Apartes de la Conferencia de la SJG del 14 y 21 de Enero de 2012Nonlinear electrodynamics and cmb polarization
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Home Search Collections Journals About Contact us My IOPscience Nonlinear electrodynamics and CMB polarization This article has been downloaded from IOPscience. Please scroll down to see the full text article. JCAP03(2011)033 (http://iopscience.iop.org/1475-7516/2011/03/033) View the table of contents for this issue, or go to the journal homepage for more Download details: IP Address: 201.39.176.35 The article was downloaded on 22/03/2011 at 21:17 Please note that terms and conditions apply.
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J ournal of Cosmology and Astroparticle Physics An IOP and SISSA journalNonlinear electrodynamics and CMBpolarizationHerman J. Mosquera Cuestaa,b,c,d and G. Lambiasee,f JCAP03(2011)033a Departmento de F´ısica Universidade Estadual Vale do Acara´, u Avenida da Universidade 850, Campus da Betˆnia, CEP 62.040-370, Sobral, Cear´, Brazil a ab Instituto de Cosmologia, Relatividade e Astrof´ ısica (ICRA-BR), Centro Brasileiro de Pesquisas F´ ısicas, Rua Dr. Xavier Sigaud 150, CEP 22290-180, Urca Rio de Janeiro, RJ, Brazilc International Center for Relativistic Astrophysics Network (ICRANet), International Coordinating Center, Piazzalle della Repubblica 10, 065112, Pescara, Italyd International Institute for Theoretical Physics and Mathematics Einstein-Galilei, via Bruno Buozzi 47, 59100 Prato, Italye Dipartimento di Fisica “E.R. Caianiello”, Universit` di Salerno, a 84081 Baronissi (SA), Italyf INFN, Sezione di Napoli, Napoli, Italy E-mail: herman@icra.it, lambiase@sa.infn.itReceived July 1, 2010Revised January 23, 2011Accepted February 8, 2011Published March 22, 2011Abstract. Recently WMAP and BOOMERanG experiments have set stringent constraintson the polarization angle of photons propagating in an expanding universe: ∆α = (−2.4 ±1.9)◦ . The polarization of the Cosmic Microwave Background radiation (CMB) is reviewedin the context of nonlinear electrodynamics (NLED). We compute the polarization angle ofphotons propagating in a cosmological background with planar symmetry. For this purpose,we use the Pagels-Tomboulis (PT) Lagrangian density describing NLED, which has the form 1L ∼ (X/Λ4 )δ−1 X, where X = 4 Fαβ F αβ , and δ the parameter featuring the non-Maxwelliancharacter of the PT nonlinear description of the electromagnetic interaction. After lookingat the polarization components in the plane orthogonal to the (x)-direction of propagationof the CMB photons, the polarization angle is deﬁned in terms of the eccentricity of theuniverse, a geometrical property whose evolution on cosmic time (from the last scatteringsurface to the present) is constrained by the strength of magnetic ﬁelds over extragalacticdistances.Keywords: CMBR polarisation, CMBR theory, extragalactic magnetic ﬁelds, cosmic mag-netic ﬁelds theoryc 2011 IOP Publishing Ltd and SISSA doi:10.1088/1475-7516/2011/03/033
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Contents1 Introduction 12 Minimally coupling gravity to nonlinear electrodynamics 23 Cosmological setting: Space-time with planar symmetry −→ universe ec- centricity −→ polarization angle 4 JCAP03(2011)033 3.1 Space-time anisotropy and magnetic energy density evolution 4 3.2 Space-time eccentricity and polarization angle 5 3.3 Eccentricity evolution on cosmic time 6 3.4 Constraints on parameter Λ from extragalactic B strengths in an ellipsoidal Universe 74 Light propagation in NLED and birefringence 85 Stokes parameters, rotated CMB spectra and constraints on parameter Λ 9 5.1 Estimative of Λ 106 Discussion and closing remarks 111 IntroductionModiﬁcations to the standard (Maxwell) electrodynamics were proposed in the literature inorder to avoid inﬁnite physical quantities from theoretical descriptions of electromagneticinteractions. Born and Infeld [1], for instance, proposed a model in which the inﬁnite selfenergy of point particles (typical of Maxwell’s electrodynamics) are removed by introducingan upper limit on the electric ﬁeld strength, and by considering the electron as an electricparticle with ﬁnite radius. Along this line, other models of nonlinear electrodynamics (NLED)Lagrangians