Photon propagation in a cold axion condensate

Photon propagation in a cold axion condensate

Abstract

We discuss some striking properties of photons propagating in a cold axion condensate oscillating coherently in time with a frequency . Three effects are discussed in this contribution: (a) due to the time dependence of the background, photons moving in the cold axion background have no definite energies and some momenta are not accessible to them. (b) we investigate the combined influence of a magnetic field and the cold axion background and propose a possible interferometric experiment to detect the latter. (c) if the axion condensate has a space dependence, the photon refraction index is modified in the medium, possibly leading to total reflection at the interface with the ordinary vacuum.

ICCUB-13-228

1 Introduction

Cold relic axions resulting from vacuum misalignment in the early universe are good candidates for dark matter[1, 2]. A coherent spatially constant axion field (it may be a genuine Peccei-Quinn axion[3] or a similar field) acquires a mass once instanton effects set in and oscillates

(1)

The energy density stored in these oscillations contributes to the energy-matter budget of the universe. This constitutes the cold axion background, or CAB for short.

As it is well known, the coupling of axions to photons is universal

(2)

The only arbitrariness lies in the coefficient but most models [4] give . Using \eqrefcos

(3)

Cosmology considerations place the axion mass in a range eV[2]. For Peccei-Quinn axions an approximate relation of the form holds, thus forcing the axion decay constant to be at least GeV. From astrophysics the limit GeV seems now well established. This makes the axion extremely long-lived and very weakly coupled.

In addition to the axion-photon coupling, as indicated above, axions can also couple to matter in specific models. However, the smallness of the coupling makes their detection extremely challenging. Nevertheless, some of the best bounds on axion masses and couplings do come from the study of abnormal cooling in white dwarfs due to axion emission[5].

In fact there are two separate questions we have to address. The first one is whether axions exist at all. This is what experiments such as CAST, AMDX, AMDXII, IAXO or ALPS try to address. If its mass turns out to be in the relevant range for cosmology we would indeed have a strong hint that axions may provide the elusive dark matter.

However, we would eventually like to verify or falsify the CAB hypothesis and determine to what extent cold axions contribute to the dark matter budget. Finding the axion particle with the appropriate properties is not enough. Unfortunately a direct experimental confirmation of the CAB is extremely difficult and it could possibly be accomplished only via some collective effect on the propagation of particles. Looking for the effect of the CAB on photon propagation is the most natural possibility.

In a previous Patras meeting we reported on three effects that the presence of a CAB induces on photon propagation[6]. The CAB modifies the photon dispersion relation introducing a Lorentz non-invariant term, which makes Bremsstrahlung from cosmic rays possible. The amount of energy radiated by this process was computed and found to be non-negligible[7], but normal synchrotron radiation background is a tough enemy for its detection. The second effect discussed was the presence of an additional rotation in the polarization plane of light (on top of the familiar one[8], see [9] for a detailed discussion). The third effect discussed is that some photon wave-lengths are actually forbidden in a universe filled with cold axions oscillating coherently[9]. In this talk we will continue our discussion on the last two points, and also speculate very briefly on possible consequences of having a CAB with some spatial dependence.

In order to determine the properties of photons in a CAB we need to solve the equation of motion in momentum space. For the time being let us ignore the magnetic field.

(4)

where . We shall approximate the sinusoidal variation with of the axion background by a piecewise linear function (see figure). The astrophysical and observational bounds on range from to eV. The quantity changes alternatively from positive to negative with a period . Within each period of oscillation two complex and space-like chiral polarization vectors can be defined (see [10]). The two polarization vectors are solutions of the vector field equations if and only if

(5)

2 Forbidden wavelengths

Using this approximation of replacing the CAB oscillation by a piecewise-linear function, as shown in the figure, we can solve exactly for the propagating modes.

The equation for is

(6)

We write and demand that have the same periodicity as . This requires the fulfillment of the condition

(7)

where coincide with the two frequencies .

A close inspection of the solutions to the previous equation reveals the existence of momentum gaps: some values of admit no solution for . The phenomenon is visible for large values of the dimensionless ratio .

In a universe filled with cold axions oscillating with a period some wavelengths are forbidden by a mechanism that is similar to the one preventing some energies from existing in a semiconductor. See [9] for more details. Unfortunately, for realistic values of the gaps are probably far too small to be seen. Their width is actually proportional to

3 Adding a magnetic field

If the theoretical technology is well known. It amounts to resumming the Feynman diagrams shown below.

Interaction with the cold axion background implies that we need to take into account also the diagrams that include interaction with the CAB

This can be done and the resulting resummed propagator can fe found in [9], where we examined the evolution of the polarization plane under the joint influence of the magnetic field and the CAB.

The relevant parameters are and , where is the magnetic field. Taking as a reference value (just to set an approximate range of variation for ) GeV (this would correspond for PQ axions to eV) and then and . However, we shall consider and (and obviously ) to be free parameters.

