Slid 1Brad Sherrill WG.9 July 2010, Slide 1
Nuclear Physics at Rare-Isotope Facilities in North-America
IUPAP WG.9 Symposium 2-3 July, 2010Bradley M. Sherrill
Michigan State University
Slid 2Brad Sherrill WG.9 July 2010, Slide 2
The Science of Rare Isotopes
Properties of nuclei (nuclear structure)– Develop a predictive model of nuclei and their interactions– Many-body quantum problem: intellectual overlap to mesoscopic
science, quantum dots, atomic clusters, etc.
Nuclear processes in the universe– Chemical history of the universe, (explosive) nucleo-synthesis– Properties of neutron stars,
EOS of asymmetric nuclear matter
Tests of fundamental symmetries– Effects of symmetry violations are
amplified in certain nuclei
Societal applications and benefits– Bio-medicine, energy, material
sciences, national security
Slid 3Brad Sherrill WG.9 July 2010, Slide 3
Nuclei matter
• The atomic nucleus is a significant intellectual challenge with three of nature’s four forces having a significant role. Can we construct a comprehensive and predictive model of its properties? How do we relate that model to QCD? Surprises are still likely.
• The properties of nuclei are relevant to other sciences, e.g., neutrinoless double-beta decay the rate is related to nuclear matrix elements
• Wealth of quantum phenomena of interest to related sciences– Mesoscopic systems– Simple patterns in complex systems (Symmetry phases)– Connections to atomic clusters– Open quantum system– Nuclear reactions– Efimov states– …
Slid 4Brad Sherrill WG.9 July 2010, Slide 4
Properties of rare isotopes are essential in determining NN and NNN potentials
• Neutron rich nuclei were key in determining the isospin dependence of 3-body forces and the development of IL-2R from UIX
• New data on exotic nuclei continues to lead to refinements in the interactions, e.g., strength of NN and NNN interactions
• EFT developments, LQCD and even computational power are providing insight for ab initio theories, but they need grounding in data
S. Pieper B.Wiringa, et al.
Slid 5Brad Sherrill WG.9 July 2010, Slide 5
Application of GFMC technique to reactions of nuclei
• Resonance states in 5He (n+4He)
Nollett, et al, PRL 2007; motivated by BBN modeling
Slid 6Brad Sherrill WG.9 July 2010, Slide 6
Theory Road Map: Comprehensive Model of Nuclear Structure and Reactions
• Theory Road Map – comprehensive description of the atomic nucleus– Ab initio models – study of neutron-rich, light
nuclei helps determine the force to use in models (measurement of sensitive properties for N=14, 16 nuclei)
– Configuration-interaction theory; study of shell and effective interactions (study of key nuclei such as 54Ca, 60Ca, 122Zr)
– The universal energy density functional (DFT) – determine parameters (broad view of mass surface, BE(2)s, BE(4)s, fission barrier surface, etc.)
– The role of the continuum and reactions and decays of nuclei (halo studies up to A ~100)
• IMPORTANT: Understand and select the most sensitive measurements Ab initio
Configurationinteraction
Energy density functional
Continuum
Relationship to QCD (LQCD)
Slid 7Brad Sherrill WG.9 July 2010, Slide 7
The Challenge: Understand the Chemical History of the Universe
• Understanding the chemical history of the universe and what it tells us about individual stars, the first stars, galactic evolution
• The abundance of elements tell us about the history of events prior to stellar formation. How can we extract that information?
Lodders (2003) Solar system abundances
Slid 8Brad Sherrill WG.9 July 2010, Slide 8
Forefront of Observational Astronomy: High Resolution 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 (Hubble, LBT, Keck, …)
• Surveys have provided large data sets (SDSS, LAMOS, SkyMap, HERMES, LSST, Gaia, …)
• 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.”
HubbleSpace
Large Binocular Telescope
Slid 9Brad Sherrill WG.9 July 2010, Slide 9
Search for the ashes of the first stars
• Less Fe implies earlier star formation
• Measured with high resolving power telescopes, Hubble, Keck, LBT, etc.
