CERN-PH-TH/2007-135 Anomaly induced effects in a magnetic field

# Cern-Ph-Th/2007-135 Anomaly induced effects in a magnetic field

Ignatios Antoniadis  ,   Alexey Boyarsky  ,   Oleg Ruchayskiy
Department of Physics, CERN - Theory Division, 1211 Geneva 23, Switzerland
Ecole Polytechnique Fédérale de Lausanne, Institute of Theoretical Physics
FSB/ITP/LPPC, BSP 720, CH-1015, Lausanne, Switzerland
On leave from CPHT (UMR CNRS 7644) Ecole Polytechnique, F-91128 PalaiseauOn leave of absence from Bogolyubov Institute of Theoretical Physics, Kyiv, Ukraine
###### Abstract

We consider a modification of electrodynamics by an additional light massive vector field, interacting with the photon via Chern-Simons-like coupling. This theory predicts observable effects for the experiments studying the propagation of light in an external magnetic field, very similar to those, predicted by theories of axion and axion-like particles. We discuss a possible microscopic origin of this theory from a theory with non-trivial gauge anomaly cancellation between massive and light particles (including, for example, millicharged fermions). Due to the conservation of the gauge current, the production of the new vector field is suppressed at high energies. As a result, this theory can avoid both stellar bounds (which exist for axions) and Â the bounds from CMB considered recently, allowing for positive results in experiments like ALPS, LIPPS, OSQAR, PVLAS-2, BMV, Q&A, etc.

## 1 Introduction

A number of experiments, studying the properties of vacuum in a strong external magnetic field (in particular the propagation of light in such a field), have been performed over the recent years, or are being in operation at the moment [1, 2, 3, 4, 5, 6, 7, 8, 9, 10, 11]. One of the main motivations for these experiments is the search for a hypothetical particle, the axion, which was originally predicted [12, 13] by the Peccei-Quinn mechanism of solving the “strong CP problem” in QCD [14, 15]. The main property of this particle from the laboratory experiments’ point of view is the coupling of the axion field to the photon via the interaction term . More generally, axion-like-particles (ALP) are pseudo-scalars which interact with ,111We denote by the dual field strength: . but may not have other properties of the QCD axion needed to solve the strong CP problem.

In [16] and [17, 18] another class of effective theories, which also predict effects in the presence of electric and magnetic fields, having completely different particle physics motivation, were considered. The coupling of axion to appears in general from chiral gauge anomalies, that may be present in theories with chiral couplings of fermions to a gauge field. Although gauge anomaly makes theory inconsistent, the theories with several chiral fields may be well-defined if the overall anomaly cancels and the overall gauge current is conserved. The fact that the net vacuum current is conserved does not mean that it is zero. If it is not, the non-trivial anomaly cancellation between heavy and light fields may give rise to experimental signatures of the heavy fields which, due to the topological nature of anomalies, are not suppressed by the mass of the heavy fermions and, therefore, may be observed at low energies [18]. For theories with non-trivial electromagnetic anomaly cancellations, such effects will be proportional to .

In this paper, we discuss in more details the theory considered in [16] and, in particular, show how the creation of the new light particles, present there, may be suppressed with energy and, therefore, the parameters of the theory may not be constrained by the stellar bounds, which severely restrict the parameter space of axions (for a recent review, see e.g. [19]). We describe the possible origin of the effective Lagrangian of [16] and show that it may appear, for example, from a theory of millicharged fermions, interacting with the photon and a “paraphoton” similar to the theory considered in [20, 21]. This allows to have the effects of vacuum dichroism and birefringence [22, 23] and “shining light through the wall” [24], observable in experiments like PVLAS [25], OSQAR [7], ALPS [26, 8], BMV [9, 10], LIPPS [11] avoiding not only the stellar constraints for the Chern-Simons like interaction of the paraphoton, but also the bounds on the parameters of millicharged particles discussed in [27].

