Multiple Lorentz groups — a toy model for superluminal muon neutrinos

Multiple Lorentz groups - a toy model for superluminal muon neutrinos

Abstract

In this article an idea is presented, which allows for the explanation of superluminal muon neutrinos. It is based on the introduction of a new superluminal, massless gauge boson coupling to the neutrino only, but not to other standard model particles.

The model is discussed with regard to the Supernova 1987 (SN 1987) velocity bound on electron antineutrinos and the Cohen–Glashow constraint on superluminal neutrino propagation. The latter can be circumvented if — within the framework of the model — a sterile neutrino mixing with the active neutrino mass eigenstates is introduced. The suggestion of a sterile neutrino accounting for superluminal neutrinos has already been proposed in several papers.

It is possible to choose mixing angles with the sterile neutrino sector such that the model respects both the SN 1987 bound and the muon neutrino travels superluminally.

Special relativity; Dispersion relations; Neutrino interactions; Non-standard-model neutrinos.
pacs:
03.30.+p, 11.55.Fv, 13.15.+g, 14.60.St

I Introduction

At the end of September 2011, the OPERA collaboration announced the remarkable detection of superluminal muon neutrinos at the -level OPERA:2011zb (). Their experimental result with statistical and systematical error was given by:1

(1.1)

Unfortunately, on February, 2012 two error sources had become evident, which were likely to ruin their result. First, a fiber connection to a computer card had not been attached properly. Second, there had been a problem with the clock at OPERA used between the synchronizations with the Global Positioning System.

At the 25th International Conference on Neutrino Physics and Astrophysics in Kyoto on June 8th, 2012 a final update on the OPERA time-of-flight measurement was given:

(1.2)

This number states the deviation of the muon neutrino time-of-flight from the time that light needs to travel the distance from CERN to the Gran Sasso underground laboratory. Hence, the deviation is now consistent with zero.

The physics community had considered the result given by Eq. (1.1) with care, since the deviation from the speed of light lay several orders of magnitude above what would be expected, if it was from quantum gravitational origin. The authors of Contaldi:2011 (); Besida:2011fi (); vanElburg:2011ze (); Alicki:2011qw (); Henri:2011wu (); Broda:2011du () tried to figure out how the OPERA result could be explained by possible systematical errors. Beyond that, in Davoudiasl:2011gb () a cross-check for the result was proposed. It was demonstrated that muon neutrinos traveling with superluminal velocity can produce signatures for highly-boosted -quark pairs at the LHC, where one or both quarks decay semileptonically.

Furthermore, on the one hand, Cohen and Glashow showed that a superluminal neutrino would lose its energy quickly by the emission of electron positron pairs Cohen:2011hx (). If muon neutrinos moved faster than light, the process would be energetically possible above a certain neutrino energy threshold resulting in a copious production of electron positron pairs. On the other hand, the authors of Mohanty:2011 (); Lingli:2011kh () discussed that the Cohen–Glashow constraint can be avoided. This may be the case when, for example, Lorentz-violating effects depend quadratically on the neutrino energy or if Lorentz-violation is not fixed but covariant with the neutrino four-momentum.

In arXiv:1111.4994 () two models were investigated, where the first gave rise to deformed energy conservation laws and the second resulted in deformed momentum conservation laws. For these models the bounds of Cohen:2011hx () are not applicable.

In the article Bi:2011nd () further constraints on the deviation of the neutrino velocity from the speed of light were given by considering pion decay and TeV-neutrinos detected by ICECUBE. These gave severe bounds on Lorentz symmetry violation in the neutrino sector clashing with the experimental OPERA result.

Although the OPERA result has now proven to be wrong, it stimulated theoretical ideas in this field and led to many new models, which can perhaps be applied to other realms of physics. It may also be the case that a certain neutrino species indeed travels superluminally. However, the deviation from the speed of light is then expected to be much smaller than the value measured by OPERA. For this reason some representative examples for models that try to describe superluminal neutrinos will be listed:

  • It is well-known that dispersion relations of particles will be modified, if they propagate through a medium. In Cacciapaglia:2011ax (); AmelinoCamelia:2011dx () the superluminal motion of muon neutrinos is interpreted in the framework of deformed dispersion relations, which are a low-energy manifestation of Lorentz-violating physics at the Planck scale. In these theories the vacuum behaves as an effective medium.