• The process that makes Ba must be different from the main process that makes Fe
• The [Ba/Fe] pattern is not understood
Logarithmic ratio of abundances relative the Sun
Slid 10Brad Sherrill WG.9 July 2010, Slide 10
There are a number of nucleosynthesis processes
• Big Bang Nucleosynthesis• pp-chain• CNO cycle• Helium, C, O, Ne, Si burning• s-process• r-process• rp-process• νp – process• p – process• α - process• fission recycling• Cosmic ray spallation• pyconuclear fusion• + others
Green – rare isotopes are necessary for accurate modeling of this process
Slid 11Brad Sherrill WG.9 July 2010, Slide 11
Tests of Nature’s Fundamental Symmetries
• Angular correlations in β-decay and search for scalar currentso Mass scale for new particle comparable
with LHCo 6He and 18Ne at 1012/s
• Electric Dipole Momentso 225Ac, 223Rn, 229Pa (30,000 more sensitive
than 199Hg; I > 1010/s)
• Parity Non-Conservation in atomso weak charge in the nucleus (francium
isotopes; 109/s)
• Unitarity of CKM matrixo Vud by super allowed Fermi decay o Probe the validity of nuclear corrections
e γ
Z
212Fr
Slid 12Brad Sherrill WG.9 July 2010, Slide 12
Rare Isotopes For Society
• Isotopes for medical research– Examples of isotopes projected to have demand much greater than supply: 47Sc, 62Zn,
64Cu, 67Cu, 68Ge, 149Tb, 153Gd, 168Ho, 177Lu, 188Re, 211At, 212Bi, 213Bi, 223Ra (DOE Isotope Workshop)
– -emitters 149Tb, 211At: potential treatment of metastatic cancer– Cancer therapy of hypoxic tumors based on 67Cu possible is a source would be available
• Nuclear power (nuclear data is needed to optimize reactor design)• Reaction rates important for stockpile stewardship and nuclear power –
related to astrophysics network calculations– Determination of extremely high neutron fluxes by activation analysis– Rare isotope samples for (n,g), (n,n’), (n,2n), (n,f) e.g. 88,89Zr
» Same technique important for astrophysics – More difficult cases studied via surrogate reactions (d,p), (3He, xn) …
• Tracers for Geology (32Si), Condensed Matter (8Li), material studies, …• Special isotopes for homeland security applications (β-delayed neutron
emitters to calibrate detectors, etc.)
Slid 13Brad Sherrill WG.9 July 2010, Slide 13
Available today
New territory to be explored with next-generation RIB facilities
The availability of rare isotopes over time
Nuclear Chart in 1966
Less than 1000known isotopes
about 3000 known isotopes
Slid 14Brad Sherrill WG.9 July 2010, Slide 14
What New Nuclides Will the Next Generation Facilities Produce?
• FRIB will produce more than 1000 NEW isotopes at useful rates (4500 available for study; compared to 1700 now)
• Theory is key to making the right measurements
• Exciting prospects for study of nuclei along the drip line to mass 120 (compared to 24)
• Production of most of the key nuclei for astrophysical modeling
• Harvesting of unusual isotopes for a wide range of applications Rates are available at http://groups.nscl.msu.edu/frib/rates/
Slid 15Brad Sherrill WG.9 July 2010, Slide 15
Rare Isotope Production Techniques using Accelerators
• Target spallation and fragmentation by light ions (Used by TRIUMF, HRIBF)
• Neutron or photon induced fission (TRIUMF)
• In-flight Separation following projectile fragmentation/fission (Used by FRIB)
beam
target
beam
target
Target/Ion SourcePost AccelerationAccelerator
Neutrons/PhotonsPost AccelerationAccelerator
Fragment Separator
Beam
Gas catcher/ solid catcher + ion source
Beams used without stopping
Post Acceleration
Accelerator
Slid 16Brad Sherrill WG.9 July 2010, Slide 16
Rare Isotope Facilities in North America
• Notre Dame University – in-flight light ions• Florida State RESOLUTE – in-flight light and mid-mass ions• Texas A&M Upgrade – ISOL, Gas Catcher, in-flight, accelerated to 50
MeV/u• ANL CARIBU – Cf fission source, in-flight light and mid-mass ions• ORNL HRIBF – ISOL production by 40 MeV light ions; fission
fragments• NSCL – 100 MeV/u in-flight ions• TRIUMF ISAC I and II, ARIEL – megawatt class photo fission source,
ISOL beams to 8 MeV/u• FRIB – 400 kW, 200 MeV/u in-flight separation, gas stopping,
reacceleration to 20 MeV/u
Slid 17Brad Sherrill WG.9 July 2010, Slide 17
RESOLUT: a newradioactive beam facility at FSU
In-flight production of radioactive beams in inverse kinematics Combination of Superconducting RF-Resonator with high acceptance
magnetic Spectrograph to create mass spectrometer
RF-ResonatorMagnetic Spectrograph
Target Position
RF-Resonator
Magnetic SpectrographSolenoid
2
Solenoid 1
Mass selectionslits
Production target
Experiment
Brad Sherrill WG.9 July 2010, Slide 18
Study of light exotic nuclei through resonance reactions at RESOLUT(G. Rogachev et al.)