were proposed by Plebanski, who also showed that Born-Infeld model satisﬁesphysically acceptable requirements [2]. Consequences of nonlinear electrodynamics have beenstudied in many contexts, such a, for example, cosmological models [3], black holes andwormhole physics [4, 5], primordial magnetic ﬁelds in the Universe [8, 9, 11], gravitationalbaryogenesis [8], and astrophysics [12, 17]. In this paper we investigate the CMB polarization of photons described by nonlinearelectrodynamics. We compute the polarization angle of photons propagating in an expand-ing Universe, by considering in particular cosmological models with planar symmetry. Thepolarization angle does depend on the parameter characterizing the nonlinearity of electro-dynamics, which will be constrained by making use of the recent data from WMAP andBOOMERANG. This kind of investigations has received a lot of interest because they rep-resent a probe of models beyond the standard model, which may violate the fundamentalsymmetries such as CPT and Lorentz invariance [13, 14]. In what follows we will followthe main lines of the paper on “Cosmological CPT violation, baryo/leptogenesis and CMBpolarization” by Li-Xia-Li-Zhang [6]. –1–
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2 Minimally coupling gravity to nonlinear electrodynamicsThe action of (nonlinear) electrodynamics coupled minimally to gravity is 1 √ 1 √ S= d4 x −gR + d4 x −gL(X, Y ) , (2.1) 2κ 4πwhere κ = 8πG, L is the Lagrangian of nonlinear electrodynamics depending on the invariantX = 1 Fµν F µν = −2(E2 − B2 ) and Y = 4 Fµν ∗ F µν , where F µν ≡ µ Aν − ν Aµ , and 4 1∗ F µν = µνρσ F αβγδ = √ 1 ρσ is the dual bivector, and 2 −g εαβγδ , with εαβγδ the Levi-Civitatensor (ε0123 = +1). JCAP03(2011)033 The equations of motion are [9] µν µ (−LX F − LY ∗ F µν ) = 0 , (2.2)where LX = ∂L/∂X and LY = ∂L/∂Y , µ Fνλ + ν Fλµ + λ Fµν = 0. (2.3) After a swift grasp on this set of equations one realizes that is diﬃcult to ﬁnd solutionsin closed form of these equations. Therefore to study the eﬀects of nonlinear electrodynamics,we conﬁne ourselves to consider the abelian Pagels-Tomboulis theory [16], proposed as aneﬀective model of low energy QCD. The Lagrangian density of this theory involves only theinvariant X in the form δ−1 X2 2 L(X) = − X = −γX δ , (2.4) Λ8where γ (or Λ) and δ are free parameters that, with appropriate choice, reproduce the wellknown Lagrangian already studied in the literature. γ has dimensions [energy]4(1−δ) . Following Kunze [9], the energy momentum tensor corresponding to the Lagrangiandensity L(X) is given by 1 Tµν = LX gαβ Fµα Fβν + gµν L (2.5) 4πand the decomposition of the electromagnetic tensor with respect to a fundamental observerwith 4-velocity uµ (uµ uµ = −1) ˆ ˆ Fµν = 2E[µ uν] − ηµνςτ uς B τ . (2.6) ˆ ˆ The electric and magnetic ﬁelds are therefore given by Eµ = Fµν uν and Bµ =1 ν F κλ (η √2 ηµνκλ u αβγδ = −g εαβγδ ). The energy density turns out to be 1 L ˆ ˆ ˆ ˆ ρ = Tµν uµ uν = − (2δ − 1)Eα E α + Bα B α . (2.7) 8π XThe positivity of ρ (weak energy condition) imposes, in general, the constraint on δ. Forthe Lagrangian (2.4) one gets δ ≥ 1 . However, this condition can be relaxed because we 2shall consider cosmological scenarios in which the electric ﬁeld is zero, and only the magneticﬁelds survive (this is justiﬁed by the fact that during the radiation dominated era the plasmaeﬀects induce a rapid decay of the electric ﬁeld, whereas magnetic ﬁeld remains (see thepaper by Turner and Widrow in [23])). –2–
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The equation of motion for the Pagels-Tomboulis theory follows from eq. (2.2) withY =0 µν µX µF = −(δ − 1) F µν . (2.8) XIn terms of the potential vector Aµ , and imposing the Lorentz gauge µ Aµ = 0, eq. (2.8)becomes µ ν µX µ A + Rνµ Aµ = −(δ − 1) ( µ Aν − ν Aµ ) , (2.9) Xwhere the Ricci tensor Rνµ appears because the relation [ µ , ν ]Aν = −Rµ Aµ . µ To proceed onward, we apply the geometrical optics approximation. This means thatthe scales of variation of the electromagnetic ﬁelds are smaller than the cosmological scales JCAP03(2011)033we consider next. In this approximation, the 4-vector Aµ (x) can be written as [18] Aµ (x) = Re (aµ (x) + bµ (x) + . . .)eiS(x)/ (2.10)with 1 so that the phase S/ varies faster than the