nuclear physics at rare-isotope facilities in north-america

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


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


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– …


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.


Application of GFMC technique to reactions of nuclei

• Resonance states in 5He (n+4He)

Nollett, et al, PRL 2007; motivated by BBN modeling


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)


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


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


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


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


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


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.)


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


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/


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


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


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.


T-REX[TAMU Reaccelerated Exotics]


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


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


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


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


- 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


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)

http://www.phy.ornl.gov/hribf/science/abc/2009/


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


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


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


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


Compact, more cost-effective solution

Project Manager: Thomas GlasmacherDirector: Konrad GelbkeTPC estimate $614MCD-4 Range 2018-2020


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


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


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…)


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.


Current status of the GFMC calculations

FRIB Theory workshop talks of J. Carlson, K. Nollet


Configuration space models – Example Coupled Cluster

Thomas Papenbrock et al. Univ of Tennessee, FRIB Theory Workshop


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


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.


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


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


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)


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


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)


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


Type I-X ray bursts

http://plus.maths.org/issue23/news/xray/index.html


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)


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


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.)


Separated Isotopes from FRIB

Half-life limit set at 1 minute


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


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)


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


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

http://meetings.nscl.msu.edu/frib-equipment-workshop2010/program.htm



http://www.fribusers.org/4_GATHERINGS/4_ARCHIVE/05_09/05_09.html




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.


World view of rare isotope facilities

Black – production in targetMagenta – in-flight production

nuclear physics at rare-isotope facilities in north-america

Documents

exotic nuclei

light nuclei

predictive model of

brad sherrill wg

body forces

properties of rare isotopes

nuclear processes

decays of nuclei halo