Transcript Document
Future Directions in Parity Violation: From Quarks to the Cosmos M.J. Ramsey-Musolf + many students, postdocs, collaborators, and colleagues PAVI ‘06 MHLOS Fundamental Symmetries & Cosmic History What are the fundamental symmetries that have governed the microphysics of the evolving universe? • Parity violation as a probe of the proton’s internal structure (sea quarks, twist) • Parity violation as probe of the hadronic weak interaction • Parity violation as a probe of additional symmetries of the early universe Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Electroweak symmetry SMHiggs “unfinished business”: breaking: ? What is the internal landscape of the proton? Sea quarks, gluons, & qq, qqg correllations Beyond the SM SM symmetry (broken) Probing the strange sea with PV GMs = 0.28 +/- 0.20 Not surprising: ms / Lc ~ 0.15 Challenge for lattice: Unquenched, light chiral quarks Preliminary World Data 4/24/06 GEs = -0.006 +/- 0.016 ~3% +/- 2.3% of proton magnetic moment ~20% +/- 15% of isoscalar magnetic moment ~0.2 +/- 0.5% of Electric distribution Consistent with s-quark contributions to mP & JP but smaller than early theoretical expectations Courtesy of Kent Pashke (U Mass) Probing Higher Twist: Beyond the Parton Model 2xF1 Experimental Status Alekhin NNLO MRST NNLO MRST NNLO with Barbieri Target Mass Corrections • Smooth transition from DIS (solid squares) to resonance region • Resonances oscillate about perturbative curves (quarkhadron duality in transverse channel) - all Q2 •Target mass corrections large and important ~ 50% fluctuations about leading twist Data from JLab E94-110 (nucl-ex/0410027, submitted to PRL) Courtesy C Keppel n = 2 Cornwall-Norton Moments F2 2xF1 FL F2, F1 in excellent agreement with NNLO + TM above Q2 = 2 GeV2 No (or canceling) higher twists Yet, dominated by large x and resonance region Remove known HT (a bit novel), the elastic, and there is no more down to Q2 = 0.5 GeV2 The case are looksthe different for Where qq and Fqqg or curve?) ? L (data correlations Probing Higher Twist with PV Looking PV Deepbeyond Ineslastic theeD parton (J Lab description 12 GeV) APV Q 2 Theoretical Challenges ~0.4% Different pQCD evolution of twist PDF fits four moments Lattice QCD for t =4 matrix elements y Organizing the program: what kinematics, complementarity E=11 GeV 0 with PC F1,2 , … q=12.5 Sacco, R-M preliminary Fundamental Symmetries & Cosmic History Electroweak symmetry business”: SM “unfinished breaking: Higgs ? How do weak interactions of hadrons reflect the weak qq force ? Are QCD symmetries (chiral, large NC,…) applicable? Is there a long range weak NN interaction? Beyond the SM SM symmetry (broken) Weak Interactions of Hadrons: Strange? Hyperon weak decays S n S p 0 S n L p L n 0 L 0 0 L 0 M B B UB A B 5 UB S-Wave: Parity-violating B Ll.o.WEAK dTrBh,B f TrBh,B P-Wave: Parity conserving B c symmetry not sufficient B B B B B B Weak Interactions of Hadrons: Strange? S p , L n , E1 (PV) i MB B U A B 5 U F MB MB Breaking of SU(3) sym M1 (PC) Are weak interactions of 2Re A B* ? s-quarks a “un-natural” Bare deeper B their 2 2 Or A HWI B puzzles with the involving all light flavors ? BB ~ ms L c ~ 0.15 S p ~ 0.76 0.08 S ~ 0.63 0.09 0 0 Th’y Exp’t Weak Interactions of S=0 