    Such a medium can result from standard model physics, as well. For example, in Nakanishi:2011vv () superluminal neutrinos are explained by the assumption that Earth is surrounded by a special kind of matter consisting of separated quarks. If the wave functions of quarks are entangled, they can form colorless objects and, hence, are confined, even when they are spatially separated by a large distance.

  • In Nojiri:2011ju () a model is proposed which describes a spontaneous breakdown of Lorentz symmetry by a scalar background field that is added to the action via a Lagrange multiplier. This framework leads to a modified neutrino dispersion relation depending on the momentum of the neutrino.

  • The neutrino velocity can be modified by Fermi point splitting (for a recent review see arXiv:1111.4627 ()), which removes the degeneracy of zeros of the fermionic energy spectrum Klinkhamer:2011mf ().

  • The neutrino dispersion relation can change because of environmental effects caused by fields that accumulate at the position of the Earth. These may lead to an effective metric, in which the neutrino propagates with superluminal velocity Dvali:2011mn (); Oda:2011kh ().2 Furthermore, in the context of general relativity, a particle traveling along a geodesic path in a metric different from the Minkowski metric can be investigated Alles:2011wq (). In the article previously mentioned the mean velocity of such a particle is calculated with the assumption that the observer stays at rest. The average velocity can be larger than the speed of light, even if the velocity as a local property defined in a spacetime point is smaller. This is investigated for a Schwarzschild metric.

  • A further alternative is to consider models of modified gravity. In the article Saridakis:2011eq () particle propagation in a Hořava-Lifshitz modified gravitational background is considered. The authors derive the Dirac equation for a fermion traveling through such a background. The condition for the existence of nontrivial solutions of the Dirac equation leads to a modified neutrino dispersion relation. The neutrino velocity can be larger than the speed of light for a special Hořava-Lifshitz scenario.

  • In Klinkhamer:2011pw () the existence of a sterile neutrino that travels with a superluminal velocity is proposed. Sterile neutrinos cleverly get around the Cohen–Glashow bound, since they do not couple to the Z boson. An analysis involving sterile superluminal neutrinos is presented e.g. in Winter:2011zf ().

Furthermore, assuming superluminal neutrino propagation at a certain energy, neutrinos may propagate with a velocity at very high energies leading to a different neutrino horizon. In Lacki:2011wv () bounds from astrophysical observations are set on for very high neutrino energies.

Ii Extension of the Lorentz group — neutrinos and a hidden sector

Let us, for now, take Eq. (1.1) as it stands, since the idea of superluminal muon neutrinos proposed in the current article is purely theoretical and does not rely on the OPERA result. The goal is to describe a superluminal neutrino species without quantum gravity effects, but by the introduction of new particles coupling to neutrinos. For the analysis presented as follows the OPERA value can be chosen just as an example (independently of its correctness) in order to demonstrate the model proposed. That is why we will often refer to Eq. (1.1) in the rest of the paper.

ii.1 Invariant and maximum velocity

The foundations of special relativity are the relativity principle and the constancy (invariance) of the speed of light. As a result, the Galilei group of classical mechanics is replaced by the Lorentz group, which leads, for example, to the relativistic law of addition of velocities. The fact that the speed of light is the maximum attainable velocity of all particles does not directly follow from the Lorentz group, since it only delivers an invariant velocity at first. In order to understand this, three Gedankenexperiments will be performed, whose concept was initiated in Liberati:2001sd ().

Figure 1: Hidden sector that decouples from all the standard model particles except the neutrino. The neutrino is assumed to carry a charge, which massless hidden sector gauge bosons couple to. These move with a velocity that is larger than the speed of light .
  • We consider some hypothetical beings living in a fluid. They are assumed to consist of fluid atoms, which are held together solely by phonon-mediated forces. The beings do not feel other forces such as electromagnetism or gravitation. Their dynamics is expected to be governed by an acoustic Lorentz group with the invariant velocity being the velocity of sound in the fluid Liberati:2001sd (). We expect the beings to build a rocket, which can be accelerated by phonon emission. From the relativistic addition of velocities it follows that the maximum attainable velocity of the rocket is given by .