amplitude. By deﬁning the wavevector kµ = µ S, which deﬁnes the direction of the photon propagation, one ﬁnds that thegauge condition implies kµ aµ = 0 and kµ bµ = 0. It turns out to be convenient to introducethe normalized polarization vector εµ so that the vector aµ can be written as aµ (x) = A(x)εµ , εµ εµ = 1 . (2.11)As a consequence of (2.11), one also ﬁnds kµ εµ = 0, i.e. the wave vector is orthogonal to thepolarization vector. By making use of eq. (2.10), one obtains µX 2ikµ = [1 + Ω( )] , (2.12) Xwhere ik[α aβ] [α aβ] + O( 2 ) µk Ω≡ . −(k[α aβ] )2 + i 2k[α aβ] ( [α aβ] + ik[α aβ] ) + O( 2 )To leading order in , the term depending on the Ricci tensors can be neglected in (2.9).Inserting (2.10) into (2.9) and collecting all terms proportional to −2 and −1 , one obtains 1 2 : kµ kµ aσ = 2(δ − 1)kµ k[µ aσ] , (2.13) 1 µ σ : 2kµ a + aσ µk µ = −2(δ − 1)kµ [µ σ] a . (2.14) Taking into account the gauge condition kµ aµ = 0, the ﬁrst equation implies 1 (2δ − 1)k2 = 0 → kµ kµ = 0 , ,provided δ = (2.15) 2hence photons propagate along null geodesics. Multiplying eq. (2.14) by aσ , and using (2.11)one obtains 1 µ µ σ µ µ k = −δk µ ln A + (δ − 1)kµ ε σε , 2so that eq. (2.14) can be recast in the form δ−1 σ kµ µε σ = Υ (2.16) δwhere Υσ ≡ kµ [ σ µ ε − (ερ µ σ ρ ε )ε ] . (2.17) –3–
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3 Cosmological setting: Space-time with planar symmetry −→ universe eccentricity −→ polarization angle3.1 Space-time anisotropy and magnetic energy density evolutionLet us consider cosmological models with planar symmetry, i.e., having a similar scale factoron the ﬁrst two spatial coordinates. The most general line-element of a geometry with plane-symmetry is [19] ds2 = dt2 − b2 (dx2 + dy 2 ) − c2 dz 2 , (3.1)where b(t) and c(t) are the scale factors, which are normalized in order that b(t0 ) = 1 = c(t0 ) JCAP03(2011)033at the present time t0 . As eq. (3.1) shows, the symmetry is on the (xy)-plane. The coherenttemperature and polarization patterns produced in homogeneous but anisotropic cosmologicalmodels (Bianchi type with a Friedman-Robertson-Walker limit has been studied in [15]). The Christoﬀel symbols corresponding to the metric (3.1) are ˙ Γ0 = Γ0 = bb , Γ0 = cc , ˙ (3.2) 11 22 33 ˙ b c ˙ Γ1 = Γ2 = , Γ3 = . 01 02 03 b c The dot stands for derivative with respect to the cosmic time t. To make an estimate on the parameter δ, we have to investigate in more detail thegeometry with planar symmetry. As pointed out by Campanelli-Cea-Tedesco (CCT) in [20],the most general tensor consistent with the geometry (3.1) is µ µ T µ = diag(ρ, −p , −p , −p⊥ ) = T(I)ν + T(A)ν , ν µin which T(I)ν = diag(ρ, −p, −p, −p) is the standard isotropic energy-momentum tensor de- µscribing matter, radiation, or cosmological constant, and T(A)ν = diag(ρA , −pA , −pA . − pA )represents the anisotropic contribution which induces the planar symmetry, and can be givenby a uniform magnetic ﬁeld, a cosmic string, a domain wall.1 In what follows, we shall con-sider a Universe matter dominated (p = 0) with planar symmetry generated by a uniformmagnetic ﬁeld B(t). Magnetic ﬁelds have been observed in galaxies, galaxy clusters, and extragalactic struc-tures [22], and it is assumed that they may have a primordial origin [9, 23]. Due to thehigh conductivity of the primordial plasma, the magnetic ﬁeld evolves as B(t) ∼ b−2 be-ing frozen into the plasma [21, 22] (see below). Denoting with ρB the magnetic ﬁelddensity, the energy-momentum tensor for a uniform magnetic ﬁeld can be written as µT(B) ν = ρB diag(1, −1, −1, −1). According to (2.7), we ﬁnd that the energy density of the magnetic ﬁeld is given by δ−1 B2 B2 ρB = . (3.3) 8π 2Λ4 1 Notice that the cases discussed in [20], i.e. the magnetic ﬁelds or the topological defects as responsible ofthe planar symmetry of the Universe, allow to explain the anomaly concerning the low quadruple amplitudeprobed by WMAP. The interesting analysis performed by CCT leads to the conclusion that an eccentricityat the decoupling of the order of e ∼ 10−2 is indeed able to explain the drastic reduction in the quadrupleanisotropy without aﬀecting higher multiples of the angular power spectrum of the temperature anisotropies. –4–
