暗能量和宇宙學(xué)CPT破壞PPT課件

1、SN Ia (SCP, HZT.)LSS (2dfGRS, SDSS)Brief Review on Dark EnergyAccelerating Universe -Dark Energy第1頁(yè)/共44頁(yè)CMB experiments第2頁(yè)/共44頁(yè)Dark matter?Dark energy?Why no antimatter?No antimatter第3頁(yè)/共44頁(yè)Candidates:1, Cosmological constant/1wp Cosmological constant problem! 41234310)10(plmeVgT0)3(34pGaa 3/1/pwNeg

2、ative pressureS. Weinberg, RMP (1989)第4頁(yè)/共44頁(yè)2, Dynamical dark energy21()( )2LV221/ 21/ 2VwVQuintessence:11w 0w Phantom:21()( )2LV 1w eVHVmeff33010)( K-essence:(, )LL 1,1ww Cannot cross -1, no-go theoremFeng, Wang & Zhang, PLB(2005);Vikman, PRD(2005);Zhao, Xia, Li, Feng & Zhang, PRD(2005); X

3、ia, Cai, Qiu, Zhao &Zhang, IJMPD(2008) Quintom: 22121211()()( ,)22LV Feng, Wang & Zhang, PLB(2005)22221()()( )2cLVMLi, Feng & Zhang, JCAP(2005)wcrosses -1 Flat potential22221()()( )2cLVM21)( VLCai,Li,Lu,Piao,Qiu&Zhang, PLB(2007)第5頁(yè)/共44頁(yè)It is important to determine w of DE by cosmolog

4、ical observations!Parameterization of equation of state: A) w=w_0+w_1 z (for small z)B) w=w_0+w_1 z / (1+z) (used mostly in the literature)C) w=w_0+w_1 sin(w_2 ln(a)+w_3)第6頁(yè)/共44頁(yè)Current constraint on the equation of state of dark energyWMAP5 resultE. Komatsu et al., arXiv:0803.0547Xia, Li, Zhao, Zha

5、ng, PRD(2008)Status: 1) Cosmological constant fits data well;2) Dynamical model not ruled out;3) Best fit value of equation of state: slightly w across -1 Quintom modelQuintessencephantomQuintom AQuintom B第7頁(yè)/共44頁(yè)Dynamical dark energy is expected to have interactions to the rest of the world besides

6、 the gravity.Two types of couplings: direct & derivative1, direct couplingInteracting Dark Energy,.),(GGFFLMceVm3310)(104plMMcA. Long range forceConstrained tightly! S.M. Carroll, PRL(1998)B. Instability under quantum correctionsmeVMm72104ewplMM ,第8頁(yè)/共44頁(yè)2, derivative coupling:cosmological CPT v

7、iolation!1, obeys the shift symmetry which guarantees the flatness of the potential. 2, propagates spin-dependent force, short range, much weaker constraint from astrophysics PDG(2002)Violates Lorentz and CPT symmetry because.const00,.),(GFOMc00101)()()()(OCPTOCPTCPTOCPTGeVM1010第9頁(yè)/共44頁(yè)1010nnnnnnnbb

8、bBsn Cosmological CPT violation and baryogenesisThe universe is not symmetric between matter and antimatterWe need baryogenesis Baryon number non-conserving interaction C and CP violations Departure from thermal equilibrium Sakharov conditions for baryogenesis: Precondition: CPT is conserved!Cohen &

9、amp; Kaplan, PLB(1987)第10頁(yè)/共44頁(yè) Interacting dark energy and baryogenesisA unified picture of matter-antimatter asymmetry and dark energy!第11頁(yè)/共44頁(yè)Albrecht & Skordis, PRL(2000) )exp()()(plMfVQuintessence model with tracking solutionCopeland, Liddle & Wands, PRD(1998). 第12頁(yè)/共44頁(yè)2,100bsggg100,1

10、022Bean, Hansen & Melchiorri, PRD(2001);Doran & Robbers, JCAP(2006)第13頁(yè)/共44頁(yè)1, The electroweak Sphaleron violates B+L and will makeas low as 100GeV, M should be GeVKuzmin, Rubakov&Shaposhnikov,PLB(1985)DT10102, If M is higher, e.g., GUT scale or Planck mass scale, the generated baryon nu