The organization of the paper is as follows. In Section 2, we review the effective field theory of [16] that introduces a new massive vector boson, coupled to the photon via a Chern-Simons term, and study the propagation of light in a magnetic field. At low energies, this theory behaves like a theory of ALP corresponding to the longitudinal component of the new gauge field. In Section 3, we modify it at high energies, so that the gauge boson couples to a conserved current, suppressing the production of its longitudinal component in stars. This modification is parametrized by effective non-local terms. We then provide an example of a microscopic theory reproducing these terms, using millicharged fermions. We also analyze the various experimental constrains and deduce the allowed parameter space that leaves open the possibility of detecting interesting effects in forthcoming experiments, such as measuring dichroism and birefringence of light and photon regeneration in the presence of strong magnetic fields. Section 4 contains our concluding remarks and a discussion on possible derivation of our model from D-brane constructions.

## 2 Effective theory at low energies and propagation of light in the magnetic field.

We start by reminding the model considered in [16]. We consider the effective theory of two vector fields: the usual photon and a massive field (paraphoton):222To simplify the notations and avoid proliferation of non-essential -tensors, we will often use differential forms, such as instead of and instead of .

 Slow=∫d4x(−14F2A−14F2B+m2B2(Dμθ)2+m2γ2(Dμχ)2+2κDχ∧Dθ∧FA) (1)

where , and is a dimensionless coupling. The Stuckelberg field makes the action explicitly gauge invariant under gauge transformations, provided that when . The field is therefore massive with mass . Another Stuckelberg field , transforming as when , restores the gauge invariance with respect to the gauge group. This means that the photon is also massive with mass . This becomes explicit in the unitary gauge (, ):

 Slow,unitary=∫d4x(−14F2A−14F2B+m2B2B2μ+m2γ2A2μ+2κA∧B∧FA) (2)

Notice, that sending (and making the field non-dynamical) will make massless and add the constraint (with the field being a Lagrange multiplier). To make the analysis simpler, we will assume massless photon and the action (2) supplemented by this constraint, although our analysis remains unchanged in the case of finite but small enough . The Chern-Simons (CS) term remains gauge invariant in this case. Notice, that in the theory (1) the field couples to a non-conserved current :

 (JμB)low=δSlowδBμ=κϵμνλρAνFλρ;∂μ(JμB)low=κ2ϵμνλρFμνFλρ (3)

The conserved (Nöther) current is a linear combination of and . As we will show below, the property (3) implies that in the theory (1) the longitudinal part of the massive vector field behaves as a massive axion with the mass  and the coupling constant .

### 2.1 Propagation of light in a magnetic field

Let us consider the equations of motion of theory (1) for the case of the propagation of photons in Ð° strong external magnetic field. We consider light propagation along the -axis in the magnetic field , pointing in -direction. Under the condition , the CS term does not depend on the choice of the background vector potential. For simplicity we choose the background vector potential, corresponding to the field , in the form . Working in the unitary gauge (i.e. ) for the -field, we obtain the following system of equations:

 ∂νFμν =−κϵμνλρ(2BνFλρ−AνFBλρ) (4) ∂νFμνB−m2BBμ =κϵμνλρAνFλρ (5) ϵμνλρFμνFBλρ =0 (6)

One can construct the solution of these equations as perturbations in small parameter around the “zeroth order approximation”: , .

A simple analysis shows that only the longitudinal part of (i.e. longitudinal electric field ) interacts with the propagating photon, with polarization parallel to the external magnetic field. To demonstrate the similarities and differences between this model and the axion, we revert from eqs. (4-5) to the system, involving the longitudinal degree of freedom of the -field and the photon .333We choose the gauge in which the plane wave, with polarization vector parallel to the external magnetic field is described by the potential . Namely, one can represent the field in terms of one scalar degree of freedom, :

 Bμ=1mB∂μϕ+δμ0~B0i.e.⎧⎪ ⎪⎨⎪ ⎪⎩Bz=∂zϕmBB0=∂0ϕmB+~B0 (7)

Notice that there is a residual uncertainty in the definition of : one can simultaneously shift and . Clearly, .

