Designer Nuclei – And How to Use Them Witold Nazarewicz (Tennessee/ORNL)

1. Designer Nuclei – And How to Use Them Witold Nazarewicz (Tennessee/ORNL) UT Science Forum, Nov. 20, 2009 • Three take-away messages: • Nuclear scientists, experimentalists and theorists, are getting better and better at controlling short-lived nuclei, in particular those which are useful • Rare isotopes are the key to answering questions in many areas of science • Rare isotopes provide society with numerous opportunities • Introduction (Lego Block Approach) • Territory of Femtoscience • Science Stories • Connections and Relevance • Perspectives 1 fm = 0.000000000000001 m = 10-15 m

3. Munster 1544 Wyld 1824 Jaillot 1694

4. reduction complexity The Quantum Ladder Galaxy clusters Galaxies Stars Planets macroscopic Living Organisms, Man-made Structures Cells, Crystals, Materials Molecules Atoms Nuclei Elementary Particles (baryons, mesons) Quarks and Leptons subatomic Super- strings ? ???

5. 4-Helium nucleus (alpha-particle) The nucleus is heavy: mp~mn~1840 me The nuclei located at the center of each atom comprise over 99.9% of the mass of the visible universe All atoms can be constructed from only three fundamental building blocks: Z electrons (charge=-e) Z protons (charge=+e) N neutrons (neutral) Protons and neutrons are very similar; hence they are termed nucleons. The nucleus has A=N+Z nucleons. Helium atom

6. Radioactive Ion Science Timeline Relativistic Coulomb excitation of 32-Mg at RIKEN Direct radiative capture with 21-Na at ISAC-I 38m-K -correlations at TRINAT 100-Sn discovered at GSI and GANIL Europe Japan First mass measurement of short-lived nuclei at PS in CERN First accelerated beam experiment (13-N) at LLN Two-proton emitters discovered at GSI and GANIL Canada Momentum distribution of halo at RIKEN Z=105 (Db) discovered in Dubna Element Z=112 discovered Measurement of half-life of r-process nucleus at Studsvik Mössbauer effect Projectile-fisson of 238-U and Z=112 discovered at GSI Proton emission discovered at Harwell Theory of nucleosynthesis BBHF theory of nucleosynthesis Z=108 chemistry at GSI Becquerel discovers radioactivity The Curies discover polonium Acceleration of RIBs at LLN Beta-delayed proton radioactivity discovered at Dubna and McGill Island of inversion at N=20 and shape coexistence in proton-rich Hg at iSOLDE Targeted alpha therapy at ISOLDE ISOLTRAP First ISOL experiment in Copenhagen Becquerel discovers radioactivity The Curies discover polonium Laser ion source at ISOLDE Neutron-induced fission IGISOL at Jyväskylä Isotopic tracer technique by von Hevesy Nobel Prize for magic numbers Nobel Prize for unified model 6-He produced in Copenhagen Explanation of magic numbers Explanation of magic numbers RIKEN SPIRAL1 ISOLDE GSI GANIL ISAC-I REX-ISOLDE Nobel Prize for unified model 1900 1930 1960 2000 Parity violation in beta decay Fermi builds controlled fission reactor NSCL HRIBF Shell structure changes in exotic nuclei at ATLAS/HRIBF/NSCL Collapse of magic numbers in exotic nuclei Nobel Prize for magic numbers Nobel Prize for nucleosynthesis Invention of PET scanner Trapped francium at Stony Brook Explanation of magic numbers First in-flight separator at Oak Ridge First therapeutic application of artificial radionuclide First in-flight fragmentation experiments at Berkeley Radiochemistry used to monitor nuclear weapons tests Shell structure of exotic nuclei with knockout reactions at NSCL 6-He enhanced reaction cross sections at TwinSol beta-NMR demonstrated at ANL Z=100 (Fm) discovered First application of radiochemistry to inertial fusion target diagnosis BBHF theory of nucleosynthesis Studies with accelerated 132-Sn and 82-Ge at HRIBF Neutron halos discovered Neutron halos discovered at Berkeley 21-Na -correlations at Berkeley Measurement of half-life of r-process nucleus at TRISTAN Charge radius of 6-He at ATLAS 78-Ni lifetime at NSCL United States

