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Nuclei as Laboratories: Nuclear Tests of Fundamental Symmetries M.J. Ramsey-Musolf N. Bell V. Cirigliano J. Erler B. Holstein A. Kurylov C. Lee C. Maekawa S. Page G. Prezeau S. Profumo S. Tulin B. Van Kolck P. Vogel S. Zhu Nuclear Science Cosmic Energy Budget Dark Matter Baryons Dark Energy The mission: Explain the origin, evolution, and structure of the baryonic matter of the Universe Nuclear Science Cosmic Energy Budget Dark Matter Baryons Three frontiers: Dark Energy • Fundamental symmetries & neutrinos • Nuclei and nuclear astrophysics • QCD Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Electroweak symmetry Standard Model “unfinished business” breaking: Higgs ? How does QCD affect the weak qq interaction? Is there a long range weak NN interaction? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Electroweak symmetry Puzzles the Standard Model can’t solve breaking: Higgs ? 1. 2. 3. 4. Origin of matter Unification & gravity Weak scale stability Neutrinos Beyond the SM What are the symmetries (forces) of the early universe beyond those of the SM? SM symmetry (broken) What are the new fundamental symmetries? • Why is there more matter than antimatter in the present universe? Electric dipole moment searches • What are the unseen forces that disappeared from view as the universe cooled? Precision electroweak: weak decays, scattering, LFV • What are the masses of neutrinos and how have they shaped the evolution of the universe? Neutrino oscillations, 0nbb-decay, q13 , … Tribble report What is the origin of baryonic matter ? Cosmic Energy Budget E d dS Dark Matter Baryons n EDM B (7.3 2.5) 1011 YB s (9.2 1.1) 1011 BBN WMAP Dark Energy dS E h T-odd , CP-odd by CPT theorem What are the Searches for permanent quantitativeelectric implications dipoleof new moments EDM experiments (EDMs) of forthe explaining neutron,the electron, origin of andbaryonic the neutral atoms component probe of new theCP-violation Universe ? What is the origin of baryonic matter? Electroweak symmetry breaking: Higgs ? Baryogenesis: When? SUSY? Neutrinos? CPV? Weak scale baryogenesis can be tested by exp’t If ruled out: more speculative ideas (n’s) ? ? Beyond the SM SM symmetry (broken) Cosmic Energy Budget EW Baryogenesis: Standard Model Sakharov: Weak Scale Baryogenesis Anomalous Processes • B violation • C & CP violation J B • Nonequilibrium dynamics A qL Sakharov, 1967 W W Different vacua: D(B+L)= DNCS Kuzmin, Rubakov, Shaposhnikov McLerran,… Sphaleron Transitions EW Baryogenesis: Standard Model Shaposhnikov 2 J s12 s13 s23 c12 c13 c 23 sin 13 (2.88 0.33) 105 Weak Scale Baryogenesis mt4 mb4 mc2 ms2 13 3 10 MW4 MW4 MW2 MW2 • B violation • C & CP violation • Nonequilibrium dynamics F F 1st order 2nd order Sakharov, 1967 • CP-violation too weak • EW PT too weak Increasing mh Baryogenesis: New Electroweak Physics 90’s: Weak Scale Baryogenesis • B violation Cohen, Kaplan, Nelson Joyce, Prokopec, Turok Unbroken phase Topological transitions new • C & CP violation • Nonequilibrium dynamics (x) Broken phase 1st order phase transition CP Violation Sakharov, 1967 new • Is it viable? • Can experiment constrain it? • How reliably can we compute it? new new e EDM Probes of New CP Violation CKM f dSM dexp dfuture e 1040 1.6 1027 1031 n 1030 6.3 1026 1029 Hg 1033 2.11028 1032 1028 1.11018 1024 199 Also 225Ra, 129Xe, d If new EWK CP violation is responsible for abundance If an EDM is seen, can we identify the new physics? of matter, will these experiments see an EDM? EDM constraints & SUSY CPV Lee et al (x) new • BBN WMAP de EDMs of different systems provide Acomplementary probes: more A 199Hg atomic experiments (RIA) de 199Hg • Nuclear theory: reliable calc’s BAUEDM dependence of atomic on CPV and other new physics parameters (RIA?) BAU new new • Nuclear theory: reliable calcs of YB Different choices for SUSY parameters new e Fundamental Symmetries & Cosmic History Electroweak symmetry? Unseen Forces: Supersymmetry breaking: Higgs ? 