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The evolution law of the energy density ρB is given by [10] 4 ρB + ΘρB + 16πσab Πab = 0 , ˙ (3.4) 3where Θ is the volume expansion (contraction) scalar, σab is the shear, and Πab the anisotropicpressure of the ﬂuid. In a highly conducting medium we still have with good approximationB ∼ b−2 provided that anisotropies can be neglected (this means that we neglect radiativeeﬀect of the primordial ﬂuid).3.2 Space-time eccentricity and polarization angle JCAP03(2011)033We shall assume that photons propagate along the (positive) x-direction, so that kµ =(k0 , k1 , 0, 0) [7]. Gauge invariance assures that the polarization vector of photons has onlytwo independent components, which are orthogonal to the direction of the photons motion. ˆTherefore, we are only interested in how the components of the polarization vector (Iµ 2 andˆIµ3) change. It then follows that Υ σ deﬁned in (2.17) assumes the form ˙ b c ˙ ˙ Υσ = −k0 δσ2 ε2 + δσ3 ε3 + bb(ε2 )2 + cc(εc )2 εσ ˙ (3.5) b c The components of Υσ given by (3.5) vanish in the case of a Friedman-Robertson-Walkergeometry. By deﬁning the aﬃne parameter λ which measures the distance along the line-element,kµ ≡ dxµ /dλ, one obtains that ε2 and ε3 satisfy the following geodesic equation (fromeq. (2.16)) dε2 ˙ b ˙ δ−1 0 b + k0 ε2 = − k ˙ + bb(ε2 )2 + cc(ε3 )2 ε2 ˙ dλ b δ b dε3 c˙ δ−1 0 c ˙ ˙ + k0 ε3 = − k + bb(ε2 )2 + cc(ε3 )2 ε3 ˙ dλ c δ cThese equations can be further simpliﬁed if one observes that k0 = dt/dλ 1 d ln(bε2 ) δ−1 ˙ b c˙ 0 D ln(bε2 ) = =− − + (cε3 )2 , (3.6) k dt δ b c 1 d ln(cε3 ) δ−1 c b ˙ ˙ 0 D ln(cε3 ) = =− − + (bε2 )2 . (3.7) k dt δ c bwhere D ≡ kµ µ. (3.8) ˙Moreover, the diﬀerence of the Hubble expansion rate b/b and c/c can be written as ˙ ˙ b c˙ 1 de2 − = 2 ) dt (3.9) b c 2(1 − ewhere we have introduced the eccentricity c 2 e(t) = 1− . (3.10) b –5–
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The polarization angle α is deﬁned as α = arctan[(cε3 )/(bε2 )]. Its time evolution isgoverned by equation δ−1 0 ˙ b c ˙ Dα − k − [(bε2 )3 + (cε3 )3 ] = 0 . (3.11) 2δ b c However, eqs. (3.6) and (3.7) implies that both bε2 and cε3 evolves as Ai + (δ − 1)fi (t),i = 2, 3 , where fi (t) is a function of time and Ai are constant of integration. Therefore, toleading order (δ − 1) eq. (3.11) reads ˙ JCAP03(2011)033 δ−1 K 0 b c ˙ Dα − k − + O((δ − 1)2 ) = 0 . (3.12) δ 2 b cwhere K = A2 + A3 . To compute the rotation of the polarization angle, one needs to evaluate α at two distinctinstants. In the cosmological context that we are considering is assumed that the referencetime t corresponds to the moment in which photons are emitted from the last scatteringsurface, and the instant t0 corresponds to the present time. One, therefore, gets2 δ−1 ∆α = α(t) − α(t0 ) = Ke2 (z) , (3.13) 4δwhere we have used e(t0 ) = 0 because of the normalization condition b(t0 ) = c(t0 ) = 1 andlog(1 − e2 ) ∼ −e2 . Notice that for δ = 1 or e2 = 0 there is no rotation of the polarization angle, as expected.Moreover, in the case in which photons propagate along the direction z-direction, so that¯ka = (ω0 , 0, 0, k), we ﬁnd that the NLED have no eﬀects as concerns to the rotation of thepolarization angle. As arises from (3.13), ∆α vanishes in the limit δ = 1, so that no rotation of thepolarization angle occurs in the standard electrodynamics, even if the background is describedby a geometry with planar symmetry. Moreover, even if δ = 1, ∆α still vanishes for anisotropic and homogeneous cosmology described by the Friedman-Robertson-Walker elementline (b = c) ds2 = dt2 − b2 (dx2 + dy 2 + dz 2 ), because in such a case the eccentricity vanishes(this agrees with the fact that for this background the components of Υσ , eq. (3.5), are zero).3.3 Eccentricity evolution on cosmic timeThe time evolution of the eccentricity is determined from the Einstein ﬁeld equations 1 d(ee) ˙ (ee)2 ˙ 2 dt + 3Hb (ee) + ˙ = 2κρB , (3.14) 1−e (1 − e2 )2 ˙where Hb = b/b. 2 Preliminary calculations [38] performed in terms of the electromagnetic ﬁeld Fµν and of time evolution ofthe Stokes parameters I, Q, U, V (this approach is alternative to one presented in the section II of the paperwhere the analysis is performed in terms of the 4-potential Aµ ) yield again the result (3.13). Calculationsshow that the total ﬂux I is not the same along the three spatial directions, as expected owing to the diﬀerentexpansion of the Universe along the x, y and z directions. Moreover the time evolution of the Stokes parametersturns out to be a mixture of each others, which reduce to standard results as δ = 1. The polarization angleis deﬁned as 2α = arctan(U/Q). –6–