To establish the connection between and we consider the Maxwell’s equation:

 iωFB0z+mB∂zϕ=−2κ¯Ay(z)(iωAx), (8)

which gives

 ~B0=mBiωϕ+2κz∫¯Ay(z′)Ax(z′)dz′. (9)

Taking the derivative of eq. (5) we arrive to the first class constraint which massive vector fields should obey

 ∂μBμ=−κ2m2BϵμνλρFμνFλρ=−4κH0(iωAx)m2B (10)

Putting relations (7), (9) into the constraint (10) we obtain

 (□+m2B)ϕ=−4κH0iωAxmB−2iκmBωz∫¯Ay(z′)Ax(z′)dz′ (11)

Next, we analyze the e.o.m. for the field :

 □Ax (12) =+2κmBiω∂zϕ¯Ay+4κ2¯A2yAx

The propagation of light, polarized perpendicularly to the magnetic field (component ), is not modified in this theory, as follows trivially from the structure of currents in the right hand side of eqs. (4)–(5).

Let us compare eqs. (11)–(12) to the pure axion case:

 ∂νFμν =1Mϵμνλρ(∂νϕ)Fλρ (13) (□+m2a)ϕ =14MϵμνλρFμνFλρ

For the propagation of linearly polarized light, parallel to the magnetic field equations (13) reduce to

 (□+m2a)ϕ =−2iωMAxH0 (14) □Ax =2iωH0Mϕ

We see that under the identification

 1M↔2κmB;ma↔mB (15)

equations (11)–(12) reduce to (14) plus some additional (non-local) terms, depending on the background potential .444The term in eq. (12) is subleading, as compared to the first term and does not change the results of our analysis in any essential way. These terms, however, are suppressed (as compared to those, depending on the field ). The easiest way to see it, is to send , while keeping the ratio fixed. Thus, equations (11)–(12) are reduced into those of massless axion. This leads to the dichroism , where is the distance traveled by the light. For finite , corrections suppressed by powers of will appear.

## 3 Possible microscopic origin of the theory.

### 3.1 Decoupling of the longitudinal polarization at high energies

In quantum electrodynamics, if one adds a small photon mass , all the processes, involving the third (longitudinal) degree of freedom, are suppressed at energies as . This is due to the fact that the electromagnetic field couples to a conserved current, which is a consequence of gauge invariance of the theory. On the other hand, if the current is not conserved, at high energies processes involving the longitudinal polarization of the vector boson are equivalent to those involving the longitudinally coupled scalar due to the so called Goldstone boson equivalence theorem [28]

This is what happens in theory (1). Although the theory is gauge invariant under the gauge symmetry, it is realized by simultaneous gauge transformations of the -field and the Stuckelberg field . As we saw in Section 2.1, the field couples to the non-conserved current (3) and therefore its longitudinal polarization behaves as an axion (for ).

However, the theory (1) is an effective field theory, valid up to a certain energy scale . In many cases it naturally happens that for the theory gets modified in such a way that the current, to which the -field couples becomes conserved. Then, all processes involving emission or absorption of the longitudinal polarization of are suppressed as . On the other hand, we are interested in the situation, where the field can be produced at low laboratory energies. This puts restriction on its mass to be . Then at stellar energies one obtains a suppression of at least . For smaller values of  the suppression is even stronger. The theory of transverse -field with CS interaction does not resemble the theory of axion anymore. For example, the production of this field due to the CS interaction is strongly suppressed by the small value of the dimensionless CS coupling .

To illustrate this idea, assume that in the theory there is an additional particle with mass , interacting with the fields of the theory (1) and giving rise to an effective action of the following (schematic) form:

 S=∫d4x(−14F2A−14F2B+m2B2(Dθ2) + κA∧B∧FA + κθm2Ψ□+m2Ψ(F~F)−κ(∂μBμ)1□+m2Ψ(F~F))

In the next subsection we will present an example of a renormalizable field theory, which has such properties (recall that we always add to this theory the constraint to make it gauge invariant). At low energies (for ) one obtains the action (1) (formally taking ).

At high energies () the effective theory is of course non-local. We can neglect the interacting term proportional to in the action (3.1) and obtain

 S(ω≫mΨ)≈∫−14F2A−14F2B+m2B2Dμθ2+κA∧B∧FA−κ(∂μBμ)1□(F~F) (17)

At these energies, the field couples to the conserved current

 JμB=κ2ϵμνλρAνFλρ−κ∂μ□(F~F). (18)

Therefore, at energies the production of the longitudinally polarized -field in theory (3.1) is suppressed. Of course, for the current (18) should be computed directly in the microscopic theory producing the non-local terms in (3.1), containing additional particles, rather than in the non-local effective theory. Next we are going to present an example of such a microscopic theory.