1. 2. 3. 4. Unification & gravity Weak scale stability Origin of matter Neutrinos n ˜ n ne W ˜0 ˜ e Beyond the SM SM symmetry (broken) Weak decays & new physics R Parity Violation R-M, V Flavor-blind dSu VKurylov, VSUSY- d u e ne ud us breaking u c t Vcd V MW td s u e ne b u e ne n ne ne O ~ 0.001 SM 12k 12k ˜ n p e ne e n O b-decay e˜ ˜ n ˜ 0 e SUSY k W R nd ene n ˜e e n e ˜ e 0 j L ˜ n 1j1 A(Z,N)q˜ A(Z 1,N 1) e n e ˜0 1j1 e d CKM unitarity ? ub Vcs Vcb s CKM Unitarity Vts Vtb b CKM, (g-2), MW, Mt ,… b F F APV l2 G Vud 1 Drb Dr G M˜ L Mq˜ L Kurylov, No long-lived LSPNew or SUSY physics DMR-M SUSY RPV b-decay Weak decays b F F G Vud 1 Drb Dr G n p e ne A(Z,N) A(Z 1,N 1) e n e 0 e n e SM theory input A(Z 1,N p 1) ne W n A(Z,N) Recent Marciano Nuclear structure & effects? Sirlin e MW ˆ M Z2 GF ln 2 CW () 2 2 Weak decays & new physics d u e ne u s u e ne b u e ne n ˜ n W ˜0 ne u˜ d Vus Vub d Vcs Vcb s Vts Vtb b pe pn pe dW 1 a An E e En Ee ˜0 u ˜ O ~ 0.001 SM O e SUSY c Vud t Vcd Vtd Correlations ne n ˜e ˜ e SUSY Non (V-A) x (V-A) interactions: me/E b-decay at RIA? Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Are they their own antiparticles? LFV & LNV ? Why are their masses so small? What is mn? Can they have magnetic moments? Implications of mn for neutrino interactions ? Neutrinos ? Beyond the SM SM symmetry (broken) 0nbb - decay probes the charge conjugation properties of the neutrino e e W e e e nM AZ,N AZ,N u W AZ 2,N 2 AZ 2,N 2 e nM W W d d u e e Light nM : Nuclear matrix difficult to elements 0 compute ˜ e u e˜ u EFF 2 2i mn d U ek mk e k d 0nbb - decay: heavy particle exchange e e e AZ,N u AZ 2,N 2 W e u How do we compute & separate exchange effects? heavy particle nM W d e e˜ d e 0 e˜ d u d u LF and LN: symmetries of the early universe? Lepton flavor: “accidental” Electroweak symmetry symmetry of the SM breaking: Higgs ? LFV initimately connected with LNV in most models R= e MEG: B!e ~ 5 x 10-14 B!e ? B!e AZ,N e AZ,N MECO: B!e ~ 5 x 10-17 Beyond the SM SM symmetry (broken) Also PRIME LF and LN: symmetries of the early universe? 0nbbdecay e Electroweak symmetry breaking: Higgs ? e nM W u W u d d MEG: B ~ 5 x 10-14 !e ? ?Light nM exchange ˜ n e * D e e e * Logarithmic enhancements of R Beyond the SM Low scale LFV: R ~ O(1) u AZ,N e e e e e e˜ e 0 d e˜ u AZ,N d -17 MECO: B !e ~ 5x 10 Heavy particle exchange ? SM symmetry (broken) Also PRIME GUT scale LFV: R ~ O 0nbb - decay: heavy particle exchange How do we compute & separate heavy particle exchange effects? e e u d AZ,N e e e u u AZ 2,Nd 2 e u W 4 quark operator, as in hadronic PV nM W d e e˜ d e 0 e˜ d u d u 0nbb - decay: effective field theory We have a clear separation of scales bb kF L-violating new physics Non-perturbative QCD Nuclear dynamics 0nbb - decay in effective field theory Operator classification L(q,e) MWEAK ! L,N,e M HAD Spacetime & chiral transformation properties 0nbb - decay in effective field theory Operator classification L(q,e) = e.g. GF2 bb MWEAK 14 c ˆ C ( ) O e e j j j j1 ab a b ˆ O1 qL qL qR qR 0nbb - decay: a = b = + h.c. 0nbb - decay in effective field theory Operator classification MWEAK ab a b ˆ O1 qL qL qR qR Chiral transformations: SU(2)L x SU(2)R qL LqL qR RqR expiqL PL R R 2 R L Oˆ1ab (3L , 3R ) Parity transformations: qL $ qR 0nbb - decay: a = b = + ˆ O ˆ O 1 1 0nbb - decay in effective field theory e e e e e e N N K p 2 N N 1 K NN p N N K NNNN p K O (p effects for -2) ,for 0) for 0 ), Enhanced 1 ), etc. ˆ ˆ O (p K KSystematic , can be O ( p O ( p operator classification O NNNN O NN 1 3 some models ? 