7. Some nuclei are more important than others - + - + - + tests of fundamental laws of nature nuclear structure + - + - 45Fe 149Tb astrophysics applications 18F,22Na 225Ra Over the last decade, tremendous progress has been made in techniques to produce designer nuclei, rare atomic nuclei with characteristics adjusted to specific research needs

8. The Nuclear Landscape superheavy nuclei proton drip line neutron drip line • How do protons and neutrons make stable nuclei and rare isotopes? • What are properties of neutron matter? • What are the heaviest nuclei that can exist? 82 126 protons terra incognita 50 82 28 20 50 stable nuclei 8 28 2 20 known nuclei 8 2 neutrons

9. Science

10. electronic shells of the atom 54 5p 4d 5s 36 4p 3d 4s noble gases (closed shells) 18 3p 3s 10 2p From: Atom Animation Resources 2s

11. nucleonic shells of the nucleus 1949 magic nuclei (closed shells) N-Z ? 126 3p1/2 1h9/2 2f5/2 2f5/2 1i13/2 3p1/2 3p3/2 Near the drip lines nuclear structure may be dramatically different. 3p3/2 Magicity is a fragile concept 1h9/2 2f7/2 2f7/2 1h11/2 82 2d3/2 1g7/2 1h11/2 2d3/2 3s1/2 3s1/2 1g7/2 2d5/2 2d5/2 50 1g9/2 1g9/2

12. 0.0000000000014 cm 11Li: Borromean halo nucleus Z=3, N=8 The Borromean Rings n+n is unbound n+ 9Li is unbound but n+n+ 9Li is bound ! n 9Li n 208Pb: well bound heavy nucleus Z=82, N=126

13. Neutron skins and neutron stars neutrons 0.12 n 0.08 p 0.04 0.00 0.12 0.08 0.04 0.00 100Sn protons N/Z=1 density (nucleons/fm3) 100Zn N/Z=2.33 0 2 4 6 8 r (fm)

14. Limits of Mass and Charge: Superheavies 226Ra 2008 238U 237Np 242Pu 245Cm 249Cf 2004 244Pu + 48Ca 243Am 248Cm hot fusion 2 events/year …also: 286,287114 48Ca+242Pu from LBNL From Y. Oganessian

15. Superheavy Elements in Nuclear DFT S. Cwiok, P.H. Heenen, W. Nazarewicz Nature, 433, 705 (2005) long-lived SHE

16. Periodic Table of Elements 2009 Cn 113 114 115 116 118 112 Cn Z=112: Copernicium very volatile noble metal! Nature 447, 72 (2007)

17. (p,) (,) (,p) (p,) (b+) How does the physics of nuclei impact the physical universe? X-ray burster supernova What is the origin of elements heavier than iron? p process s-process nova How do stars burn and explode? r process rp process neutron star Crust processes proton number stellar burning What is the nucleonic structure of neutron stars? neutron number N

18. Rare isotope measurements for novae Hernanz et al, 2003 ESA INTEGRAL Satellite searching for novae signatures O Ne Mg Nova Nova QUVul, HST 26gAl(p,)27Si TRIUMF (2006) 17F(p,)18Ne 18Ne capture reaction 21Na(p,)22Mg TRIUMF (2004) 17F energy loss scattered 17O scattered on resonance (600 keV) HRIBF (2008) total energy Example of synergy between nuclear science and astronomy predicted -ray flux from decaying radionuclides 18F, 22Na... synthesized in explosion Synthesis of e.g. 18F, 22Na, (26Al) very important for characteristic g-ray emission from nova

