Nuclear PhysicsyQuestions, Directions, Applications

Science Questions & Goals of Nuclear PhysicsScience Questions & Goals of Nuclear PhysicsImplications of Nuclear Physics for other FieldsApplications of Nuclear Physics in other Fieldspp y

h N l hThe Nuclear ChartProton: 2 up, 1 down quarkProton: 2 up, 1 down quarkp, qp, qNeutron: 2 down, one up quarkNeutron: 2 down, one up quarkGluons: quark antiquark Gluons: quark antiquark

Nucleus as few body system interacting through Nucleus as few body system, interacting through the strong, weak, and electromagnetic forces!

Implications for: Astrophysics, Particle physics,Mesoscopic physics, Condensed matter physics

Applications in: Medicine, Material Science, Artand Archaeology, Geology and Climatology,Energy Production, Defense, Nuclear Forensics

Science Goals in Nuclear PhysicsQ k S f N lQuark Structure of Nucleon

Quark gluon plasma NP ScienceQuark gluon plasma

Nuclear Structure

NP Science

Nuclear Astrophysics

Fundamental StudiesNP Implications

Nuclear Physics Applications

QCD and the Structure of Hadrons

The research aspect focuses on the use of the electromagneticinteraction to probe the structure of nucleons, few-nucleonsystems and complex nucleisystems, and complex nuclei.

Quark structure & distribution in nucleons

Quark confinement in nucleonsQuark confinement in nucleons

Quark-gluon origin of nuclear spin(spin direction of up and down quarks)

Ch di ib i f hCharge distribution of the neutron(positive core and negative pion cloud)

Present facilities JLab, USADesy, Germany, Mami GermanyMami, GermanyJ-Parc, Japan

QCD h t iti i

Phases of Nuclear Matter

QCD phase transitions innuclear matter from quarkstructure of nuclei to quarkqgluon plasma. (from quark gluonliquid to quark gluon gas)

Measurements performedby the study of Relativisticby the study of RelativisticHeavy Ion Collisions: RHIC

Collision creates the conditions ofthe early universe in a split second!

A li h i Accomplishments in Quark Gluon Plasmas

Starting the Relativistic Heavy Ion Collider program with BRAHMS, PHENIX, PHOBOS, and STAR

The quark gluon liquid or quark-gluon glassq g q q g g

Jet production in collision experimentsp p

Lattice QCD calculations for QCD matterLattice QCD calculations for QCD matter

nucleons ⇒ quarks

F G l & EffUp-grade of PHENIX & STAR

Future Goals & Efforts

Increase of RHIC luminosity

US participation in heavy ion program at LHC at CERN withprogram at LHC at CERN with the detectors ALICE

Relativistic heavy ion beam yexperiments at FAIR/GSI

LHC Accelerator at CERN

N l St tNuclear StructureFrom collective modes of excitation toprobe the quantum structure and meanprobe the quantum structure and meanfield model descriptions of the nucleus,

halo nucleusto the study of drip-line behavior of thenucleus at the limits of stability; fromstructure of halo to super-heavy nuclei!

superheavy nucleus

structure of halo to super-heavy nuclei!

Nuclear StructureAccomplishments

R d V b f L d DRotations and Vibrations of a Liquid DropBreathing Mode g

Squeezing Mode

M f ff b lMatter far off StabilityNuclear Masses & decay propertiesNeutron halosDisappearance of shell structureEmergence of new shapes New collective modes of excitationMapping the driplinesIslands of stability

Accelerator Probes5 id i i it f ilitiUnited States5 midsize university facilitiesFSU, ND, TUNL, UoW, Yale2 large university facilities, TAMU, NSCL/MSU ,2 national laboratory facilitiesATLAS/ANL, HIBRF/ORNL

International Community

CCF/NSCL/MSU

HRIBF/ORNL

International CommunitySeveral universitiesGANIL, FranceGSI, Germany

GSI, Germany

INFN Legnaro, Italyi-Themba, South AfricaLanzhou, ChinaRCNP Osaka JapanRCNP Osaka, JapanRIKEN, JapanSaha Institute, IndiaISAC TRIUMF, Canada