### 3.2 Theory with millicharged fermions

Consider a theory with several sets of chiral fermions, whose masses are given by Yukawa interactions with Higgs fields and :

 L=∑i=1,2(i¯Ψito0.0pt$D$\large/Ψi+fi¯ΨiΦ1Ψi)+(i¯Ξito0.0pt$D$\large/Ξi+λi¯ΞiΦ2Ξi)+h.c. (19)

The fermions are charged with respect to , with one of the possible choices of charges shown in Table 1. Integrating out the fermions for energies below their masses, one obtains “anomalous” (CS-like) terms in the effective action :555Of course, integrating out these fermions, one obtains also terms leading to a renormalization of charges of the fields and , of the mass, possible generation of kinetic mixing between and , etc. However, in the case of chiral fermions, one expects additional contributions from “anomalous” (triangular) diagrams (shown in Figs. 12) (see e.g. [29]).

 S\textsccs=∫(e21−e22)q116π2θFA∧FA+κA∧B∧FA (20)

Only fermions contribute to the term (fermions are vector-like with respect to the gauge group and therefore do not interact with ). The contribution to the CS term comes from both sets of fermions. The interaction of the -field with the photon is very weak due to the small value of , therefore in the action (20) we omitted anomalous terms, containing more than one power of the -field.

The relation between the coefficient in front of the CS term and the fermion charges is dictated by the gauge invariance of the action with respect to gauge transformation

 κ=q1(e21−e22)16π2 (21)

The Higgs field which provides mass to the fermions is charged with respect to the with charge . If it acquires a vacuum expectation value (VEV) , one has and the Yukawa term for fields becomes . The Higgs then provides mass to the -field:

 mB=2q1vB (22)

and Higgs’s kinetic term becomes that of the field in action (1).

Let us take Yukawa couplings , so that fermions are much heavier that . Consider energies . The resulting expression for the current is given by the expression

 JμB=κ2ϵμνλρAνFλρ−κ∂μ□(F~F) (23)

which arises from the effective action

 Seff,high=∫κ(∂μBμ)1□FA∧FA+κA∧B∧FA (24)

(compare e.g. [30] where similar result for the massless chiral fermions is presented).

### 3.3 The parameters of the model

Next, we study the restrictions on the parameters of our model. First of all, notice that in order to expect positive outcome in laboratory experiments, which aim to measure dichroism and birefringence or photon regeneration (shining light through the wall), we need to have a mass of the -field to be within the energy reach of laboratory experiments:

 mB≲ωlab∼1 eV (25)

This means that

 vB≲1 eV/q1 (26)

Notice, that the charges of fermions with respect to the “paraphoton” are not restricted and therefore one may have . This will make  to be also in the sub-eV region.

When speaking about ALPs, it is convenient to characterize their interaction with the photon by the dimensionful coupling (see eqs. (13)). It follows from eq. (15) that in terms of the parameters of our model . Using then relations (21) and (22), we obtain the following expression for the interaction strength in terms of the parameters of the microscopic model:666We consider the case when .

 M∼vBe2Ψ (27)

For our analysis of the classical equations of motion to remain valid, the tree-level unitarity bound for processes involving massive vector bosons should not be saturated at all relevant energies. The saturation of this bound is reached at energies which is again .

There are various restrictions on the charges of new types of fermions with the electromagnetic field. First, laboratory bounds, coming from the contributions to the Lamb shift [31] and invisible orthopositronium decay [31] (based on the results of [32]) give . This translates into

 M≳108vB=0.1 GeV(vB eV) (28)

This bound is very weak. A stronger bound on the charges of millicharged fermions () with sub-eV masses comes from the requirement that such fermions do not distort the CMB spectrum too much [27]. However, this restriction is not applicable in our case as the mass of our fermions  (see discussion below).

