理物理的方法等效原理到宇宙课件

W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW1CMB Polarization ObservationlIn 2002,DASI microwave interferometer observed the polarization of the cosmic background.lWith the pseudoscalar-photon interaction,the polarization anisotropy is shifted relative to the temperature anisotropy.lIn 2003,WMAP found that the polarization and temperature are correlated to 10.This gives a constraint of 10-1 rad or 6 degrees of the cosmic polarization rotation angle.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW2CMB Polarization ObservationlIn 2005,the DASI results were extended(Leitch et al.)and observed by CBI(Readhead et al.)and CAPMAP(Barkats et al.)lIn 2006,BOOMERANG CMB PolarizationlDASI,CBI,and BOOMERANG detections of Temperature-polarization cross correllationlPlanck Surveyor will be launched next year with better polarization-temperature measurement and will give a sensitivity to cosmic polarization rotation of 10-2-10-3.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW3WMAP 3 year Polarization MapsTTTTTEEEBB(r=0.3)BB(lensing)foregroundW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW4Pseudo-scalars:Pseudoscalar-Photon CouplingW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW5,AF (1/2)FF(Mod Divergence)W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW6Change of Polarization due to Cosmic PropagationlThe effect of in(2)is to change the phase of two different circular polarizations of electromagnetic-wave propagation in gravitation field and gives polarization rotation for linearly polarized light.6-8 lPolarization observations of radio galaxies put a limit of 1 over cosmological distance.9-14l Further observations to test and measure to 10-6 is promising.lThe natural coupling strength is of order 1.However,the isotropy of our observable universe to 10-5 may leads to a change()of over cosmological distance scale 10-5 smaller.Hence,observations to test and measure to 10-6 are needed.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW7Pseudoscalar-Photon Interaction and AxionlW.-T.Ni,A Nonmetric Theory of Gravity,preprint,Montana State University,Bozeman,Montana,USA(1973),http:/gravity5.phys.nthu.edu.tw.lW.-T.Ni,Bull.Am.Phys.Soc.,1919,655(1974).lW.-T.Ni,Phys.Rev.Lett.3838,301(1977).lS.Weinberg,sl Phys.Rev.Lett.4040,233(1978).lF.Wilczek,sl Phys.Rev.Lett.4040,279(1978).lM.Dine sl et al.,sl Phys.Lett.104B104B,1999(1981).lM.Shifman sl et al.,sl Nucl.Phys.B166B166,493(1980).lJ.Kim,sl Phys.Rev.Lett.4343,103(1979).lS.L.Cheng,C.Q.Geng and W.-T.Ni,sl Phys.Rev.D52D52 3132(1995)and references therein.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW8ElectomagneticElectomagnetic Wave Propagation and Polarization EP Wave Propagation and Polarization EPlW.-T.Ni,Equivalence Principles and Precision Experiments pp.647-651,in Precision Measurement and Fundamental Constants II,ed.by B.N.Taylor and W.D.Phillips,Natl.Bur.Stand.(U.S.),Spec.Publ.bf 617(1984).lW.-T.Ni,Timing Observations of the Pulsar Propagations in the Galactic Gravitational Field as Precision Tests of the Einstein Equivalence Principle,pp.441-448 in Proceedings of the Second Asian-Pacific Regional Meeting of the International Astronomical Union,ed.by B.Hidayat and M.W.Feast(Published by Tira Pustaka,Jakarta,Indonesia,1984).lW.-T.Ni,Equivalence Principles,Their Empirical Foundations,and the Role of Precision Experiments to Test Them,pp.491-517 in Proceedings of the 1983 International School and Symposium on Precision Measurement and Gravity Experiment,Taipei,Republic of China,January 24-February 2,1983,ed.by W.-T.Ni(Published by National Tsing Hua University,Hsinchu,Taiwan,Republic of China,June,1983).lM.P.Haugan and T.F.Kauffmann,sl Phys.Rev.D bf 52,3168(1995).lT.P.Krisher,sl Phys.Rev.D bf 44,R2211(1991).W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW9PseudoscalarPseudoscalar-Photon Interaction and Astrophysical/Cosmic-Photon Interaction and Astrophysical/Cosmic Polarization Rotation Polarization Rotation (=(=)of Electromagnetic Wave of Electromagnetic Wave PropagationPropagationlW.