19. r (apid neutron capture) process Supernova masses, decays, level structure, and reactions are all important for calculating r-process reaction flow • The origin of about half of elements heavier than iron • Goes through neutron-rich rare isotopes The iron in your blood and the calcium in your bones were formed in the supernova explosion of a massive star millions of years before the formation of the Earth itself. http://www.jinaweb.org/html/gallery3.html

20. Superallowed Fermi 0+ 0+-decay studies (testing the unitarity of the Cabibbo-Kobayashi-Maskawa matrix) Rare Isotopes, Weak Force, and the 2008 Nobel Prize in Physics … for "the discovery of the origin of broken symmetry, which predicts the existence of at least three families of quarks in nature." Half-life Q-value Branching Ratio

21. with new symmetry-breaking corrections: with new symmetry-breaking corrections: 0.9996(7) nuclear meson decay From Hardy/Savard

22. Connections and Relevance The physics of nuclei forms the intellectual bridge between the very large and the very small in our natural world

23. Connections to small complex systems Understanding the transition from microscopic to mesoscopic to macroscopic Carbon nanotubes Trapped condensates Quantum dots • Dilute fermion matter • Low-density neutron matter • Cold fermions in traps

24. Societal Benefits • Energy, transmutation of waste… • Can we use fast neutron reactors and accelerators for the mitigation of long-lived radioactive waste? • Can we design an economically competitive, energy efficient, reduced-waste nuclear reactor? • Medical and biological research • Numerous applications of radionuclides • Materials science • Rare-isotopes have broad applications in condensed matter and materials science as low density, very high signal to noise in situ detectors of local atomic environments • Environmental science • Stockpile stewardship • Modeling the diverse reaction pathways driven by both neutrons and charged particles spanning an energy spectrum from about 0.1 to 16 MeV (analogous to the r-process)

25. Ernest and John Lawrence John Lawrence was a physicist and physician, a pioneer of nuclear medicine. He discovered treatments for leukemia and polycythemia by injecting infected mice with radioactive phosphorus derived from the cyclotron invented by his brother In the summer of 1935, John came to Berkeley to conduct research on the medical applications of radiation. He injected some leukemic mice with radioactive phosphorus produced by the cyclotron and then went fishing; when he returned he found the mice improved. It was the beginning of medical physics at Berkeley. John was also more aware than were the physicists in the laboratory of the dangers of exposure to radiation, so he insisted that they undertake some experiments with the radiation produced by the cyclotron. He conducted an experiment that he described, years later, in this way: One of the first animals that we exposed - I'm not sure that it wasn't the first one - we … placed within the cyclotron between the two poles of the magnet near the beryllium target which was being struck with alpha particles. So Paul and I told Ernest to turn off the cyclotron because we wanted to go back and see how the rat was. Well, the rat was dead. That scared everybody because it had only been exposed for about a minute and the dose was very low. We were very scared and we then recommended increasing the shielding around the cyclotron. Later we found that the rat died of suffocation but not radiation.

26. None of these achievements however was as important and satisfying as that which occurred in 1937. Within months of John's arrival in Berkeley, he and Ernest learned that their mother was diagnosed with uterine cancer; she went to the Mayo Clinic for treatment. John went to Mayo immediately. Mother Lawrence was told that she had only three months to live. John tells the story in his oral history, in the archives at Berkeley: So then I got on the phone with Ernest. I said, "They don't want to treat her here with radiation. How about my bringing her out and we'll talk to Dr. Stone?" We did talk to Dr. Stone and he said, "Sure, I'll take her." So I took her on the train, wheeled her across the station in Omaha. (…) She was about 67 or 68 years old then…. They started treating her through four fields…. To make a long story short, this massive tumor just started evaporating. At the end of ten years my mother finally agreed that she must be cured. It took me about ten years to convince her and she died at 83 and had the best years of her life…. It was really, really a fantastic result.