The strongest bounds on charges of fermions with mass below comes from limiting the contribution of these particles to the energy transfer in stars [33] (see also [34]). This gives . This bound translates into the following lower bound on :

 M>1028vB=1019 GeV(vB eV) (29)

For instance, if we take (the sensitivity expected to be reached by the OSQAR experiment [7]), this would require . This would imply an extremely light field with and (which is still a possibility).

However, the mass  is not necessarily so small. In our model, the paraphoton field would acquire a kinetic mixing with the photon due to the loop corrections coming from light fermions. Therefore, the mechanism of additional suppression of the coupling of fermions with the photon in stars, similar to that proposed in [35], is possible. The restriction then becomes , i.e. the stellar bound of [33, 31] is weakened by at least six orders of magnitude. This would lead to the following bound

 M≳107 GeV(vB eV)5 (30)

with .

We are interested in the situation where at laboratory energies the effective action is given by (2). For this to be true, the mass of the fermions should be greater than laboratory energies . At the same time, the mass should be lower than the stellar energies for (23) to be true. Therefore the fermion mass  lies in the interval . As we saw in Section 3.1, in the limit the massive vector field is coupled to a conserved current and therefore its production in stars is suppressed at least as . At higher energies () additional contributions to the action (24) due to finite behave as . These terms contribute to the divergence of the current :

 ∂μJμB∼κ(mΨω% star)2ϵμνλρFμνFλρ (31)

This gives an additional contribution to the production of the longitudinally polarized -field, not suppressed by . However, in comparison with the low-energy expression (3), there is an additional suppression . For convenience, in what follows, we will characterize the interaction strength in terms of an energy dependent coupling constant :

 M(ω)∼mBκ(ωmΨ)2,ω>mΨ (32)

To determine the admissible values of , let us assume that one of the laboratory experiments (light propagation in a magnetic field or regeneration experiments) had positive outcome. This determines the value of . As a conservative estimate we take it to be equal to the laboratory lower bound, reported by PVLAS collaboration [6]: . This value is much lower than those coming from the astrophysical bounds: restriction from the helioseismology  [36, 37] and restrictions from the horizontal branch (HB) stars: (for a review see e.g. [34, 38, 19]). Demanding that the modification (32) at star energies is greater than these astrophysical bounds (which we will collectively call ), one arrives to the following restriction on the mass :

 mΨ≲ωstar√MlabMstar (33)

As an estimate for we take the plasma frequency in the stellar interim: for the Sun and for HB stars. As a result, we obtain using solar data or using restrictions from HB stars.

The recent bound from CAST collaboration [39, 40] would give the restriction on the mass of the fermions few eV. However, it should be noted that the present CAST bounds do not extend above axion masses . The model presented here allows (while still below ), therefore the CAST restrictions may not be applicable in our case.777The CAST Phase II will test the range of masses  [40] and will allow to probe further our model.

Additional restriction on the parameter space may come from the following fact. Integrating out fermions leads in general to terms suppressed by (as in any renormalizable field theory [41]). At laboratory experiment energies with , such contributions may still be significant. In particular, they contribute to the action the following terms (analogous to the Euler-Heisenberg corrections in quantum electrodynamics [42])

 SΨ=∫d4x245e4Ψm4Ψ(716(F~F)2+4(F2μν)2) (34)

These terms of course do not contribute to dichroism (as we consider ), while their contribution to birefringence is given by

 βψ∼(ωL)e4Ψm4ΨH02 (35)

Taking , (to maximize the value of (35)), and typical values for ,  m, and  T, one finds a value of birefringence – much below the current experimental limits.

Thus, the final range of allowed parameters of millicharge fermions ranges from

 vB≲1 eV;eΨ≲10−8;qΨ<1 (36)

to

 vB≲10−10 eV;eΨ≲10−14;qΨ<1 (37)

with the fermion mass .888The allowed window for  can become higher, if future laboratory experiments strengthen bounds of [6].

