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Dark energy and QCD axion from approximate U(1) de & U(1) PQ

Dark energy and QCD axion from approximate U(1) de & U(1) PQ. Jihn E. Kim Kyung Hee Univ. & Seoul National Univ. KASI, 16 April 2014. JEK, Phys. Rev. Lett. 111 (2013) 031801; JEK, Phys. Lett. B726 (2013) 450; JEK+H. P. Nilles, Phys. Lett. B730 (2014) 53 ;

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Dark energy and QCD axion from approximate U(1) de & U(1) PQ

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  1. Dark energy and QCD axion from approximate U(1)de & U(1)PQ Jihn E. Kim Kyung Hee Univ. & Seoul National Univ. KASI, 16 April 2014 JEK, Phys. Rev. Lett. 111 (2013) 031801; JEK, Phys. Lett. B726 (2013) 450; JEK+H. P. Nilles, Phys. Lett. B730 (2014) 53 ; JEK, JKPS 64 (2014)795 [arXiv:1311.4545[hep-ph] ].

  2. Sure, data needs more crayons! Or, color generating computer! All colors are constructed with three fundamental ones! (She may be a theorist)

  3. 1. Introduction 2. Axions and the strong CP problem 3. QCD axion from discrete symmetries 4. Dark energy from U(1)de

  4. 1. Introduction

  5. Cosmic pie CC Follows the cold dark matter Responsible for galaxy formation We discuss DE of order 10-47 GeV4 and CDM axion.

  6. A rough sketch of WIMP masses and cross sections. [Baer-Choi-Kim-Roszkowski, Soon appearing [arXiv:1404.xxxx]] 6/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  7. ★Because DE is a property of potential energy, bosonic coherent motion (BCM) can account for it. BCM such as axion also accounts for CDM. ★Higgs boson is a fundamental scalar. In the age of fundamental scalars, can these explain both DE and CDM? In the age of GUT scale vacuum energy observed, can these explain all of DE and CDM and inflation-finish? Higgs portal: The Higgs fields know the fundamental scalars contributing to CDM and DE. THEN, GLOBAL SYMMETRIES, AS FOR THE AXION, IS BETTER TO BE CONSIDERED. 7/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  8. Quantum gravity problem ★But quantum gravity effects are known to break global symmetries: the Planck scale wormholes connect observable universe O to the shadow world S. They can take out the global charges from O. ★ We can think of two possibilities of discrete symmetries realized from string compactification, below MP: • The discrete symmetry arises as a part of a gauge symmetry. • [Krauss-Wilczek, PRL 62 (1989) 1211] (ii) The string selection rules directly give the discrete symmetry. [JEK, PRL 111 (2013) 031801] ★ So, we start with discrete gauge symmetries. 8/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  9. Exact and approximate symmetries Vertical, exact sym.: gauged U(1), or string dictated. The global symmetry violating terms. A few low order W’s respected by discrete symmetry defines a global symmetry. 9/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  10. 2. Axions and Strong CP

  11. Strong CP The strongly interacting θ(Gluon)μν(Gluon-dual)μν term gives a nEDM. Neutron EDM is measured very accurately. dnth = (1.2-14.5)x10-16θe cm dnexp = 2.9 x10-26 e cm, Baker et al (2006) “Why is nEDM so small?” is the strong CP problem. 1140 J E Kim “Dark energy and QCD axion”, KASI, 16 April y 2014

  12. For gauge symmetry breaking, exactly flat. For global symmetry breaking, a potential is generated: Approximate 12/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  13. It is very flat if the axion decay constant is large, CP conserving point 10-20 In the evolving universe, at some temperature, say T1, a starts to roll down to end at the CP conserving point sufficiently closely. This analysis constrains the axion decay constant (upper bound) and the initial VEV of a at T1. Still oscillating nEDM was suggested to be measured 20 years ago: Hong-Kim-Sikivie, PRD42, 1847 (1990), Hong-Kim PLB265, 197 (1991), Hong-Kim-Nam-Semertzdis, 1403.1576. Graham et al, 1101.2691, Budker et al, 1306.6089, Sikivie et al, 1310.8545. The axion oscillation is just one example of Bosonic Coherent Motion (BCM). 13/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  14. The Lagrangian is invariant under changing θ → θ-2α.But θ becomes dynamical and the θ=a/Fapotential becomes The true vacuum chooses θ=a/Faat 14/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  15. A recent calculation of the cosmic axion density is, 109 GeV < Fa < {1012 GeV ?} Turner (86), Grin et al (07), Giudice-Kolb-Riotto (08), Bae-Huh-K (JCAP 08, [arXiv:0806.0497]): recalculated including the anharmonic term carefully with the new data on light quark masses. It is the basis of using the anthropic argument for a large Fa. Without string radiation All these three figures, Baer-Choi-Kim-Roszkowski, “Nonthermal DM”, to appear. 15/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  16. L. Rosenberg and G. Rybka in front of the ADMX apparatus. Science 343, 552 , 1 November 2013. CAPP at KAIST(Y. Semertzdis) will do for a larger axion mass and more. Xe tank at XMASS before completing filling water 30 October 2013.