Hadrons: Strange? Zhu, Puglia, Holstein, R-M W ,Z 0 q S=0 analog of BB’ : PV E1 N- transition q N A ~ 5 108 “natural” d PV Asymmetry Q2=0: Nonzero PVES: G0, QWEAK What does QCD predict ? d mN A 2 V C3 L c A ~ 1106 enhanced d Weak Interactions of S=0 Hadrons: Strange? W ,Z 0 q Nuclear effects: 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 ? h ~ 10 g , Cs , Anapole moment 133 Boulder, atomic PV N N h ~0 0 18 Long range: -exchange? Ne ,0 0 ,1 T=1 force 0 ,1 1 ,0 18 F Analog 2-body matrix elements Model independent 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 1,2,3 s , t , t h1NN O(p) O(p) O(p-1) O(p) Zhu, Maekawa, Holstein, R-M, van Kolck ‘05 Six constants to O(p) R-M & Page ‘06 One new O(p) constant PV Current Operators O(p-1) Long Range h1NN Hadronic PV: Effective Field Theory Medium Range Short Range C h1NN 1,2,3 s , t , t O(p) O(p) O(p) Hadronic PV: Few-Body Systems Pionless theory mN pp 1.22 AL (pp) Ab initio few-body calcs Done LANSCE, SNS 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 AL d np P nd t 0 1 2 6 pp s s s NIST,SNS A nd t AL pd nn 0s 1s 2s 6 d np New 2few-body Pionless th’y: 5 exp’ts 0 s calcs 2 sneeded 6 dzpn Dynamical pions: 7 exp’ts Hadronic PV: Theoretical Challenges 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” from QCD standpoint? Does EFT power counting work in nuclei ? Implications for 0-decay Hadronic PV & 0 - decay e e e AZ,N u AZ 2,N 2 How do we compute & separate exchange effects? heavy particle e M W W d u d e e Light M : 0-decay rate may 0 scale of yield c m e˜ u e˜ u EFF 2 m U ek mk e 2i d k d Hadronic PV & 0 - decay 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 M W d e e˜ d e c 0 e˜ d u d u 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 0-decay N K p2 N K NN p1 N N K NNNN p 0 Prezeau, R-M, & Vogel 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) PV as a Probe of New Symmetries 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 implications of m and PV expts for possible new symmetries & forces? SM symmetry (broken) PV as a Probe of New Symmetries Electroweak symmetry? Unseen Forces: Supersymmetry breaking: Higgs ? 1. 2. 3. 4. Unification & gravity Weak scale stability Origin of matter Neutrinos ˜ e W ˜0 c ˜ e Beyond the SM SM symmetry (broken) PV Correlations in Muon Decay & m 3/4 0 3/4 1 TWIST (TRIUMF) PV Correlations in Muon Decay & m Model Independent Analysis 0 0 H H H 0 e MPs constrained by m 1,2 m , and decay corr P e TWIST P W Also -decay, Higgs production e e m Erwin, Kile, Peng, R-M 06 Constraints on non-SM Higgs production at ILC: Model Dependent Analysis H0 Z,W Prezeau,Kurylov 05 2005 Global fit: Gagliardi et al. TWIST First row CKM P MWR (GeV) Weak decays & new physics R Parity Violation R-M, V Flavor-blind dSu VKurylov, VSUSY- d u e e ud us breaking u c t Vcd V MW td s u e e b u e e e e O c ~ 0.001 SM 12k 12k ˜ n p e e e O -decay e˜ ˜ ˜ 0 e SUSY k W R d ee ˜e e e ˜ c e 0 j L ˜ 1j1 A(Z,N)q˜ A(Z 1,N 1) e e ˜0 c 1j1 e d CKM unitarity ? ub Vcs Vcb s CKM Unitarity Vts Vtb b CKM, (g-2), MW, Mt ,… F F APV l2 G Vud 1 r r G M˜ L Mq˜ L Kurylov, No long-lived LSPNew or SUSY physics DMR-M SUSY RPV Weak decays & PV F F G Vud 1 r r G Ultra cold neutrons 58Ni coated stainless guide -decay n p e e A(Z,N) A(Z 1,N 1) e e 0 e e