Excitation function of elastic (top) to inelastic p+7Be scattering (bottom), showing the presence of additional resonances in 8B, observed throughinelastic scattering only
Excitation functions of elastic (top) to inelastic p+7Be scattering (bottom) at various angles, R-matrix fit fit with additional resonances included.
Slid 19Brad Sherrill WG.9 July 2010, Slide 19
T-REX[TAMU Reaccelerated Exotics]
Slid 20Brad Sherrill WG.9 July 2010, Slide 20
Science accessible with the TAMU upgrade
• Nuclear Astrophysics – indirect techniques
• Nuclear Structure – transfer reactions, g spectroscopy, …
• Fundamental Interactions – trapping expts.
• Dynamics and Thermodynamics – N/Z degrees of freedom
(p,n) Max. Energy Intensity
Product MeV/A particles/s27Si 57 6 x 103
50Mn 45 2 x 104
54Co 45 6 x 103
64Ga 45 4 x 104
92Tc 35 4 x 104
106In 28 4 x 104
108In 28 3 x 104
110In 26 6 x 104
Projected Beam Intensities from LIG after K500
Assuming 14 mA beam, realistic LIG, CBECR,transport and K500 extraction efficiencies
Brad Sherrill WG.9 July 2010, Slide 22
Examples of reaccelerated beams produced in DIC:
Isotope Max. Energy Intensity MeV/u Pps Neutron rich 9Li 45 1.7-3.4106 11Be 45 0.7-1.4106 22O 40 2.0-4. 2.0-4.0104 24Ne 40 0.5-1.0104 32Mg 40 1.3-2.6104 38S 36 2.5-5.0105 40S 32 0.5-1.0105 42S 29 1.8-3.6103 42Ar 39 3.3-6.6105 44Ar 38 0.9-1.8105 46Ar 35 1.8-3.6104 62Fe 38 1.9-3.8104 60Cr 32 0.5-1.0103 Proton rich
7Be 60 0.5-1.0106 8B 70 1.2-2.4106 11C 63 1.3-2.6106 14O 70 0.7-1.4105 22Mg 57 3.1-6.3104 23Al 60 1.2-2.4103 27P 62 1.0-2.0103 62Ga 47 2.1-4.3102 64Ga 45 0.9-1.9104
t1/2>100ms
Calculation details inposter by G. Souliotis
Slid 23Brad Sherrill WG.9 July 2010, Slide 23
CARIBUATLAS Energy
Upgrade
HELIOS
CARIBU gives access to exotic beams not available elsewhere. Physics with beams from CARIBU (1 & 2 nucleon transfer reactions) needs the new energy regime
opened by the Energy Upgrade (12 MeV/u) . Solenoid Spectrometer greatly expands the effectiveness of both the fission fragment beams and the
existing in-flight RIB program at these higher energies. These three projects combine to form a truly unique facility which complements the capabilities of
other world facilities in the era leading to FRIB
ATLAS Tomorrow: CARIBU & Energy Upgrade & HELIOS: Unique Synergy
CARIBU upgrade
Slid 24Brad Sherrill WG.9 July 2010, Slide 24
CARIBU
• CARIBU Plan:
Spring 2010: 2 mCi source tests & yields studies
Summer-Fall 2010: 100 mCi source 1st test expts.