  17. Science Vol. 343, 552 (2013): 1 November 2013, Focus Year invented 1977 by Lee-Weinberg; SUSY WIMP 1983 Gold. 1979 invisible axion 1982 CDM Solve technical problem in theory of strong nuclear force Explain dark matter Turn into photons in strong magnetic field Bounce off atomic nuclei Follow naturally from supersymmetry; provide many models and multiple avenues of detection Solve more than one problem; allow for decisive test.

  18. Many lab. searches were made, and we hope the axion be discovered . Graham et al, 1101.2691, Budker et al, 1306.6089, Sikivie et al, 1310.8545. Oscillating nEDM was suggested to be measured 20 years ago: Hong-Kim-Sikivie, PRD42, 1847 (1990), Hong-Kim PLB265, 197 (1991), Hong-Kim-Nam-Semertzidis, arXiv:1403.1576[hep-ph]. 18/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  19. KSVZ axion: The Peccei-Quinn symmetry by renormalizable couplings to heavy quarks. Why are we restricted to renormalizable interactions only at the EW scale? Definition of a global symmetry can be non- renormalizable terms also: DFSZ. Here, Higgs doublets are neutral under PQ. If they are not neutral, then it is not necessary to introduce heavy quarks [DFSZ axion]. In any case, the axion is the phase of the SM singlet S, if the VEV of S is much above the electroweak scale. Kim-Nilles term Because Fa can be in the intermediate scale, axions can live up to now (m<24 eV) and constitute DM of the Universe. 19/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  20. The axion is created at T=Fa, but the universe  (<a>)does not roll until 3H=ma (T=0.92 GeV [Bae-Huh-Kim]). From then on, the classical field <a> starts to oscillate. harmonic oscillator motion: ma2 Fa2 = energy density = max number density = like CDM. See,Bae-Huh-Kim, arXiv:0806.0497 [JCAP09 (2009) 005], Figure will be given with correct coefficients and new data Baer-Choi-Kim-Roszkowski, “Nonthermal DM”, to appear. 109 GeV < Fa<10 12 GeV, 20/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  21. 3. QCD axion from discrete symmetries

  22. S2(L) x S2(R) symmetric fermion masses can arise from The fermion mass matrix will be The first step for the solution of the μ-problem. [JEK, arXiv:1303.1822]. 22/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  23. [JEK, PRL111, 031801 arXiv:1303.1822].

  24. In string theory, matter fields are from E8 x E8 representations. Not from BMN . Kim-Nilles μ-term arises from Where do X and X–bar belong? Probably, in matter reps. Anyway, BMN fields: decay constant is very large F>1016 GeV [Choi-Kim (1984), Svrcek-Witten(2006)] 24/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  25. How can we break S2(L) x S2(R) symmetry ? Spontaneously by The massless (0) fields, and superheavy (G) fields 25/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  26. This defines the PQ charges of X and H. 26/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  27. ★Quantum gravity effects occurring at the Planck scale connect the observable universe O to the shadow world S via the Planck size wormholes. The discrete symmetry is a part of a gauge symmetry. How did we succeed? 27/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  28. The d=4 example is the θ term of Callan-Dashen-Gross and Jackiw-Rebbi. The d=5 examples are Weinberg operator and KN operator(with SUSY). The global symmetry violating terms. A few low order W’s are respected by discrete symmetry. 28/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  29. The PQ breaking diagram is 29/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  30. But the dominant breaking is by the QCD anomaly term: 30/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  31. 31/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  32. 4. Dark energy from U(1)de