We see, that this range of parameters differs from those of Refs. [20, 21], which suggested that the PVLAS experiment can be explained by the existence of millicharged particles with and charges . Such millicharged particles, however, would introduce a distortion of CMB energy spectrum [27]. On the other hand, the millicharged particles with parameters (36)–(37) and vector field with parameters (30) can give rise to effects testable in present and forthcoming experiments (PVLAS, OSQAR, ALPS, LIPPS, BMV, Q&A): shining light through the wall and dichroism and birefringence of light propagating in strong magnetic field.999Note that as eq. (30) shows, taking  in the sub-eV range allows to have and thus explaining the effect of dichroism, reported by the PVLAS collaboration in 2006 [3]. To avoid the stellar constraints this would require to have . However, the contribution of these fermions to dichroism at laboratory energies is subleading compared to the corresponding contribution of the CS term (2), which differs this model from the one proposed in [21, 20].

## 4 Discussion

In this paper we presented a simple example of a theory in which non-trivial anomaly cancellation between light and heavy sectors gives rise to possible observable effects in optical laboratory experiments. We showed that the structure of the effective action changes at high energies, suppressing the production of light particles. Therefore the stellar constraints can be significantly weaker in this case, allowing for relatively strong optical effects, that may be observed in current or future experiments.

We would like to notice that although we have presented an explicit microscopic theory (19), which leads to the effective theory (3.1) we are interested in, the actual fundamental theory could be rather different. For example, instead of heavy set of fermions in the theory (19), the CS term may be generated by different mechanisms in the underlying high-energy theory.

Actually, the low-energy effective action (1) or (2) with the CS coupling can arise easily in D-brane realizations of the Standard Model [43, 29]. Indeed, gauge groups come often in unitary factors containing extra ’s. Moreover, the smallness of the mass and the CS coupling of the vector boson to the photon may be naturally explained in models of large extra dimensions and low string scale [44, 45]. For this, should propagate in the bulk of extra dimensions, while its mass should arise from localized anomalies due to chiral fermions present for instance in the intersections of the Standard Model branes with the brane extended in the bulk. Assuming for simplicity an homogeneous bulk of volume in string units and identifying the axion with the string scales , one has and . It follows that eV for TeV, in which case . On the other hand, the microscopic theory with millicharged fermions is more difficult to accommodate. One could imagine for instance that the hypercharge (or the electric charge) acquires a tiny mixing with the bulk gauge boson , creating millicharges, although it is not clear how to get a consistent setup with “natural” suppression.

Another example of a theory with non-trivial anomaly cancellation between light and heavy sectors, is in the presence of extra dimensions, discussed in [17, 18]. In this theory a plane wave, propagating in a strong magnetic field with polarization parallel to the field, is described by the equation

 1Δ(z)∂z(Δ(z)∂zAx)+□Ax=α2EMκ20→H2M25Δ2(z)Ax+O(κ0) (38)

This leads to the massive wave equation

 □Ax(x)−m2γHAx(x)=0 (39)

where the “magnetic mass”

 m2γH∼α\textscemκ0|→H| (40)

depends only on 4-dim quantities; it is not suppressed by the scale of the 5-dim theory . The wave equation for perpendicular to the magnetic field component remains the same (massless): .

This theory is drastically different from the models discussed in this paper (as well as other models, predicting non-trivial effects in strong magnetic fields). Namely, it does not contain any new light degrees of freedom. This means, that the regeneration experiments (“shining light through the wall”), as well as the measurements of dichroism will produce no results in this case. However the theory leads to an ellipticity (birefringence) of the linearly polarized light:

 Δϕ=m2γH2ωL∼κ0α%EM|→H|2ωL (41)

Actually, the static (“capacitor”) experiment suggested in [18] is also sensitive to the model described in this paper. As different models, predicting non-trivial results in optical experiments behave differently in this static experiment, it provides a good way to distinguish among them.

## Acknowledgements

We would like to thank M. Fairbairn, G. Raffelt and M. Shaposhnikov for useful discussions. This work was supported in part by the European Commission under the RTN contract MRTN-CT-2004-503369 and in part by the INTAS contract 03-51-6346. The work of A.B. was (partially) supported by the EU 6th Framework Marie Curie Research and Training network ”UniverseNet” (MRTN-CT-2006-035863). O.R. would like to thank Swiss Science Foundation.