0 An open question Is the power counting of operators sufficient to understand weak matrix elements in nuclei ? n g 9 2 2 n n Oˆ 0Lnbb p p p , f 32 76Ge 76Se 0, ,9 0, ,5 2 52 2 An open question Is the power counting of operators sufficient to understand weak matrix elements in nuclei ? L ˆ O0nbb 0, ,9 0, ,5 Oˆ 0Lnbb0 M fi ~ p2 0 2, 0 M fi ~ p2 0, 2 Oˆ 0Lnbb2 M fi ~ p 4 4, 0 L 4 ˆ O0nbb etc. naive M fi ~ p0 Oˆ 0Lnbb2 An open question Complications: • Bound state wavefunctions (e.g., h.o.) don’t obey simple power counting • Configuration mixing is important in heavy nuclei Is the power counting of operators sufficient to understand weak matrix elements in nuclei ? • More theoretical study required (RIA) • Hadronic PV may provide an empirical test Fundamental Symmetries & Cosmic History Electroweak symmetry Standard Model “unfinished business” breaking: Higgs ? How does QCD affect the weak qq interaction? Is there a long range weak NN interaction? Beyond the SM SM symmetry (broken) The weak qq force is short range W ,Z 0 q W,Z ~ 0.002 fm RCORE q Meson-exchange model , , N N Use parity-violation to filter out EM & strong interactions Seven PV mesonnucleon couplings h1 , h0,1,2 , h0,1, h1 Desplanques, Donoghue, &Holstein (DDH) Is the weak NN force short range ? , , N T=1 force N Long range: -exchange? Is the weak NN force short range ? , , N N b 0 ,0 0 ,1 T=1 force 1 ,0 18 F 18 0 ,1 Ne Analog 2-body matrix elements Model independent Is the weak NN force short range ? , , N N T=1 force Anapole moment Boulder, atomic PV 133 Cs h ~ 10 g Is the weak NN force short range ? , , N N • Problem with expt’s • Problem with nuc th’y • Problem with model T=1 force • No problem (1) EFT Hadronic PV: Effective Field Theory PV Potential Long Range Medium Range Short Range h1NN k 1a NN 1,2,3 s , t , t h1NN O(p-1) O(p) O(p) O(p) A program of few-body measurements Pionless theory Ab initio few-body calcs Done mN pp 1.22 AL (pp) LANSCE mN t 9.35 AL (np d ) HARD* mN pn 1.6 AL (pp) 3.7 AL (p ) 37 A (np d ) 2 P (np d ) mN t 0.4 AL (pp) 0.7 AL (p ) 7 A (np d ) P (np d ) d n mN nn 1.6 AL (pp) 0.7 AL (p ) 33.3 A (np d ) 1.08 P (np d ) 0.83 dz pp 0s 1s 2s 6 nn 0s 1s 2s 6 pn 0s 2 2s 6 NIST *HIGS AL d np A program of few-body measurements Complete determination of PV NN & NN interactions through O (p) Attempt to understand the i, h etc. from QCD Attempt to understand nuclear PV observables systematically Are the PV LEC’s “natural”? Does EFT power counting work in nuclei ? Hadronic PV in n-rich nuclei ? Hadronic PV as a probe • Determine VPV through O (p) from PV low-energy few-body studies where power counting works O ( p -1 ) e • Re-analyze nuclear PV observables using this VPV O ( p) e e e e e we would have some •If successful, indication that operator power counting works in nuclei N N • Apply to 0nbb-decay N K p2 N K NN p1 N N K NNNN p 0 Conclusions • Nuclei provide unique and powerful laboratories in which to probe the fundamental symmetries of the early universe • RIA will provide opportunities to carry out new and complementary experiments whose impact can live on well into the LHC era • A number of theoretical challenges remain to be addressed at the level of field theory, QCD, and nuclear structure • New experimental and theoretical efforts in nuclear structure physics are a key component of this quest