The relevant evolution equations are

(8)

We try a solution of the form: :

(9)

Within each period of oscillation the proper frequencies are in the limit

(10)
(11)
(12)

To be compared with the proper modes without magnetic field

(13)

Note that one should not attempt to take the limit above because we assume . The natural basis is now parallel and perpendicular (to the magnetic field) rather than left or right polarization. Notice that the proper frequencies in this natural basis and in this limit contain only even powers of and hence do not change when changes sign. Unlike the case both modes are in an eigenstate of energy. We do not expect momentum gaps.

Numerically for eV (a magnetic field of T for GeV), eV and keV, the relevant terms are

(14)
(15)

The splitting between the two polarizations goes as

(16)

The relevance of the CAB is somehow enhanced by the magnetic field and dominates for

(17)

The difference (16) is very small; typically it could be as “large” as eV. Small as this number is, it should be remembered that Michelson-Morley type experiments can detect differences in frequencies with 17 significant figures[11]. If so, by tuning the magnetic field one should be able to switch in and out the effect of the CAB and perhaps “seeing” it.

There is also a change in the plane of polarization with an angle

(18)

(for “large” axion masses, the actual result is more complicated). This angle could be be as large as . What this means is that the plane of polarization changes from period to period. Of course the change is not instantaneous and a more complete description of the evolution can be found with the help of the photon correlator derived in [9]. The evolution of the plane of polarization with respect to the case has a new component due to the CAB.

The rotation survives even without magnetic field and the effect is independent of the frequency. Note that the previous result holds only for table-top experiments when the photon can approximately be considered an eigenstate of energy, i.e. when the time-of-flight of the photon, , is smaller than . This means and the method could perhaps be useful for very small axion masses.

Due to the smallness of the numbers involved it is somewhat dangerous to rely on approximate formulae - many scales play in the game. In a forthcoming paper[12] a detailed numerical analysis will be performed.

4 Crossing the boundary

Let us finish with a few words on the third topic that was discussed in our presentation. This is work done in collaboration with A. Andrianov and S. Kolevatov and it will be described very succintly here. We refer the readers to [13] for more details.

We want to explore different possible axion backgrounds (other than the cold background oscillating in time with period ). Consider the term in the lagrangian

(19)

This associates a space-like boundary with a space-like vector

(20)

The Lorentz invariance violating vector has been renamed from to to avoid confusion with the CAB case.

Although not totally realistic for astrophysical purposes, this would correspond to a region where a linearly decreasing axion density meets the vacuum. For convenience the “wall” is placed in the direction at . Matching on the boundary leads to

(21)

Different polarizations have different dispersion relations in the axion phase

(22)

that have to be matched to the usual dispersion law in the normal phase ( is the photon mass and need not be zero, due to plasma effects)

(23)

This actually leads to a non-trivial reflection coefficient (see [13] for details). As a function of the invariant mass of the photon

(24)

Again, the effect seems to depend crucially on the ratio of two very small numbers: and .

Acknowledgments

It is a pleasure to thank the organizers of Patras 2013 for an enjoyable conference and encouragement. We acknowledge financial support from projects FPA2010-20807, 2009SGR502 and Consolider CPAN.

References

  1. L.Abbott and P. Sikivie, Phys. Lett. 120B, 133 (1983).
  2. M. Kuster, G. Raffelt and B. Beltran (eds), Lecture Notes in Physics 741 (2008).
  3. R.D. Peccei, H.R. Quinn, Phys. Rev. Lett. 38 (1977) 1440; S. Weinberg, Phys. Rev. Lett. 40 (1978) 223; F. Wilzcek, Phys. Rev. Lett. 40 (1978) 279.
  4. M. Dine, W. Fischler and M. Srednicki, Phys. Lett. B, 104, 199 (1981); A.R. Zhitnitsky, Sov. J. Nucl. Phys. 31, 260 (1980); J. E. Kim, Phys. Rev. Lett. 43, 103 (1979); M. A. Shifman, A. I. Vainshtein and V. I. Zakharov, Nucl. Phys. B 166, 493 (1980).
  5. A.H. Corsico et al, JCAP 1212 (2012) 010.
  6. D. Espriu and A. Renau, in Proceedings, 7th Patras Workshop, PATRAS 2011, Mykonos, Greece [arXiv:1111.3141].
  7. A. Andrianov, D. Espriu, F. Mescia and A. Renau, Phys. Lett. B 684 (2010) 101; D. Espriu, F. Mescia, A. Renau, JCAP 1108 (2011) 002.
  8. G. Raffelt and L. Stodolsky, Phys. Rev. D 37, 1237 (1988).
  9. D. Espriu and A. Renau, Phys. Rev. D85 (2012) 025010.
  10. A.A. Andrianov, D. Espriu, P. Giacconi and R. Soldati, JHEP 0909:057,2009.
  11. S. Herrmann et al., Phys. Rev. D 80 (100): 105011.
  12. D. Espriu and A. Renau, in preparation.
  13. A. Andrianov, S. Kolevatov, Theor.Math.Phys. 175 (2013) 744.
137254
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
Edit
-  
Unpublish
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel
Comments 0
Request comment
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description