## References

• [1] BFRT Collaboration, G. Ruoso et al., Limits on light scalar and pseudoscalar particles from a photon regeneration experiment, Z. Phys. C56 (1992) 505–508.
• [2] BFRT Collaboration, R. Cameron et al., Search for nearly massless, weakly coupled particles by optical techniques, Phys. Rev. D47 (1993) 3707–3725.
• [3] PVLAS Collaboration, E. Zavattini et al., Experimental observation of optical rotation generated in vacuum by a magnetic field, Phys. Rev. Lett. 96 (2006) 110406, [hep-ex/0507107].
• [4] PVLAS Collaboration, E. Zavattini et al., Pvlas: Probing vacuum with polarized light, Nucl. Phys. Proc. Suppl. 164 (2007) 264–269, [hep-ex/0512022].
• [5] S.-J. Chen, H.-H. Mei, and W.-T. Ni, Q & A experiment to search for vacuum dichroism, pseudoscalar-photon interaction and millicharged fermions, hep-ex/0611050.
• [6] PVLAS Collaboration, E. Zavattini et al., New pvlas results and limits on magnetically induced optical rotation and ellipticity in vacuum, arXiv:0706.3419 [hep-ex].
• [7] OSQAR Collaboration, P. Pugnat et al., Optical search for QED vacuum magnetic birefringence, axions and photon regeneration (OSQAR), . CERN-SPSC-2006-035.
• [8] ALPS Collaboration, K. Ehret et al., Production and detection of axion-like particles in a HERA dipole magnet: Letter-of-intent for the ALPS experiment, hep-ex/0702023.
• [9] BMV Collaboration, C. Rizzo, “Laboratory and astrophysical tests of vacuum magnetism: the BMV project.” 2nd ILIAS-CAST-CERN Axion Training, http://cast.mppmu.mpg.de, May, 2006.
• [10] BMV Collaboration, C. Robilliard et al., No light shining through a wall, arXiv:0707.1296 [hep-ex].
• [11] LIPPS Collaboration, A. V. Afanasev, O. K. Baker, and K. W. McFarlane, Production and detection of very light spin-zero bosons at optical frequencies, hep-ph/0605250.
• [12] S. Weinberg, A new light boson?, Phys. Rev. Lett. 40 (1978) 223–226.
• [13] F. Wilczek, Problem of strong P and T invariance in the presence of instantons, Phys. Rev. Lett. 40 (1978) 279–282.
• [14] R. D. Peccei and H. R. Quinn, CP conservation in the presence of instantons, Phys. Rev. Lett. 38 (1977) 1440–1443.
• [15] R. D. Peccei and H. R. Quinn, Constraints imposed by CP conservation in the presence of instantons, Phys. Rev. D16 (1977) 1791–1797.
• [16] I. Antoniadis, A. Boyarsky, and O. Ruchayskiy, Axion alternatives, hep-ph/0606306.
• [17] A. Boyarsky, O. Ruchayskiy, and M. Shaposhnikov, Observational manifestations of anomaly inflow, Phys. Rev. D72 (2005) 085011, [hep-th/0507098].
• [18] A. Boyarsky, O. Ruchayskiy, and M. Shaposhnikov, Anomalies as a signature of extra dimensions, Phys. Lett. B626 (2005) 184–194, [hep-ph/0507195].
• [19] G. G. Raffelt, Astrophysical Axion Bounds, Submitted to Lect. Notes Phys. (Nov., 2006) [hep-ph/0611350].
• [20] H. Gies, J. Jaeckel, and A. Ringwald, Polarized Light Propagating in a Magnetic Field as a Probe for Millicharged Fermions, Phys. Rev. Lett. 97 (Oct., 2006) 140402–+, [arXiv:hep-ph/0607118].
• [21] M. Ahlers, H. Gies, J. Jaeckel, and A. Ringwald, On the particle interpretation of the pvlas data: Neutral versus charged particles, Phys. Rev. D75 (2007) 035011, [hep-ph/0612098].
• [22] L. Maiani, R. Petronzio, and E. Zavattini, Effects of nearly massless, spin zero particles on light propagation in a magnetic field, Phys. Lett. B175 (1986) 359.