  • Einstein found that the dynamics of particles in our universe is governed by the “standard” Lorentz group with the invariant speed of light . His theory has been heralded or substantiated by various experiments MichelsonMorley:1887 (); Kennedy:1932 (); Ives:1938 (). In the second Gedankenexperiment humans build a rocket which is accelerated by a light engine, namely the emission of photons. In this case, the relativistic addition of velocities leads to as the upper limit of the rocket velocity.

  • Now we are ready to discuss the central idea of this article. The basic assumption is that the photon is not the gauge boson which moves with the highest velocity. We adopt neutrinos carrying a new charge differing from all charges of the standard model. This charge is to be mediated by a postulated massless gauge boson moving with a speed . Neutrinos couple to these gauge bosons, which form — possibly together with other unknown particles — a hidden sector. The latter does not interact with any other particle of the standard model, cf. Fig. 1. This leads to a neutrino dynamics which is based on a “hidden sector Lorentz group” with an invariant velocity . The third Gedankenexperiment is to build a rocket consisting of neutrinos with an acceleration process working by the emission of gauge bosons . The limiting velocity of the rocket is then given by , which is larger than the speed of light.

Figure 2: Illustration of the situation presented in the previous three Gedankenexperiments. The horizonal axis shows different sectors, each containing a massless boson which transforms under the Lorentz group with a special invariant velocity. The velocity of this boson sets the maximum attainable velocity for all particles coupling to the corresponding sector. In the first sector the maximum velocity is given by the speed of sound of phonons. Note that the phonon takes a special role here, since it is not a gauge boson. However, for the very general argument this is not of importance. In the second sector the photon sets the upper limit, which manifests itself as the speed of light , whereas for the hidden sector it is the velocity of the gauge boson . There is the possibility of further sectors whose invariant velocity may also be smaller than . If in the latter case a standard model particle couples to such a sector, its kinematics will still be governed by a Lorentz group with the invariant velocity .

The consequences from this deliberation is that different levels of the Lorentz group each with a distinct invariant velocity can be realized in nature. The coupling constant is assumed to be small enough such that neutrino propagation is not affected too much to violate existing bounds on the interaction of neutrinos with matter. The size of the coupling is not important for now — only its existence. The situation described is depicted in Fig. 2. Each new coupling of particles to massless gauge bosons3 opens a new sector with a maximum attainable velocity for these particles from left to right.

ii.2 Modified neutrino kinematics and Lagrangian of the hidden sector

The gauge boson is assumed to couple to neutrino mass eigenstates. This seems a more natural choice than the coupling to flavor eigenstates, since the hidden sector does not know anything about neutrino flavors. Hence, the neutrino mass eigenstates () obey a kinematics resting upon special relativity, but with the speed of light replaced by the speed of the hidden sector gauge boson :

(2.3)

Here is the relativistic neutrino energy of the -th mass eigenstate, the neutrino momentum, and its mass.4 The modified neutrino dispersion relation in Eq. (II.2) is isotropic and gives the deformation. If we suppress the mass eigenstate index for a moment and interpret neutrinos as matter waves with frequency and three-momentum , we have to carry out the replacements and , which leads to:

(2.4)

The front velocity, which corresponds to the velocity of the highest frequency forerunners of a wave, is then given by Brillouin1960 ():

(2.5)

It equals the signal velocity of a -function shaped pulse in configuration space. Hence, any possible distortion of a signal does not play a role for the front velocity. The case is related to superluminal, to luminal, and to subluminal motion.

If the gauge boson is assumed to have spin 1 analogously to the photon, at the level of Lagrange densities the ordinary minimal coupling procedure can be performed with again replaced by :

(2.6a)
(2.6b)
(2.6c)
(2.6d)
(2.6e)
(2.6f)
(2.6g)

where are the neutrino spinor fields describing a specific mass eigenstate and are the standard Dirac matrices. The covariant derivative contains the vector field of the gauge boson and the charge , to which couples. Both a Dirac mass term and two possible choices for Majorana mass terms ChengLi:1984 () with Dirac mass and Majorana masses , are given.5 Here, is a left-handed, a right-handed neutrino spinor, and in Eq. (2.6g) denotes the charge conjugation operator.