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It is extremely diﬃcult to exactly solve this equation. We shall therefore assume thatthe e2 -terms can be neglected. Since b(t) ∼ t2/3 during the matter-dominated era, eq. (3.14)implies (0) e2 (z) = 18Fδ (z)ΩB , (3.15)where we used 1 + z = b(t0 )/b(t), e(t0 ) = 0, and 3 3(1 + z)4δ−3 3 Fδ ≡ −2− + 2(1 + z) 2 . (3.16) (9 − 8δ)(4δ − 3) (9 − 8δ)(4δ − 3) (0)ΩB is the present energy density ratio JCAP03(2011)033 δ−1 2 δ−1 (0) ρB B 2 (t0 ) B 2 (t0 ) −11 B(t0 ) B 2 (t0 ) ΩB = = 10 , (3.17) ρcr 8πρcr 2Λ4 10−9 G 2Λ4with ρcr = 3Hb (t0 )/κ = 8.1h2 10−47 GeV4 (h = 0.72 is the little-h constant), and B(t0 ) is the 2present magnetic ﬁeld amplitude. From eq. (3.13) then follows δ−1 ∆α = K e2 (zdec ) . (3.18) 4δwhere e(zdec )2 the eccentricity (3.15) evaluated at the decoupling z = 1100.3.4 Constraints on parameter Λ from extragalactic B strengths in an ellipsoidal UniverseTo make an estimate on the parameter δ, we need the order of amplitude of the presentmagnetic ﬁeld strength B(t0 ). In this respect, observations indicate that there exist, incluster of galaxies, magnetic ﬁelds with ﬁeld strength (10−7 − 10−6 ) G on 10 kpc - 1 Mpcscales, whereas in galaxies of all types and at cosmological distances, the order of magnitudeof the magnetic ﬁeld strength is ∼ 10−6 G on (1-10) kpc scales. The present acceptedestimations is [22]3 B(t0 ) 10−9 G . (3.20)Moreover, for an ellipsoidal Universe the eccentricity satisﬁes the relation 0 ≤ e2 < 1. Thecondition e2 > 0 means Fδ > 0, with Fδ deﬁned in (3.16). The function Fδ given by eq. (3.16)is represented in ﬁgure 1. Clearly the allowed region where Fδ is positive does depend onthe redshift z. On the other hand, the condition e2 < 1 poses constraints on the magneticﬁeld strength. By requiring e2 < 10−1 (in order that our approximation to neglect e2 -termsin (3.14) holds), from eqs. (3.15)–(3.17) it follows B(t0 ) 9 × 10−8 G . (3.21) 3 The bound (3.19) is consistent with the estimation on the present value of the magnetic ﬁeld strengthobtained from Big Bang Nucleosynthesis (BBN). As before pointed out, the magnetic ﬁelds scales as B ∼ b−2where the scale factor does depend on the temperature T and on the total number of eﬀectively massless −1/3degree of freedom g∗S as b ∝ g∗S T −1 [26]. The upper bound on the magnetic ﬁeld at the epoch of theBBN is given by [27] B(TBBN ) 1011 G, where according to the standard cosmology TBBN = 109 K 0.1MeV.Referred to the present value of the magnetic ﬁeld, the bound on B(TBBN ) becomes [20, 24] „ «2/3 „ «2 g∗S (T0 ) T0 B(t0 ) = B(TBBN ) 6 × 10−7 G , (3.19) g∗S (TBBN ) TBBNwhere T0 = T (t0 ) 2.35 × 10−4 eV and g∗S (TBBN ) g∗S (T0 ) 3.91 [26]. –7–
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F∆ 73 000 72 800 z 1100 72 600 72 400 ∆ 0.85 0.90 0.95 1.00 JCAP03(2011)033 F∆ 1. 106 800 000 600 000 z 1100 400 000 200 000 ∆ 1.05 1.10 1.15 1.20 200 000 400 000Figure 1. In this plot is represented Fδ vs δ for δ ≤ 1 (upper plot) and δ ≥ 1 (lower plot). Thecondition that the eccentricity is positive follows for Fδ > 0. It must also be noted that such magnetic ﬁelds does not aﬀect the expansion rate of theuniverse and the CMB ﬂuctuations because the corresponding energy density is negligiblewith respect to the energy density of CMB.4 Light propagation in NLED and birefringenceIn this section we discuss the modiﬁcation of the light velocity (birefringence eﬀect) for themodel of nonlinear electrodynamics L(X, Y ). We shall follow the paper [32] (see also [2, 33]),in which is studied the propagation of wave in local nonlinear electrodynamics by making useof the Fresnel equation for the wave covectors kµ . The latter are related to phase velocity k0 ˆ ˆv of the wave propagation by the relation ki = ki , where ki are the components of the vunit 3-covector. Thus, in what follows we conﬁne ourselves to the phase velocity. It isstraightforward to show that for the models under consideration (2.4) the group velocity isalways greater or equal to the phase velocity [32]. The main result in ref. [32] corresponds to the optic metric tensors µν √ g1 = X gµν + (Y + Y − X Z)tµν , (4.1) µν µν √ µν g2 = X g + (Y − Y − X Z)t , (4.2)which describe the eﬀect of birefringent light propagation in a generic model for nonlinearelectrodynamics. The quantities X , Y, and Z are related to the derivatives of the LagrangianL(X, Y ) with respect to the invariant X and Y , and tµν = F µα F ν . α –8–