-T.Ni,A Nonmetric Theory of Gravity,preprint,Montana State University,Bozeman,Montana,USA(1973),http:/gravity5.phys.nthu.edu.tw.lS.M.Carroll,G.B.Field,R.Jackiw,sl Phys.Rev.D bf 41,1231(1990).lS.M.Carroll and G.B.Field,sl Phys.Rev.D bf 43,3789(1991).lB.Nodland and J.P.Ralston,sl Phys.Rev.Lett.bf 78,3043(1997).lJ.F.C.Wardle,R.A.Perley,and M.H.Cohen,sl Phys.Rev.Lett.bf 79,1801(1997).lD.J.Eisenstein and E.F.Bunn,sl Phys.Rev.Lett.bf 79,1957(1997).lS.M.Carroll and G.B.Field,sl Phys.Rev.Lett.bf 79,2394(1997).lT.J.Loredo,E.A.Flanagan,and I.M.Wasserman,sl Phys,Rev.bf D 56,7507(1997).lS.M.Carroll,sl Phys.Rev.Lett.bf 81,3067(1998).lA.Lue,L.Wang,and M.Kamionkowski,Phys.Rev.Lett.bf 83,1506(1999).W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW10Nomenclature in OpticslBirefringence:velocity dependent on polarization linear-polarization to elliptical-polarization lDichroism:absorption varies with polarizationlFaraday rotation(dependent on wavelength)lCosmic polarization Rotation not like QED vacuum birefringence(no V Stokes parameter produced)W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW11Space contribution to the local polarization rotation Space contribution to the local polarization rotation angle-angle-1313,x x =|=|coscos x0.The time x0.The time contribution is contribution is,0,0 x0.The total contribution is x0.The total contribution is(|(|coscos +,0,0)x0.x0.(x0 x0 0)0)Intergrated:(2)-(1)1:a point at the decoupling epoch2:observation point W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW12Variations and Fluctuationsl lrotation(2)-(1)rotation(2)-(1)l l(2)-(2)-(1):(1):(2)variations and fluctuations at(2)variations and fluctuations at the last scattering surface of thethe last scattering surface of the decoupling epoch;decoupling epoch;(1),at present observation(1),at present observation point,fixedpoint,fixedl l variance of fluctuation(1)2 variance of fluctuation couplingcoupling 10(-5)2 10(-5)2l lThe coupling depends on various cosmological The coupling depends on various cosmological modelsmodelsW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW13Constraints on cosmic polarization rotation from CMBAll consistent with null detection and with one another at 2 levelW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW14FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY FIVE-YEAR WILKINSON MICROWAVE ANISOTROPY PROBE(WMAP1)OBSERVATIONS:PROBE(WMAP1)OBSERVATIONS:COSMOLOGICAL INTERPRETATION,Komatsu et al.,COSMOLOGICAL INTERPRETATION,Komatsu et al.,arXiv:0803.0547v2 arXiv:0803.0547v2 astroastro-ph 17 Oct 2008-ph 17 Oct 2008lThe power spectra of TB and EB correlations constrain a parity-violating interaction,which rotates the polarization angle and converts E to B.The polarization angle could not be rotated more than 5.9 2.4(95%CL)between the decoupling and the present epoch.I.e.-30 73 mrad(2)W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW15ReferencesW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW16COSMOLOGICAL MODELSlPSEUDO-SCALAR COSMOLOGY,e.g.,Brans-Dicke theory with pseudoscalar-photon couplinglNEUTRINO NUMBER ASYMMETRYlBARYON ASYMMETRYlSOME other kind of CURRENTlLORENTZ INVARIANCE VIOLATIONlCPT VIOLATIONlDARK ENERGY(PSEUDO)SCALAR COUPLINGlOTHER MODELSW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW17W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW18Pseudoscalar QuintessenceW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW19JCAPW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW20Neutrino number asymmetrylNeutrino number asymmetry is function of electron-neutrino degeneracy parameter e with e=e(chemical potential)/Te l ecould be 0.001W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW21Significance and OutlooklPseudoscalar-photon interaction is proportional to the gradient of the pseudoscalar field.From phenomenological point of view,this gradient could be neutrino number asymmetry,other density current,or a constant vector.In these situations,Lorentz invariance or CPT may effectively be violated.lProbing neutrino number asymmetrylBetter accuracy in CMB polarization observation is expected from PLANCK mission to be launched this year.A dedicated CMB polarization observer in the future would probe this fundamental issue more deeply.