End 2010: 1 Ci source Full research program
CARIBU upgrade
Slid 25Brad Sherrill WG.9 July 2010, Slide 25
- Astrophysics: towards the r-process pathPath critically depends on nuclear properties of neutron-rich nuclei:
mass, lifetime, b-delayed neutrons, fissionabilitycontinuation of CPT program, Greatly benefits from even the weakest source and requires > 0.1 ion/s
- Nuclear Structure: Changes in shell structure and new collective modes:
- Reaction dynamics Fusion with n-rich nuclei Deep inelastic reactions Surrogate reactions
CARIBU: Main Science Focus
Shell structure with single-nucleon transfer Pair correlations with transfer of nucleon pairs Collective modes with Coulomb Excitation and decay studies
All marked nuclei accessible with 80 mCi source
All but about half of the grey nuclei are accessible with 2.5 mCi source
CPT moved to CARIBU
Decay studies with X-array & tape system
N ew CPT/O ld CPTM easurem ents
N ew CPT/O ld CPTM easurem ents
CARIBU enables the initial exploration of the heavy neutron-rich region using precision low-energy transfer reactions and helps develop and test the required techniques
HELIOS & other techniques (GS&FMA,..)
Coulomb excitation & decay studies will address issues such as octupole collectivity in the Kr and Ba regions, triaxiality in the neutron-rich Mo and Pd regions, shape coexistence and new symmetries in Sr and Ce regions
Gammasphere & FMA, GRETINA, CHICO,..
26 Managed by UT-Battellefor the U.S. Department of Energy
Recoil Mass Spectrometer (RMS)
Injector for Radioactive Ion Species 1 (IRIS1)
25MV Tandem Electrostatic Accelerator
Daresbury Recoil Separator (DRS)
Oak Ridge Isochronous Cyclotron (ORIC)
On-Line Test Facility (OLTF)
High Power Target Laboratory (HPTL)
Injector for Stable Ion Species (ISIS)
Enge Spectrograph
HRIBF
27 Managed by UT-Battellefor the U.S. Department of Energy
HRIBF Post-accelerated Beams
175 RIB species available (+26 more unaccelerated)32 proton-rich species143 neutron-rich species
Post-accelerated Intensity
Beam list increased by ~50% since 2003
Slid 28Brad Sherrill WG.9 July 2010, Slide 28
Science highlights in 2009/2010
HRIBF General public highlights:http://www.phy.ornl.gov/hribf/science/abc/2009/
Experiments and outcomeshttp://www.phy.ornl.gov/hribf/experiments/results/
The magic nature of 132Sn explored through the single-particle states of 133Sn
K. L. Jones et al., Nature, May 27 (2010)(discussed by Jones)
Brad Sherrill WG.9 July 2010, Slide 29
Brad Sherrill WG.9 July 2010, Slide 30
Brad Sherrill WG.9 July 2010, Slide 31
208Pb
132Sn
78Ni
Evolution of shell structure: towards the r process path
Halo nuclei and neutron skin
10 μA of 500 MeV protons on 238U (22 g/cm2)Fundamental Symmetries Radon EDM, Fr PNC
Initial tests completed in Aug 2008, expect license for routine operation by fall 2010
Brad Sherrill WG.9 July 2010, Slide 32
Present status of the Ariel Project
• 50 MeV, 500 kW superconducting e-linac funded
• requires matching funding from BC province for buildings (funded)
• second proton beamline deferred until next 5YP
Brad Sherrill WG.9 July 2010, Slide 33
132Sn
78Ni
Evolution of shell structure: towards the r process path
Photo-fission of 238U (7 g/cm2)
10 mA, 50 MeV electrons on Hg converter
High yields and fewer isobaric contaminants
NuSTAR B.M Sherrill, 3/5/2010, Slide 34
Rare Isotope Beam Production – Coupled Cyclotron Facility, CCF
A1900Morrissey et al., NIM B 204, 90 (2003)
K500
K1200
A1900
ECR ion sources
A1900 Parameters• Dp/p ~5% max• Br = 6.0 Tm max• 8 msr solid angle• 35 m in length
CCF Parameters• 90 to 200 MeV/u• 1 pnA 238U• 80 pnA 48Ca
NuSTAR B.M Sherrill, 3/5/2010, Slide 35
Exotic Beams Produced at NSCL