  33. DE magnitude ★There exists a tiny DE of order 10-47 GeV4. ★We propose to relate this DE scale to a pseudo-Goldstone boson mass scale. ★The breaking scale of U(1)de is trans-Planckian, and the intermediate scale PQ symmetry breaking of U(1)de just adds the decay constant only by a tiny amount. 33/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  34. ★The discrete and global symmetries below MP are the consequence of the full W. So, the exact symmetries related to a discrete gauge symmetry or to string compactification are respected by the full W. Considering only W(3), we can consider approximate symmetries too. In particular, the approximate PQ symmetry. ★In string compactification, the bottom-up approach constraints [Lee et al, NPB 850, 1] toward a discrete gauge symmetry need not be considered. They are automatically satisfied with suitable massless singlets. ★For the MSSM interactions supplied by R-parity, one needs to know all the SM singlet spectrum. Z2 needed for a WIMP candidate. 34/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  35. ★Because the Higgs scalar is known to be a fundamental scalar, fundamental SM singlet scalar VEVs at the PQ symmetry breaking scale are considered, The DE potential height is The singlets must couple to Hu Hd : Then, to remove the U(1)de-QCD anomaly , U(1)PQ must be introduced for one linear combination is free of the QCD anomaly. The needed discrete symmetry must be of high order such that some low order W are forbidden. 35/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  36. ★A related comment is on the dilatonic symmetry: The dilatonic symmetry is spontaneously broken at the Planck scale. So, the dilaton is created without potential. It appears in the exponent. How do we raise the height of the dilaton potential? Another VEV such as <Hu> and <Hd> cannot render a potential for the dilaton. Maybe a confining force can do it. So, dilaton may have a severe problem accounting the scale of DE. 36/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  37. ★ But, if QCD anomaly coupling to U(1)de is present, then we have the usual QCD axion. ★ U(1)de should not have QCD anomaly. ★ We need one more U(1) such that one linear combination U(1)de does not have the QCD anomaly. We must introduce to global U(1)s, of course approximate: U(1)de and U(1)PQ . ★ We have the scheme to explain both 68% of DE and 28% of CDM via approximate global symmetries. With SUSY, axino may contribute to CDM also. Hilltop inflation 37/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  38. Typical example ★ The height of the potential is highly suppressed and we can obtain 10-47 GeV4 from discrete symmetry Z10R, without the gravity spoil of the global symmetry breaking term. ★ The discrete symmetry Z10R charges are the gauge charges of the mother U(1) gauge symmetry. ★ As a byproduct of the Mexican hat potential, Fig. (b), we also have a model of inflation, the so-called ‘hilltop inflation’. It is a small field inflation, consistent with the recent PLANCK data. 38/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  39. ★The simplest orbifold is Z(12-I), since there are only 3 fixed points. Note Z(3) has 27 fixed points. The model of [Huh-Kim-Kyae, PRD 80, 115012] has the Higgs with two units of discrete charge. ★For example, the Z10 is a subgroup of one U(1) direction Z10 = (0 0 0 0 0 4 2 0) (0 0 0 0 0 -8, 4, 0)’ (A) ★For the MSSM interactions supplied by R-parity, one needs to know all the SM singlet spectrum. Z2 needed for a WIMP candidate. 39/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  40. ★Some singlets have the even discrete charges. For example, s9 and s13 have Z10 quantum number magnitude 10. ★The VEVs of s9 and s13 break U(1) gauge symmetry direction (A) to Z10 . Even if Higgs doublets obtain VEVs, the resulting discrete group is Z2. From this direction, we can obtain Z10 if d=3 superpotential term contains Z10 =0 terms. We obtain Z10R if d=3 superpotential term does not contain Z10 =0 terms, but contains Z10 =2, 12, 22, etc. terms. For Z10 or Z10R , the d=2 μ Hu Hd term is not allowed. ★In conclusion, it is so simple to obtain the desired ZN or ZnR symmetry if we know all the SM singlets. We presented it in a Z(12-I) model. We find the method very useful for model building. And we can obtain an approximate PQ global symmetry as discussed in[JEK, PRL 111, 031801 (2013)] for the case of S2xS2. . 40/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  41. 5. Gravity waves from U(1)de

  42. DE magnitude ★There exists a tiny DE of order 10-47 GeV4. ★ What is the form of the U(1)de breaking V? ★We propose to relate this DE scale to a pseudo-Goldstone boson mass scale. ★The breaking scale of U(1)de is trans-Planckian, and the intermediate scale PQ symmetry breaking of U(1)de just adds the decay constant only by a tiny amount. The height is (GUT scale)4 ★It is by closing the green circle of (a): 42/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  43. ★We obtain [0.96, 0.008] New type (chaoton) hybrid inflation 43/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  44. Natural inflation starting at 0 is here. Natural inflation starting at π is here. Freese-Kinney: 1403.5277. 44/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  45. ★One condition to have a large e-folding is the Lyth bound, in our case fDE > 15 MP[D. Lyth, PRL 78 (1997) 1861] ★It is possible if the potential energy density is lower than MP4 .. One method is natural inflation: [Freese-Frieman-Olinto, PRL 65 (1990) 3233]. But, trans-Planckian needed two Axions at least: [Kim-Nilles-Peloso, JCAP 01 (2005) 005] 45/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  46. Kim-Nilles, PLB 730 (2014) 53 [arXiv:1311.0012]. Kim [arXiv:1404.4022].

  47. 49/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  48. U(1)de inflation with ‘chaoton’ X, more range. 48/40 J E Kim “Dark energy and QCD axion”, KASI, 16 April 2014

  49. Conclusion ★ BCM is one possibility of CDM. ★ For CDM, it must live sufficiently long. ★ Invisible axion is a CDM candidate. ★ Global symmetry U(1)PQ needed. ★Higgs portal, or anomaly portal always give U(1)PQ –gluon-gluon anomaly. ★U(1)de can give anomaly–free pseudo- Goldstone boson for the observed DE.

  50. City of Daejeon, Yusung Prefecture Center for Underground Physics: Young Duk Kim Head Q Campus Center for Theoretical Physics of the Universe(hep-ph, -th, nucl-th, astro-ph[CO]): Kiwoon Choi 3 km KAIST Campus Center for Axion and Precision Physics: Yannis Semertzidis

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