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW22Detectability of Primordial G-WavesW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW23The Gravitational Wave Background from Cosmological Compact BinariesAlison J.Farmer and E.S.Alison J.Farmer and E.S.PhinneyPhinney(Mon.Not.RAS 2003)(Mon.Not.RAS 2003)Optimistic(upper dotted),fiducial(Model A,lower solid line)and pessimistic(lower dotted)extragalactic backgrounds plotted against the LISA(dashed)single-arm Michelson combination sensitivity curve.Theunresolved Galactic close WDWD spectrum from Nelemans et al.(2001c)is plotted(with signals from binaries resolved by LISA removed),as well as an extrapolated total,in which resolved binaries are restored,as well as an approximation to the GalacticMSMS signal at low frequencies.Super-ASTRODRegionDECIGOBBO RegionW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW24LISA LISA consists of a fleet of 3 spacecraft 20 behind earth in solar orbit keeping a triangular configuration of nearly equal sides(5 106 km).Mapping the space-time outside super-massive black holes by measuring the capture of compact objects set the LISA requirement sensitivity between 10-2-10-3 Hz.To measure the properties of massive black hole binaries also requires good sensitivity down at least to 10-4 Hz.(2017)W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW25ASTROD configuration(baseline ASTROD after 700 days from launch)W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW26Super-ASTROD(1Super-ASTROD(1stst TAMA Meeting1996)TAMA Meeting1996)W.-T.Ni,“ASTROD and gravitational waves”in W.-T.Ni,“ASTROD and gravitational waves”in Gravitational Gravitational Wave DetectionWave Detection,edited by K.Tsubonoedited by K.Tsubono,M.-K.Fujimoto and K.Kuroda,M.-K.Fujimoto and K.Kuroda(Universal Academy Press,Tokyo,Japan,1997),pp.117-129.(Universal Academy Press,Tokyo,Japan,1997),pp.117-129.lWith the advance of laser technology and the development of space interferometry,one can envisage a 15 W(or more)compact laser power and 2-3 fold increase in pointing ability.lWith these developments,one can increase the distance from 2 AU for ASTROD to 10 AU(25 AU)and the spacecraft would be in orbits similar to Jupiters.Four spacecraft would be ideal for a dedicated gravitational-wave mission(Super-ASTROD).W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW27Primordial GW and Super-ASTRODlFor detection of primordial GWs in space.One may go to frequencies lower or higher than LISA/ASTROD bandwidth where there are potentially less foreground astrophysical sources to mask detection.lDECIGO and Big Bang Observer look for gravitational waves in the higher range lSuper-ASTROD look for gravitational waves in the lower range.lSuper-ASTROD(ASTROD III):3-5 spacecraft with 5 AU orbits together with an Earth-Sun L1/L2 spacecraft and ground optical stations to probe primordial gravitational-waves with frequencies 0.1 Hz-1 mHz and to map the outer solar system.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW28Primordial Gravitational Waves strain sensitivity strain sensitivity (2)energy sensitivity2)energy sensitivity W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW29Sensitivity to Primordial GWlThe minimum detectable intensity of a stochastic GW background is proportional to detector noise spectral power density S_n(f)times frequency to the third powerlwith the same strain sensitivity,lower frequency detectors have an f(-3)-advantage over the higher frequency detectors.lcompared to LISA,ASTROD has 27,000 times(303)better sensitivity due to this reason,while Super-ASTROD has an additional 125(53)times better sensitivity.W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW30Primordial Gravitational Waves strain sensitivity strain sensitivity (2)energy sensitivity2)energy sensitivity W.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW31lPolarization as a tool to test cosmological models and to look into(gravitational)axion and possible dark energy pseudoscalar,CPT,Neutrino Asymmetry,etc.lPrimordial gravitational waves may possibly be detected by ASTROD/Super-ASTROD and DECIGO/Big Bang ObserverW.-T.Ni2008.11.29.PP-A-QFT SingaporeCosmic polarization rotation,cosmological models&Primordial GWCosmic polarization rotation,cosmological models&Primordial GW32lThank you!