More than 1000 RIBs have been made – morethan 830 RIBs have been used in experiments
12 Hours for a primary beam change; 3 to 12 hours for a secondary beam
Slid 36Brad Sherrill WG.9 July 2010, Slide 36
Facility for Rare Isotope Beams, FRIB Broad Overview
• Driver linac capable of E/A 200 MeV for all ions, Pbeam 400 kW
• Early date for completion is in 2018• In-flight 200 MeV/u, stopped, reaccelerated to 20 MeV/u LBNL
Slid 37Brad Sherrill WG.9 July 2010, Slide 37
Compact, more cost-effective solution
Project Manager: Thomas GlasmacherDirector: Konrad GelbkeTPC estimate $614MCD-4 Range 2018-2020
Slid 38Brad Sherrill WG.9 July 2010, Slide 38
Summary
• We have entered the age of designer atoms – new tool for science• High power in-flight facility at FRIB and ISOL facilities at TRIUMF
will allow production of a wide range of new isotopes– Necessary for the next steps in accurate modeling of atomic nuclei– Necessary for progress in astronomy (chemical history, mechanisms of
stellar explosions)– Opportunities for the tests of fundamental symmetries– Important component of a future U.S. isotopes program
• Other facilities play a key role in cost effective development of programs and techniques, e.g., ANC method developed at Texas A&M and resonance methods being developed at FSU
• New applications range from nuclear modeling, astrophysics, fundamental interactions, and use of isotope
Slid 39Brad Sherrill WG.9 July 2010, Slide 39
FRIB specialty – Produce new exotic isotopes
208Pb
11Li
80Ni
•Large neutron skins•Modified mean field•Resonance properties
New
r
V(r)
Science: Pairing in low-density material, new tests of nuclear models, open quantum system, interaction with continuum states - Efimov States - Reactions
Slid 40Brad Sherrill WG.9 July 2010, Slide 40
How do we model nuclei?
• The origin of the strong force that binds nuclei is QCD. How would we prove that? Surprises are likely.
• We construct potentials based on neutron and proton scattering data and properties of light nuclei (Bonn, Reid, Illinois AV18, Nijmegen, etc.)
• QCD Inspired EFT (String Theory Inspired – Hashimoto et al.)
S Aoki
Goal: Develop an Effective Field Theory based on QCD Symmetries(Furnstahl, van Kolck, Navrátil, Vary, Machliedt…)
Slid 41Brad Sherrill WG.9 July 2010, Slide 41
Properties of exotic isotopes are essential in determining NN and NNN potentials
• Neutron rich nuclei were key in determining the isospin dependence of 3-body forces and the development of IL-2R from UIX
• New data on exotic nuclei continues to lead to refinements in the interactions
• EFT developments, LQCD and even computational power are providing insight for ab initio theories, but they need grounding in data
S. Pieper B.Wiringa, et al.
Slid 42Brad Sherrill WG.9 July 2010, Slide 42
Current status of the GFMC calculations
FRIB Theory workshop talks of J. Carlson, K. Nollet
Slid 43Brad Sherrill WG.9 July 2010, Slide 43
Configuration space models – Example Coupled Cluster
Thomas Papenbrock et al. Univ of Tennessee, FRIB Theory Workshop
Slid 44Brad Sherrill WG.9 July 2010, Slide 44
Solar System Elemental Abundances
• Understanding the chemical history of the universe• The abundance of elements tell us about the history of events prior to
stellar formation
Lodders (2003)
Solar system abundances
Slid 45Brad Sherrill WG.9 July 2010, Slide 45
Simulation of Solar System Abundances
Timmes, Woosley, Weaver Astrophysical Journal 1995
Success ! ? Above 72 we can’t model well
Parameters: • Supernovae type Ia and
II• Number (77 supernovae
with Ms 11-40 Msun)• Progenitor mass
distributions• Age of the galaxy• …Results:• SN rate1/3 comes from
type Ia • Reproduction of
measured 7Li abundance metalicity vs. time etc.