Lifetime & correlations Flapper valve Liquid N2 pe p pe dW 1 a An E e E Ee Be reflector LHe Solid D2 77 K poly UCN Detector Tungsten Target LANSCE: UCN “A” NIST, ILL: tn Future SNS: tn, a,b,A,… Future LANSCE: Correlations Weak decays & PV d u e e u s u e e b u e e ˜ W ˜0 c e u˜ d Vus Vub d Vcs Vcb s Vts Vtb b pe p ppe dW 1 a Bme Ee An n E e E EE e ˜0 c u ˜ O ~ 0.001 SM O e SUSY c Vud t Vcd Vtd e ˜e ˜ c e SUSY Non (V-A) x (V-A) interactions: me/E -decay at “RIAcino”? Weak decays & PV: Correlations Fierz int (current) -decay correlations QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. -decay hparameter Profumo, R-M, Tulin PV w/ radioactive isotopes ? GF from t Probing SUSY with PV eN Interactions e Z SUSY dark matter e 0 ˜ c Z0 f c SUSY loops ˜ e˜ e f e e˜ f f c0 -> QuickTime™ and a TIFF (Uncompressed) e+e decompressor are needed to see this picture. is Majorana e e ˜ Rk e RPV 95% CL fit to 12k decays, M ,etc. 12k weak W Kurylov, Su, MR-M Probing SUSY with PV eN Interactions Deep Inelastic eD vs elastic ef e RPV Loops p SUSY effects Probing SUSY with PV eN Interactions Kurylov, R-M, Su “DIS Parity” SUSY loops SUSY dark matter QWp,SUSYQuickTime™ QWp,SM and a TIFF (Uncompressed) decompressor are needed to see this picture. Linear collider E158 &QWeak JLab Moller RPV 95% CL QWe, SUSY QWe, SM Fundamental Symmetries & Cosmic History Electroweak symmetry breaking: Higgs ? Baryogenesis: When? SUSY? Neutrinos? CPV? WIMPy D.M.: Related to baryogenesis? “New gravity”? Lorentz violation? Effects on CMB? ? Beyond the SM SM symmetry (broken) Cosmic Energy Budget What is the origin of baryonic matter ? Cosmic Energy Budget E d dS Dark Matter Baryons 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 ? 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 of matter, will these experiments see an EDM? Baryogenesis & Dark Matter: MSSM Chargino Mass Matrix T << TEW CPV new 0 0 0 0 M c C =11B 12W 13Hd 14Hu mW 2 sin WINO M1 0 HIGGSINO Neutralino Mass Matrix MN = background field m W 2 cos M2 BINO T ~TEWT:~scattering TEW ~ ~ (xH,W ) of from T << TEW : mixing ~ ~ ~0 of H,W to c~,c q , W˜ , B˜ , H˜ u,d 0 -mZ cos sin qW mZ cos cos qW M2 mZ sin sin qW -mZ sin sin qW -mZ cos sin qW mZ cos cos qW 0 - mZ sin sin qW -mZ sin sin qW - 0 EDM constraints & SUSY CPV Neutralino-driven baryogenesis Baryogenesis LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 Dark Matter: Future Experiments Cirigliano, Profumo, R-M EDMs, Baryogenesis, & Dark Matter • Continued progress in performing systematic computations of the baryon asymmetry • Continued scrutiny of QCD & nuclear structure uncertainties in EDM computations • Comprehensive phenomenology with other models of new CPV (extended Higgs sector) • Funding for experiments ! Future Directions: • Parity violation in electron scattering and hadronic interactions will continue to provide new insights into proton’s internal structure and weak qq interactions • PV in weak decays and electron scattering will continue to provide insights into new physics (SUSY, ’s, Higgs) that will complement LHC, ILC probes • PVTV will provide powerful probe of the origin of baryonic matter and non-baryonic dark matter Considerable theoretical and experimental challenges and opportunities remain: PAVI must go on!