11、mber asymmetry would be very small compared with the observation. 3, In this case, we turn to leptogenesis Comments:第14頁(yè)/共44頁(yè)Mingzhe Li, Jun-Qing Xia, Hong Li, Xinmin Zhang, PLB (2007)The ModeliJMcL第15頁(yè)/共44頁(yè)MTsnDLB210the decoupling temperature of B-L violating interaction. DTSphaleron conserves B-L

12、and converts B-L asymmetry generated above to a same order of baryon number asymmetry.GeVTMMDplanck1010,第16頁(yè)/共44頁(yè)Baryon isocurvature perturbationAdiabatic or isothermal:Isocurvature or entropy: nnssnnsnXXX , 0)/(0)/(snXsnBIn our caseThe fluctuation of the dark energy scalar field will induce a nonze

13、ro baryon isocurvature perturbation第17頁(yè)/共44頁(yè))exp()()(plMfVThe quintessence model with potential )()(212/1kJCkJC510)(planckinreisocurvatuBBMHnnConsistent with the observations!第18頁(yè)/共44頁(yè)MGeVMV2230010In our model of baryo/leptogenesisThe CPT violation is very small, was large to generate enough baryon

14、number asymmetry in the early universe.第19頁(yè)/共44頁(yè)This CPT violation can be observed by CMB polarization experiments!iJMcL第20頁(yè)/共44頁(yè)The full lagrangian of photonsThe action integral is gauge invariant.Geometric Optics Approximation第21頁(yè)/共44頁(yè)Basic equations:第22頁(yè)/共44頁(yè)P(yáng)olarization and Stokes parametersAt t

15、he inertial frameI intensity Q&U linear polarization V circular polarizationieUQiUQ222The polarization angle: QUarctan21第23頁(yè)/共44頁(yè)Local Lorentz frame第24頁(yè)/共44頁(yè)第25頁(yè)/共44頁(yè)第26頁(yè)/共44頁(yè)CPT violation induced the rotation of the polarization directionRotation angle only depends on the difference of dark ene

16、rgy field at the source and the observers positions. Which characterize such CPT-violating effect!)(fifiifdxpdkpMcpem32第27頁(yè)/共44頁(yè)Observation of cosmological CPT violation through CMB experiments第28頁(yè)/共44頁(yè)In the case of homogeneous Without CPT violation, the correlations of TB and EB vanish第29頁(yè)/共44頁(yè)第30

17、頁(yè)/共44頁(yè)第31頁(yè)/共44頁(yè)第32頁(yè)/共44頁(yè)WMAP3 only: 0.057 degPLANCKdeg 0 . 40 . 6deg 8 . 32 . 61)2)3)6)Bo Feng et al., PRL 96, 221302 (2006)5)4)(WMAP Group) Komatsu et al., arXiv:0803.0547WMAP5 onlydeg 0 . 35 . 2deg 1 . 27 . 1deg 9 . 16 . 2P.Cabella, Natoli & Silk, PRD (2007)第33頁(yè)/共44頁(yè)Spatial dependent rotation

18、angle:Mingzhe Li & Xinmin Zhang, PRD(2008)第34頁(yè)/共44頁(yè)第35頁(yè)/共44頁(yè)第36頁(yè)/共44頁(yè)This is the direct consequence of invariance of under the rotation sin,obsEBlobsTBlCCOnly the background evolution of dark energy provides CPT violation!第37頁(yè)/共44頁(yè)The corrections are at the order of 2In the quintessence model wi

19、th tracking potential, )()(212/1kJCkJC2222)10(MeVBy assuming the initial fluctuation of quintessence generated from a GUT scale inflation第38頁(yè)/共44頁(yè)Constraining a spatially dependent rotation of the Cosmic Microwave Background Polarization.Yadav, Biswas, Su, Zaldarriaga,arXiv:0902.4466How to De-Rotate the Cosmic Microwave Background Polarization.M. Kamionko