RCNP, Japan

Future FacilitiesRIKEN, Japan (2008)

GSI/FAIR Germany (2015)

GANIL, France (2013)

FRIB at MSU

Construction has started, completion is scheduled for 2016

Neutrino Physics AccomplishmentsLast decade opened new era of nuclear physics,the study of low energy neutrinos from sun and supernova and in laboratory decay1998 Super Kamiokande (light water Cherenkov detector)1998 Super Kamiokande (light water Cherenkov detector) announces evidence for neutrino oscillations which indicates that neutrinos have mass (0.05 – 0.18 eV)

2001 SNO (heavy water Cherenkov detector) confirmed2001 SNO (heavy water Cherenkov detector) confirmed neutrino oscillations and solves solar neutrino problem by detecting neutrinos consistent with predicted decay rate of 8B in the 3rd pp-chain

2003 KamLAND (liquid scintillator detector) confirmed neutrino oscillation from terrestrial neutrino source (reactor) and showed oscillation pattern

2007 Borexino (liquid scintillator detector) at Gran Sasso detects low energy solar neutrinos consistent with the predicted electron capture rate of 7Be in 2nd pp chain.

Fundamental SymmetriesStandard Model Initiative

KATRIN

Standard Model Initiative

What are the neutrino masses?Tritium decay measurements with KATRIN CUORETritium decay measurements with KATRIN

Are neutrinos their own antiparticles?Neutrino less double beta decay measurementsI b k d f d d i t

MAJORANA CUORE76Ge

In background free underground environments(Gran Sasso, SNO, WIPP, ...)

Violation of CP symmetry (matter anti-matter

130Te

balance) by neutrino oscillation experimentsand neutron EDM measurements (ultra-cold neutrons at Los Alamos, SNS, PSI, TRIUMF ...)

Neutrin Physics Under r undNeutrino Physics Underground

designed for experiments that require extremely low cosmogenic backgrounds: in particular, the search for neutrino-less double beta decay and relic dark matter.

N l hUnderstanding nuclear processes at

Nuclear Astrophysics

the extreme temperature & density conditions of stellar environments!

Stellar matterStellar explosionsWhite Dwarf matterNeutron Star matterQuark Star matter

Field req ires close comm nication bet eenField requires close communication betweennuclear experimentalists, theorists, stellarmodelers and stellar observers (astronomers)

Nuclei are made in StarsNuclei are made in Stars

time

Measurements of solar reaction rates at LUNA, Gran Sasso within Gamow window of solar core temperature

Mapping the s-process at ORELA, LANSCE, n-ToF. Model simulations for AGB stars.

Probing reactions and decays farProbing reactions and decays far off stability for r- and rp-process at HRIBF and NSCL for supernovae and cataclysmic binariesand cataclysmic binaries.

Observation of r-process signatures in metal poor (old) halo stars

26Al 60Fe

p ( )

Mapping Galactic RadioactivityMapping Galactic Radioactivity with gamma ray satellites

Astrophysics undergroundAstrophysics undergroundNuclear Reactions at stellar temperatures

Timescale of stellar evolutionStellar energy productionNucleosynthesis from He to Fe Seed production for explosive nucleosynthesisNeutron production for trans-Fe elements

DIANA - two-Acceleratorlaboratory at DUSEL atNeutron production for trans Fe elements

Solar neutrino production the 4850 ft depth level.

Measurements handicapped by Cosmic Ray background

A h i f ff S biliAstrophysics far off StabilityStudy of nuclear reaction and decay processes far off stability for r- ν- rp- νp and p-process in cataclysmicstability for r , ν , rp , νp, and p process in cataclysmic binaries and/or supernova shock environments

Measurements at RIB facilities

FRIB reachFRIB reach

I t ti l Sit tiInternational SituationRoadmap for existing and planned underground laboratories with the size of the box corresponding to the relative space for experiments at each depth. These facilities are p g p p ptypically shared or primarily funded by other disciplines such as particle astrophysics.

Nuclear Physics World WideNuclear Physics World Wide