Note that there is a in the zeroth component of the partial derivative . In the context of the Lorentz-violating Standard Model Extension Colladay:1998fq () the nonzero Lorentz-violating coefficients can be found in the left-handed neutrino sector of in their Eq. (9).6 If we write this term in the mass eigenstate basis and denote the corresponding coefficients by , the -matrix is both diagonal in the eigenstate coefficients , and diagonal in the Lorentz indices. The latter holds, since the model is isotropic. This leads to

(2.7)

The coefficient matrix is both symmetric and traceless:

(2.8)

This resembles the CPT-even nonbirefringent modified Maxwell theory coefficients in the photon sector BaileyKostelecky2004 (); Altschul:2006zz (), which is clear, since both sectors are related by a coordinate transformation — at least at first order in the Lorentz-violating coefficients Altschul:2006zz ().

ii.3 Extension of the toy model to three neutrino flavors

The neutrino masses are eigenvalues to the mass eigenstates . However, the weak interaction gauge bosons couple to flavor eigenstates with . The transformation from mass to flavor eigenstates and (vice versa) is governed by the unitary -PNMS matrix :

(2.9a)
When, for simplicity, the CP-violating phases are set to zero,7 the matrix reads
(2.9b)

where, for brevity, and have been used Nakamura:2010zzi (). Here, for are the neutrino mixing angles. Kinematik measurements of neutrino masses (e.g. for pion decay and beta decay8) lead to “masses of neutrino flavors,” which are the weighted average of the neutrino mass eigenvalues arXiv:0909.2104 ():

(2.10a)
(2.10b)
(2.10c)

Since in Eq. (II.2) the neutrino mass eigenvalues are multiplied by , the maximum velocity of each neutrino flavor will be defined in the following way:

(2.11a)
(2.11b)
(2.11c)

If we assume

(2.12a)
(2.12b)

it is sufficient to linearize the equations above:

(2.13)

Here, . From the latter equation follows the simplified result

(2.14a)
(2.14b)

In the rest of the article the neutrino velocities will be approximated by for the mass eigenstates and by for the flavor eigenstates, since neutrino masses are assumed to be much smaller than neutrino energies.

The Supernova 1987 bound

The point of extending the toy model to all active neutrino flavors, is to account for the Supernova 1987 (SN 1987) bound on electron antineutrinos9 Hirata:1987hu (); Longo:1987ub ():

(2.15)

An electron neutrino produced by a weak interaction process is a mixture of neutrino mass eigenstates according to the relation

(2.16)

After the neutrino has traveled through space and reaches a distance from the origin of its production it holds

(2.17)

where has been assumed Nakamura:2010zzi (). Hence, the initial electron neutrino state then corresponds to a mixture of all flavor eigenstates. However, the initial composition of mass eigenstates remains the same, because quantum mechanically the statement

(2.18)

is valid. As a result of that, also the velocity of the neutrino does not change during its propagation, since it is determined by the initial composition of mass eigenstates. The antineutrinos coming from the supernova were detected as electron antineutrinos on Earth. For this reason the bound of Eq. (2.15) will be considered as a bound on the velocity of electron neutrinos — regardless of whether their flavor was different on their way to Earth.

We assume three distinct hidden sectors each with its own gauge boson , where only couples to the first mass eigenstate, to the second, and to the third, via the respective charge for , 2, and 3, respectively. If any sector obeys a different invariant velocity , the constraint of Eq. (2.15) does not necessarily contradict a deviation from the speed of light of the order of for one single neutrino flavor. This will be shown as follows.

