013) 700 + = (| + |b )/ 2 1000 Schiff moment of 225 Ra, Dobaczewski, Engel (2005) Schiff moment of 199 Hg, Ban, Dobaczewski, Engel, Shukla (2010) RHIC Users Meeting June 2013, Slide 51

More than half of Z>28 from an r-process § E. M. Burbidge, G. R. Burbidge, W. A. Fowler, and F. Hoyle. (1957). "Synthesis of the Elements in Stars". Rev Mod Phy 29: 547, must be an r-procees (10% of gold from s-process) § We know they must be made in a neutron-rich environment T > 109 K, neutron ≈ 1020 -28 cm-3 , that lasts for about 1 second; called the rapidneutron capture process, r-process § Type II supernovae are a possible site (+ variants) • Neutrino driven shock wave, however models do not produce the entropy and neutron flux needed to match abundance data (although we can’t say that for sure) • Shock waves in C-O layers • Magnetic outflows § Colliding neutron stars would also work, but there does not seem to be enough of these in the early universe to explain how much heavier elements we see § Once the underlying physics is known, we can infer information of the site from observational data RHIC Users Meeting June 2013, Slide 52

Transiently Accreting Neutron Stars Allow the Study of Dense Matter § Reliable crust models need rare isotope data to interpret observations KS 1731 -260 Cooling profile provide information on the crust Bright X-ray burster for ~12 yr Accretion shut off early 2001 Unknown heat source was added Neutrons drip here? Superfluid? Core? MXB 1659 -29 Brown & Cumming 2009 NASA/Chandra/Wijnands et al. Brown&Cumming 2009 RHIC Users Meeting June 2013, Slide 53

FRIB Will Provide Isotopes Needed for the Nation’s Future “Most of the isotopes in use today in practical settings were developed as long as 50 years ago. With few exceptions (e. g. , 82 Sr and 90 Y) there are no new products or services that use isotopes developed in the past 20 years. Without the availability of research isotopes, it is not possible to develop new science or new applications based on isotopes. This problem is extreme in the case of accelerator isotopes …” Subcommittee Finding Isotopes for the Nation's Future NSAC Long Range Plan Study 2008 § FRIB can provide isotopes for applied science while serving forefront nuclear research § FRIB is designed to provide fast access to a broad range of new isotopes for research RHIC Users Meeting June 2013 , Slide 54

One of the Challenges: Nuclear Structure 12 C Hoyle State triple α process See e. g. EFT of E. Epelbaum et al. PRL 106, 192501 (2011) α+α+α Energy [Me. V] http: //www. tunl. duke. edu/nucldata/ Nucl. Phys. A 506 (1990) RHIC Users Meeting June 2013, Slide 55