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For our model, expressed by eq. (2.4), the quantities X , Y, and Z are given by 2 γ 2 δ2 2(δ−1) γ 2 δ2 X ≡ K1 = X , Y ≡ K1 K2 = (δ − 1)X 2(δ−1)−1 , Z = 0, 4 4 ∂L ∂2Lwhere K1 = 4 and K2 = 8 , while the metrics (4.1) and (4.2) are ∂X ∂X 2 µν µν g1 = K1 (K1 gµν + 2K2 tµν ) , g2 = K1 gµν . 2As a consequence, birefringence is present in our model. This means that some photons prop- JCAP03(2011)033agate along the standard null rays of spacetime metric gµν , whereas other photons propagatealong rays null with respect to the optical metric K1 gµν + 2K2 tµν . The velocities of the light wave can be derived by using the light cone equations (eﬀectivemetric) µν µν g1 kµ kν = 0 and g2 kµ kν = 0 .It is worthwhile to report the general expression for the average value of the velocity scalar [32] 4 T 00 (Y + Zt00 ) 2 2Y 2 − X Z + Z(t00 )2 + 2YZt00 v2 = 1 + + S2 3 X + 2Yt00 + Z(t00 )2 3 [X + 2Yt00 + Z(t00 )2 ]2where T 00 = −t00 + X = (E2 + B2 )/2 (t00 = −E2 ), and S2 = δµν t0µ t0ν , where S = E × B γ γ γis the energy ﬂux density. The subscript γ is introduced for distinguishing the photon ﬁeldfrom the magnetic background. The value of the mean velocity has been derived averagingover the directions of propagation and polarization. For our model, we get v2 1 + (δ − 1)R + (δ − 1)2 S , (4.3) 4 T 00 4 S2 R≡ , S= 3 4X + 2(δ − 1)t00 3 [4X + 2(δ − 1)t00 ]2 The high accuracy of optical experiments in laboratories requires tiny deviations fromstandard electrodynamics. This condition is satisﬁed provided |δ − 1| 1. Moreover, thereare two aspects related to (4.3): • The average velocity does depend on (only) the parameter δ, so that γ or Λ in our model can be ﬁxed independently. This task is addressed in the next section. • Because R is positive, one has to demand that δ − 1 < 0 in order that v 2 < 1.The above considerations hold for ﬂat spacetime, and can be straightforwardly generalizedto the case of curved space time [32].5 Stokes parameters, rotated CMB spectra and constraints on parameter ΛThe propagation of photons can be described in terms of the Stokes parameters I, Q, U ,and V . The parameters Q and V can be decomposed in gradient-like (G) and a curl-like(C) components [30] (G and C are also indicated in literature as E and B), and characterizethe orthogonal modes of the linear polarization (they depend on the axes where the linear –9–
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polarization are deﬁned, contrarily to the physical observable I and V which are independenton the choice of coordinate system). The polarization G and C and the temperature (T ) are crucial because they allow tocompletely characterize the CMB on the sky. If the Universe is isotropic and homogeneousand the electrodynamics is the standard one, then the T C and GC cross-correlations powerspectrum vanish owing to the absence of the cosmological birefringence. In presence of thelatter, on the contrary, the polarization vector of each photons turns out to be rotated bythe angle ∆α, giving rise to T C and GC correlations. Using the expression for the power spectra ClXY ∼ dk[k2 ∆X (t0 )∆Y (t0 )], where X, Y =T, G, C and ∆X are the polarization perturbations whose time evolution is controlled by theBoltzman equation, one can derive the correlation for T , G and C in terms of ∆α [14]4 JCAP03(2011)033 Cl T C = ClT C sin 2∆α , Cl T G = ClT G cos 2∆α , (5.1) 1 Cl GC = C GG − ClCC sin 4∆α , (5.2) 2 l Cl GG = ClGG cos2 2∆α + ClCC sin2 2∆α , (5.3) CC Cl = ClCC 2 cos 2∆α + ClGG sin2 2∆α . (5.4) The prime indicates the rotated quantities. Notice that the CMB temperature powerspectrum remains unchanged under the rotation. Experimental constraints on ∆α have been put from the observation of CMB polariza-tion by WMAP and BOOMERanG [14, 25]. ∆α = (−2.4 ± 1.9)◦ = [−0.0027π, −0.0238π] . (5.5)The combination of eqs. (5.5) and (3.18), and the laboratory constraints |δ − 1| 1 allow toestimate Λ.5.1 Estimative of ΛTo estimate Λ we shall write B = 10−9+b G b 2, (5.6) 3/2 Fδ = 2z z = 1100 1. (5.7)The bound (5.5) can be therefore rewritten in the form 10−3 10−2 |δ − 1| , (5.8) A Awhere 4 δ−1 9K (0) −6+2b −56+2b GeV A≡ Fδ ΩB K 10 0.24 × 10 . (5.9) 14 ΛThe condition |δ − 1| 1 requires A 1. It turns out convenient to set A = 10a , a > O(1) . (5.10) 4 Notice that in ref. [29] the analysis did not include the rotation of the CMB spectra, and in ref. [30] theanalysis focused on only the TC and TG modes. Other approximated approaches to discuss the rotation anglecan be found in refs. [28, 31]. – 10 –
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Log GeV Log GeV ∆ 1 10 7 35 7 ∆ 1 10 25 b 0 30 b 1 a 4 25 a 4 20 x 19 20 x 19 15 15 10 10 5 K K 22 026.2 22 026.2 22 026.3 22 026.3 2980.91 2980.92 2980.93 2980.94 Log GeV Log GeV 1000 ∆ 1 10 10 ∆ 1 10 10 JCAP03(2011)033 b 0 3000 b 1 500 a 7 a 7 2000 x 19 K 442 413 442 413 442 414 442 414 1000 x 19 500 K 59 874.1 59 874.1 59 874.1 59 874.1 59 874.2 59 874.2 1000 1000Figure 2. Λ vs K for diﬀerent values of the parameter δ − 1, a and b. The parameter a is related tothe range in which δ − 1 varies, i.e. −10−3−a δ − 1 −10−2−a , while b parameterizes the magneticﬁeld strength B = 10−9+b G. The red-shift is z = 1100. Plot refers to Planck scale Λ = 10Λx GeV,with Λx=P l = 19. Similar plots can be also obtained for GUT (ΛGUT = 16) and EW (ΛEW = 3)scales.From eqs. (5.9) and (5.10) it then follows 1 − 4(δ−1) −14+b/2 1 a−2b+6 Λ = 10 10 GeV , (5.11) Kor equivalently Λ b (−1) Log = −14 + + [a − 2b + 6 − LogK] . (5.12) GeV 2 4(δ − 1) The constant K can now be determined to ﬁx the characteristic scale Λ. WritingΛ = 10Λx GeV, where Λx=P l = 19, ΛGUT = 16 and ΛEW = 3 for the Planck, GUT andelectroweak (EW) scales, respectively, eq. (5.12) yields 4(δ − 1)Λx K = 10a−2b+6− , ≡ 1. (5.13) 14 − b/2In ﬁgure 2 is plotted Log(Λ/GeV) vs K for ﬁxed values of the parameters a, b and δ − 1.Similar plots can be derived for GUT and EW scales6 Discussion and closing remarksIn conclusion, in this paper we have calculated, in the framework of the nonlinear electro-dynamics, the rotation of the polarization angle of photons propagating in a Universe withplanar symmetry. We have found that the rotation of the polarization angle does depend on – 11 –
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the parameter δ, which characterizes the degree of nonlinearity of the electrodynamics. Thisparameter can be constrained by making use of recent data from WMAP and BOOMERang.Results show that the CMB polarization signature, if detected by future CMB observations,would be an important test in favor of models going beyond the standard model, includingthe nonlinear electrodynamics. Some comments are in order. In our investigation we have assumed that the planar-symmetry is induced by a magnetic ﬁeld. This is not the unique case. In fact, a planargeometry can also be induced by topological defects, such as cosmic string (cs) or domainwall (dw) [20]. In such a case, one has [20] 2 (0) 3 JCAP03(2011)033 e2 = Ωdw + 4(1 + z)3/2 − 7 , (6.1) 7 (1 + z)2 dwand 4 3 e2 = Ω(0) cs + 2(1 + z)3/2 − 5 , (6.2) 5 (1 + z) cs (0)where are the present energy densities, in units of critical density, of the domain wall Ω(dw,cs)and cosmic string. At the decoupling, one obtains (0) Ωdw e2 (zdec ) 10−4 , (6.3) 5 × 10−7 dwand (0) Ωcs e2 (zdec ) 10−4 . (6.4) 4 × 10−7 csThe analysis leading to determine the bounds on δ from CMB polarization goes along theline above traced. Moreover, a complete analysis of the planar-geometry is required to ﬁx the parameterδ. From a side, in our calculations in fact we have assumed that the Universe is matterdominated. A more precise calculation should require to use (to solve (3.14)) the relation z 1 1+z t= dz , (6.5) H0 0 Ωm (1 + z)3 + ΩΛwhere Ωm = 0.3, ΩΛ = 0.7 and H0 = 72 km sec−1 Mpc−1 (z = 1100). From the other side,a complete study of the eq. (3.14) is necessary in order to put stringent constraints on theparameter δ. As closing remark, we would like to point out that the approach to analyze the CMBpolarization in the context of NLED that we have presented above can also be