The current experimental values or bounds for the three neutrino mixing angles , , and are Nakamura:2010zzi ():

(2.19a)
(2.19b)
(2.19c)

With the lower bound on and the upper bound on we obtain the PNMS matrix

(2.20)

Current experimental data imply that neutrinos are almost massless. Concretely, this means from neutrino oscillation data Nakamura:2010zzi () and10

(2.21)

which is obtained from WMAP observations Komatsu:2008hk (). Therefore, an approximate value of directly follows from Eq. (1.1):

(2.22)

Assuming and we obtain:11

(2.23)

Hence, Eq. (1.1) for muon neutrinos and the SN 1987 bound for electron neutrinos do not clash, if the velocity of the first mass eigenstate is a little bit lower than and if the second moves faster than . Since the first eigenstate propagates slower than , it need not necessarily couple to any hidden sector. In contrast, the second mass eigenstate has to couple to a traveling faster than light.

ii.4 Challenges of the model and introduction of sterile neutrinos

The argument of Cohen:2011hx () resulting in the rapid loss of the neutrino energy by electron positron emission relies on fundamental principles: four-momentum conservation and the coupling of the neutrino sector to the Z boson. Models for superluminal neutrino propagation have to compete with the very general result mentioned, and this is also the case for the toy model presented here.

  • We could assume the energy loss of muon neutrinos to be compensated by a Compton scattering type process, where gauge bosons scatter with muon neutrinos. However, this argument leads to additional problems. First of all, the free parameters of the model (e.g. the charge or the initial energy of a boson) have to be chosen such that this compensation is possible, which requires extreme finetuning. If the momentum distribution of is homogeneous and isotropic, the average energy transfer to the neutrino will be zero. In principle, the distribution may be anisotropic, but then neutrinos might be deflected on their way from CERN to the Gran Sasso underground laboratory.

  • An alternative proposal is that a neutrino itself is part of the hidden sector making it to some kind of superluminal, sterile neutrino . Then the neutrino does not couple to the Z boson, rendering the process forbidden. The sterile neutrino may mix with the active neutrino species leading to superluminal propagation of at least some of the standard model neutrino flavors. This idea has already been suggested in other publications, see e.g. Klinkhamer:2011pw (); Klinkhamer:2011js () and references therein. Reference Marfatia:2011bw () states that sterile neutrino models may be in conflict with the atmospheric neutrino data measured at Super-Kamiokande. However, the models considered in the latter article only involve one sterile neutrino and one single mixing angle with this neutrino. Conclusions for models with more mixing angles have not been obtained.

(a)    
(b)    
(c)    
Figure 3: Each panel shows the plane of a different pair of sterile neutrino mixing angles, where the remaining angle is set to the special value given below the corresponding panel. Regions of the electron and the muon neutrino velocity are shown, where , and is the common choice. The blue areas depict the region and the green areas show the region . The condition is fulfilled for all possible mixing angles in each panel, so is .

According to the second item of the list above, we extend the toy model by sterile neutrino mass eigenstates. Then the transformation between the flavor and mass eigenstates is governed by a unitary -matrix :

(2.24)

Following Eq. (2.14) we can write:

(2.25)

For our toy model we consider the simplest case with one single sterile neutrino, hence . In principle, this sterile neutrino mass eigenstate mixes with the active neutrino mass eigenstates for . This mixing can be described by introducing three additional mixing angles , , and . The corresponding -mixing matrix can then be constructed from as follows:12

(2.26)

where . In what follows, we examine a subspace of the free toy model parameters, which is seven-dimensional. It is spanned by the three sterile neutrino mixing angles , , and by the invariant velocities of the neutrino mass eigenstates , , , . Since this phase space is that large, it will be reduced by the special choice below. We assume that the invariant velocities of the three standard neutrino mass eigenstates correspond to the speed of light, which means . The single sterile neutrino is assumed to travel with superluminal speed: we therefore set .

As a result, only the sterile mixing angles remain as free parameters. In Fig. 3 three cases are considered, where in each one of these angles is fixed: , , and . We would like to explore, whether in each case the remaining two angles can be chosen such that the electron anti-neutrino velocity respects the SN 1987 bound of Eq. (2.15) and that the muon neutrino velocity lies in the error band of Eq. (1.1). In all plots overlapping regions are small, but they exist. At least one of the three mixing angles has to be rather large. A special possibility is , , and that becomes evident from the third panel. With these values we obtain the following results for the velocities of the three active neutrino flavors:

(2.27a)
(2.27b)
(2.27c)

Whether there exists a choice of angles that does not contradict existing atmospheric neutrino data — as was proposed in Marfatia:2011bw () — will not be examined here.