27. What are the next medically viable radioisotopes required for enhanced and targeted treatment and functional diagnosis? Example: Targeted Alpha Therapy in vivo The radionuclide 149Tb decays to alpha particles 17 percent of the time and has a half-life of 4.1 hours, which is conveniently longer than some other alpha-emitting radionuclides. Low-energy alpha particles, such as in 149Tb decays, have been shown to be very efficient in killing cells, and their short range means that minimal damage is caused in the neighborhood of the target cells. -knife! First in vivo experiment to demonstrate the efficiency of alpha targeted therapy using 149Tb produced at ISOLDE, CERN G.-J. Beyer et al.Eur. J. Nucl. Med. and Molecular Imaging 33, 547 (2004)

28. Survival of mice… 100 149 5 MBq Tb, 5 µg MoAb 90 80 70 no MoAb 60 300 µg MoAb, cold % of survived mice 50 40 5 µg MoAb, cold 30 20 10 0 0 20 40 60 80 100 120 Survival time, days 5*106 Monoclonal Antibody 2 days later the mice have been devided into 4 groups:

29. Perspectives on designer nuclei

30. Experiment FRIB TRIUMF GSI NSCL GANIL ISOLDE RIKEN HRIBF Future major facilities Existing major dedicated facilities Radioactive Ion Beam Facilities Worldwide

31. Theoretical Tools and Connections to Computational Science 1Teraflop=1012 flops 1peta=1015 flops (today) 1exa=1018 flops (next 10 years)

32. Multimodal fission in nuclear DFT 1939 - Meitner & Frisch 1939 - Bohr & Wheeler 70 years ago! • Staszczak et al., Phys. Rev. C 80, 014309 (2009)

33. Outlook The study of rare isotopes makes the connection between the fundamental building block of matter, complex systems, and the cosmos • Exciting and transformational science; old paradigms revisited • Interdisciplinary science • Science relevant to society Over the last decade, tremendous progress has been made in techniques to produce designer nuclei, rare atomic nuclei with characteristics adjusted to specific research needs. Guided by unique data on short-lived nuclei, we are embarking on a comprehensive study of all nuclei based on the most accurate knowledge of nuclear interactions, the most reliable theoretical approaches, and the massive use of the computer power available at this moment in time. The prospects are excellent. Thank You

34. Backup

35. nano… Complex Systems Giga… Cosmos femto… Physics of Nuclei Quantum many-body physics Nuclear Astrophysics • In-medium interactions • Symmetry breaking • Phases and phase transitions • Chaos and order • Open systems • Origin of the elements • Energy generation in stars • Neutron-rich nucleonic matter • Electroweak processes subfemto… • Hot and dense • Cold • How does complexity emerge from simple constituents? • How can complex systems display astonishing simplicities? How do nuclei shape the physical universe? In search of the New Standard Model Fundamental interactions • Neutrinos • Matter-antimatter imbalance • Beyond the new standard model

36. 62Ga @ TRIUMF (2006-2008) T1/2=116.100(22)ms, BR=99.858(8)% Jyväskylä (2008) BR=99.893(24) 34Ar, 34Cl @TAMU (2006) T1/2=843.8(4) ms,1.5268(5)s 38mK @TRIUMF (2008) BR=99.967(4)% 46V @ ANL (2005) Q=7052.90(40) keV 46V @ Jyväskylä (2006) Q=7052.72(31) keV Munich tandem (2008) Q=7052.10(31) keV 50Mn,54Co @Jyväskylä (2007) Q=7634.48(7), 8244.54(10) keV 26mAl,42Sc @Jyväskylä (2006) Q=4232.83(13),6426.13(21) keV 26mAl @ISOLDE (2008) Q 38mK

39. How do protons and neutrons make stable nuclei and rare isotopes? What is the origin of simple patterns in complex nuclei? What is the equation of state of matter made of nucleons? What are the heaviest nuclei that can exist? When and how did the elements from iron to uranium originate? How do stars explode? What is the nature of neutron star matter? How can our knowledge of nuclei and our ability to produce them benefit the humankind? Life Sciences, Material Sciences, Nuclear Energy, Security Questions that Drive the Field Physics of nuclei Nuclear astrophysics Applications of nuclei