Slid 46Brad Sherrill WG.9 July 2010, Slide 46
Goal: Understanding of Astrophysical Environments
• Use observational data to infer conditions at the site by modeling
• Accurate modeling requires • that we make the same isotopes
that participate in astrophysical environments
• reproduce the nuclear reactions that occur in those environments
• The hard part is that nature produces isotopes in environments like the r-process with T > 109 K, rneutron ≈ 1020-28 cm-3
Price & Rosswog 2006
n-star mergers
Sneden 2003; Cowan 2006
Mt Palomar
CrabNebula
observationmodel
Slid 47Brad Sherrill WG.9 July 2010, Slide 47
Where do gold atoms come 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, but …
• We know they must be made in a neutron-rich environment T > 109 K, rneutron ≈ 1020-28 cm-3 , that lasts for about 1 second; called the rapid-neutron capture process, r-process
• Type II supernovae are a possible site (variants)– Neutrino driven shock wave– 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
Slid 48Brad Sherrill WG.9 July 2010, Slide 48
About Half of Heavier Elements must be made in an r-Process
Nuclear physics shapes the characteristic final abundance pattern for a given r-process model
(Click on image to start animation)
Slid 49Brad Sherrill WG.9 July 2010, Slide 49
100 120 140 160 180 200 22010 -4
10 -3
10 -2
10 -1
100
101Nuclear physics
Hot bubbleClassical model
Same nuclear physics
ETFSI-Q massesETFSI-1 masses
Mass number Mass number
Freiburghaus et al. 1999
Astrophysics
10-4
10-3
10-2
10-1
100
101
Same (classical) r-process model
Uncertainty between models and nuclear properties
Abu
ndan
ce
Slid 50Brad Sherrill WG.9 July 2010, Slide 50
Mass Uncertainties and r-process
• Are the fine details a reflection of the site or of nuclear physics?
• “Site independent model” – Fe seed nuclei are irradiated with ≈ 20 flashes of 1020 to 1028 n/cm3 over a time scale of seconds (T ≈ 1 GK)
B. Sun et al. PRC 78 025806 (2008)
Slid 51Brad Sherrill WG.9 July 2010, Slide 51
126
Known half-life
NSCL reachFirst experiments
28
50
82
82
50
FRIB reachfor (d,p)
• β-decay properties• masses (Trap +
TOF)• (d,p) to constrain
(n,γ)• fission barriers,
yields
(66) Dy
(68) Er
(70) YbRISACKey Nuclei
(67) Ho
(69) Tm
FutureReach
N=126
FRIB reach forhalf-lives
Reach of FRIB – Will Allow Modeling of the r-Process
Current reach
Slid 52Brad Sherrill WG.9 July 2010, Slide 52
Type I-X ray bursts
http://plus.maths.org/issue23/news/xray/index.html
Slid 53Brad Sherrill WG.9 July 2010, Slide 53
Rare Isotope Crusts of Accreting Neutron Stars
Nuclear reactions in the crust set thermal properties
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…)
Cackett et al. 2006 (Chandra, XMM-Newton)
KS 1731-260(Chandra)
Slid 54Brad Sherrill WG.9 July 2010, Slide 54
XH=0.661
2
erg/
g/s/
1e17
XH=0.55
XH=0.29 Fix one key parameter (more meaningful model comparisons)
Determine Eddington Luminosity (apparent Ledd from PRE bursts) Standard candle/distance
Constrain EOS model atmosphere in transients
Mass uncertaintieswithin AME95(Brown et al. 2002)
New trap mass measurementsSchury et al. 2007 (LEBIT)Rodriguez et al. 2004 (ISOLTRAP)Clark et al. 2004, 2007 (CPT)
Lum
inos
ity (e
rg/g
/s)
Time (s)
H-fraction in surface from X-ray burst light curves
Mass uncertainties in 64Ge – 74Sr region:
H. Schatz, Brown 2002, Schatz 2001
Slid 55Brad Sherrill WG.9 July 2010, Slide 55
Rare Isotopes For Society
• Isotopes for medical research– Examples: 47Sc, 62Zn, 64Cu, 67Cu, 68Ge, 149Tb, 153Gd, 168Ho, 177Lu, 188Re, 211At, 212Bi, 213Bi,
223Ra (DOE Isotope Workshop)– -emitters 149Tb, 211At: potential treatment of metastatic cancer– Cancer therapy of hypoxic tumors based on 67Cu possible is a source would be
available
• Reaction rates important for stockpile stewardship and nuclear power – related to astrophysics network calculations– Determination of extremely high neutron fluxes by activation analysis– Rare isotope samples for (n,g), (n,n’), (n,2n), (n,f) e.g. 88,89Zr
» Same technique important for astrophysics – More difficult cases studied via surrogate reactions (d,p), (3He, xn) …
• Tracers for Geology (32Si), Condensed Matter (8Li), material studies, …• Special isotopes for homeland security applications (β-delayed neutron
emitters to calibrate detectors, etc.)