applied todiscuss the extreme-scale alignments of quasar polarization vectors [36], a cosmic phenomenonthat was discovered by Hutsemekers [34] in the late 1990’s, who presented paramount evidencefor very large-scale coherent orientations of quasar polarization vectors (see also Hutsemekersand Lamy [35]).5 As far as the authors of the present paper are awared of, the issue has 5 Hutsemekers and Lamy, and collaborators, have presented, in a long series of papers (not all cited here)published over the period 1998 to 2008, a tantamount evidence that the alignment of quasar polarizationvectors is a factual cosmological enigma deserving to be properly addressed in the framework of the standardmodel of cosmology. The papers quoted here are intended to call to the attention of attentive readers theparamount evidence presenting this cosmic phenomenon. – 12 –
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remained as an open cosmological connundrum, with a few workers in the ﬁeld having focusedtheir attention on to those intriguing observations. Nonetheless, we quote “en passant” thatin a recent paper [37] Hutsemekers et al. discussed the possibility of such phenomenon to beunderstood by invoking very light pseudoscalar particles mixing with photons. They claimedthat the observations of a sample of 355 quasars with signiﬁcant optical polarization presentstrong evidence that quasar polarization vectors are not randomly oriented over the sky, asnaturally expected. Those authors suggest that the phenomenon can be understood in termsof a cosmological-size eﬀect, where the dichroism and birefringence predicted by a mixingbetween photons and very light pseudoscalar particles within a background magnetic ﬁeldcan qualitatively reproduce the observations. They also point out at a ﬁnding indicating that JCAP03(2011)033circular polarization measurements could help constrain their mechanism. Since cosmic magnetic ﬁelds have a typical strength of ∼ 10−7 − 10−8 G, on average,for a characteristic distance scale of 10-30 Mpc, it is our view that such phenomenology canbe understood in the framework of a nonlinear description of photon propagation (NLED)over cosmic background magnetic ﬁelds and the use of a planar symmetry for the space-time.Speciﬁcally, phenomena involving light propagation as dichroism and birefringence can beinscribed on to the framework of Heisenberg-Euler NLED, which predicts the occurrence ofbirefringence on cosmological distance scales. We plan to present such analysis in a forth-coming communication [38].AcknowledgmentsThe authors express their gratitude to the referee for relevant comments. The authors alsothank Prof. Xin-min Zhang, and Dr. Mingzhe Li for reading the manuscript and theirsuggestions. H.J.M.C. thanks ICRANet International Coordinating Center, Pescara, Italyfor hospitality during the early stages of this work. G.L. acknowledges the ﬁnancial supportof MIUR through PRIN 2006 Prot. 1006023491− 003, and of research funds provided by theUniversity of Salerno. H.J.M.C. is fellow of the Ceara State Foundation for the Developmentof Science and Technology (FUNCAP), Fortaleza, Ceara, Brazil.References [1] M. Born, Modiﬁed Field Equations with a Finite Radius of the Electron, Nature 132 (1933) 282; On the Quantum Theory of the Electromagnetic Field, Proc. Roy. Soc. A 143 (1934) 410; M. Born and L. Infeld, Electromagnetic Mass, Nature 132 (1933) 970; M. Born and L. Infeld, Foundations of the New Field Theory, Proc. Roy. Soc. A 144 (1934) 425; W. Heisenberg and H. Euler, Consequences of Dirac’s theory of positrons, Z. Phys. 98 (1936) 714 [physics/0605038]. J.S. Schwinger, On gauge invariance and vacuum polarization, Phys. Rev. 82 (1951) 664 [SPIRES]. [2] S.A. Gutierrez, A.L. Dudley and J.F. Plebanski, Signals and discontinuities in general relativistic nonlinear electrodynamics, J. Math. Phys. 22 (1981) 2835 [SPIRES]; J.F. Plebanski, Lectures on nonlinear electrodynamics, monograph of the Niels Bohr Institute, Nordita, Copenhagen (1968). [3] P.V. Moniz, Quintessence and Born-Infeld cosmology, Phys. Rev. D 66 (2002) 103501 [SPIRES]; R. Garcia-Salcedo and N. Breton, Born-Infeld cosmologies, Int. J. Mod. Phys. A 15 (2000) 4341 [gr-qc/0004017] [SPIRES]; – 13 –
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