• [23] G. Raffelt and L. Stodolsky, Mixing of the photon with low mass particles, Phys. Rev. D37 (1988) 1237.
• [24] K. Van Bibber, N. R. Dagdeviren, S. E. Koonin, A. Kerman, and H. N. Nelson, An experiment to produce and detect light pseudoscalars, Phys. Rev. Lett. 59 (1987) 759.
• [25] M. Roncadelli, Behind Pvlas, arXiv:0706.4244 [hep-ph].
• [26] A. Ringwald, Photon regeneration plans, hep-ph/0612127.
• [27] A. Melchiorri, A. Polosa, and A. Strumia, New bounds on millicharged particles from cosmology, Phys. Lett. B650 (2007) 416–420, [hep-ph/0703144].
• [28] J. M. Cornwall, D. N. Levin, and G. Tiktopoulos, Derivation of gauge invariance from high-energy unitarity bounds on the s matrix, Phys. Rev. D10 (1974) 1145.
• [29] P. Anastasopoulos, M. Bianchi, E. Dudas, and E. Kiritsis, Anomalies, anomalous u(1)’s and generalized chern-simons terms, JHEP 11 (2006) 057, [hep-th/0605225].
• [30] A. Smailagic and E. Spallucci, Higher dimensional schwinger-like anomalous effective action, Phys. Rev. D62 (2000) 045010, [hep-th/0003293].
• [31] S. Davidson, S. Hannestad, and G. Raffelt, Updated bounds on milli-charged particles, JHEP 05 (2000) 003, [hep-ph/0001179].
• [32] T. Mitsui et al., Search for invisible decay of orthopositronium, Phys. Rev. Lett. 70 (1993) 2265–2268.
• [33] S. Davidson, B. Campbell, and D. C. Bailey, Limits on particles of small electric charge, Phys. Rev. D43 (1991) 2314–2321.
• [34] G. G. Raffelt, Stars as laboratories for fundamental physics: The astrophysics of neutrinos, axions, and other weakly interacting particles. University of Chicago Press, Chicago, USA, 1996.
• [35] E. Masso and J. Redondo, Compatibility of CAST search with axion-like interpretation of PVLAS results, Phys. Rev. Lett. 97 (2006) 151802, [hep-ph/0606163].
• [36] H. Schlattl, A. Weiss, and G. Raffelt, Helioseismological constraint on solar axion emission, Astropart. Phys. 10 (1999) 353–359, [hep-ph/9807476].
• [37] J. N. Bahcall, A. M. Serenelli, and S. Basu, New solar opacities, abundances, helioseismology, and neutrino fluxes, Astrophys. J. 621 (2005) L85–L88, [astro-ph/0412440].
• [38] G. G. Raffelt, Particle physics from stars, Ann. Rev. Nucl. Part. Sci. 49 (1999) 163–216, [hep-ph/9903472].
• [39] CAST Collaboration, S. Andriamonje et al., An improved limit on the axion-photon coupling from the CAST experiment, JCAP 0704 (2007) 010, [hep-ex/0702006].
• [40] CAST Collaboration, C. Eleftheriadis, Results on axion physics from the CAST experiment at CERN, arXiv:0706.0637 [hep-ex].
• [41] T. Appelquist and J. Carazzone, Infrared singularities and massive fields, Phys. Rev. D11 (1975) 2856.
• [42] W. Heisenberg and H. Euler, Consequences of dirac’s theory of positrons, Z. Phys. 98 (1936) 714–732, [physics/0605038].
• [43] I. Antoniadis, E. Kiritsis, J. Rizos, and T. N. Tomaras, D-branes and the Standard Model, Nucl. Phys. B 660 (June, 2003) 81–115, [hep-th/0210263].
• [44] N. Arkani-Hamed, S. Dimopoulos, and G. R. Dvali, The hierarchy problem and new dimensions at a millimeter, Phys. Lett. B429 (1998) 263–272, [hep-ph/9803315].
• [45] I. Antoniadis, N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, New dimensions at a millimeter to a fermi and superstrings at a TeV, Phys. Lett. B 436 (Sept., 1998) 257–263, [arXiv:hep-ph/9804398].
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