Slid 56Brad Sherrill WG.9 July 2010, Slide 56
Separated Isotopes from FRIB
Half-life limit set at 1 minute
Slid 57Brad Sherrill WG.9 July 2010, Slide 57
DOE Workshop Report Appendix HIsotopes with Future Demand > Supply
Isotope FRIB mCi (4 hour) Comment
Actinium-225 0.063 Significant gain from ISOL capability
Promethium-147 1x1014 atoms
Astatine-211 3.5 100 gain from ISOL capability
Nickel-63 1x1016 atoms
Chlorine-36 1x1016 atoms
Cesium-137 1x1013 1000 gain if ISOL used
Gallium-68 1310 Additional alternative Ga isotopes
Iridium-192 1x1014 atoms
Copper-67 750 Additional alternative Cu isotopes
Silicon-32 1x1016 atoms
http://www.er.doe.gov/np/program/isotope.html
Slid 58Brad Sherrill WG.9 July 2010, Slide 58
Sensitivity of Nuclear Properties to Model Parameters
• Example: Level structure of 24O and the 1S0 NN interaction• Structure of these loosely bound or unbound isotopes is strongly
influenced by the 1S0 component of the NN interaction• Calculation of 24O in a shell model that correctly treats weakly-bound
and continuum states (specifically Gamow Shell Model)
Tsukiyama, Horth-Jensen, Hagen PRC 80 051301(2009)
Slid 59Brad Sherrill WG.9 July 2010, Slide 59
How do we know QCD is responsible for nuclei?
• Lattice QCD has the promise to verify QCD as the correct description for the strong force in nuclei
• The lattice may be able to provide the isospin dependence of the NNN force needed to understand nuclei
• Comparison of this dependence to rare isotope data allows a test of lattice QCD in nuclei
T. Otsuka Accepted PRLNNN force may be the solution to understanding the Oxygen drip line
ExperimentTheory
Slid 60Brad Sherrill WG.9 July 2010, Slide 60
FRIB Users www.fribusers.org
• FRIB Equipment Workshop held Feb. 20-22, 2010 in East Lansing– 265 registered participants from
76 institutions in 15 countries– 18 working groups held sessions
and presented summaries– SAC report released (see website)– meetings.nscl.msu.edu/frib-equipment-workshop2010/program.htm
Prior workshop held May 30-31, 2009 at Argonne National Laboratory• “Step Forward to FRIB"• 210 registered participants from
47 institutions in 11 countries• www.fribusers.org/4_GATHERINGS/4_ARCHIVE/05_09/05_09.html
Slid 61Brad Sherrill WG.9 July 2010, Slide 61
Density Functional Theory
• EDF calculation of the binding energies of 9000 isotopes (M. Stoitsov et al.)
• Key tests of the theory come at the limits of binding (see figure)
• Remarkable success so far; Global DFT mass calculations from HFB Δm~700keV
• Goal is to achieve the kind of results obtained in quantum chemistry
M. Stoitsov et al.
Slid 62Brad Sherrill WG.9 July 2010, Slide 62
World view of rare isotope facilities
Black – production in targetMagenta – in-flight production