To summarize, within the toy model presented a superluminal sterile neutrino mass eigenstate can be introduced, such that the electron neutrino respects the SN 1987 bound and the muon neutrino travels with the superluminal velocity that is given by Eq. (1.1). For the parameters chosen above the tau neutrino is then slightly superluminal, as well.

Iii Conclusions

In this article a concept accounting for superluminal muon neutrinos was presented. It is based on a multiple Lorentz group structure. The dynamics of the neutrino is assumed to obey the Lorentz group with an invariant velocity that is larger than the speed of light. This will be possible, if the neutrino couples to a hidden sector of massless gauge bosons that move faster than photons. Then the neutrino field transforms under the Lorentz group with an invariant velocity which corresponds to the velocity of these gauge bosons.

If an experiment measures a deviation of the neutrino velocity that is much larger than the speed of light, this will be very difficult to understand in the context of physics at the Planck scale. The idea presented here leads, in principle, to a modified dispersion relation of the neutrino, as well. However, the framework is not quantum gravity, but special relativity and field theory with an invariant velocity imposed that differs from the speed of light.

First of all, every physical model describing superluminal muon neutrinos has to compete with the SN 1987 bound. This is a minor difficulty, since the toy model presented here can be altered such that electron neutrinos behave differently compared to muon neutrinos. More severe is the Cohen–Glashow constraint that is based on fundamental principles of present-day physics, which are difficult to circumvent. Honestly, the latter is also a severe problem for the current model, unless the superluminal neutrino itself is part of a hidden sector, hence sterile.

Besides that, the toy model makes the following predictions that can be verified or falsified by experiment:

  • If the muon neutrino moves with a superluminal velocity, its velocity is isotropic and does not depend on the neutrino energy (besides any mass-related dependence).

  • It is not a local effect, i.e. muon neutrinos move with a superluminal velocity in interstellar space, as well.

To find a physical theory both explaining superluminal neutrinos without bothering already established data and facts about the neutrino sector is a great challenge for model builders.

Acknowledgments

It is a pleasure to thank S. Thambyahpillai (KIT) and A. Crivellin (University of Bern) for reading an early draft of the paper and for useful suggestions. Furthermore, the author thanks V. A. Kostelecký (Indiana University, Bloomington) for helpful discussions.

The author acknowledges support by Deutsche Forschungsgemeinschaft and Open Access Publishing Fund of Karlsruhe Institute of Technology.

Footnotes

  1. These numbers can be found in the updated version 2.0 of OPERA:2011zb ().
  2. Reference Iorio:2011ay () gives new experimental bounds on the mass scale that is characteristic for the model presented in Dvali:2011mn ().
  3. Remark that the phonon is not a gauge boson, but a Goldstone boson (massless excitation) resulting from the spontaneously broken translation symmetry in a solid. This does not matter for the argument, though.
  4. We assume that all mass eigenstates propagate with the same momentum . Whenever we refer to kinematics we stick to the notation of with an index (denoting the mass or flavor eigenstate) for the neutrino mass.
  5. The question, whether the neutrino is a Dirac or a Majorana particle, has not been answered so far.
  6. Alternatively, the effective Hamiltonian given by Eq. (14) in Kostelecky:2003cr () can be considered.
  7. Furthermore, currently no experimental data concerning these phases are on hand Nakamura:2010zzi ().
  8. Neutrinoless double beta decay that occurs for Majorana neutrinos leads to a different definition of the “flavor eigenstate mass” arXiv:0909.2104 ().
  9. An antineutrino is assumed to travel with the same velocity as the corresponding neutrino. This makes sense, since the model presented corresponds to a CPT-even term of the Lorentz-violating Standard Model Extension. See the end of Sec. II.2 for a brief discussion concerning this issue.
  10. Note that under the assumptions taken, the unit should be replaced by , as well. But since the mass values given have been obtained in the context of special relativity, where the speed of light is the invariant velocity, we keep .
  11. The latter choice is reasonable, since according to Eqs. (1.1) and (2.15). We keep in mind that the constraints on and were obtained at different neutrino energies, but this does not play a role in our model, though.
  12. with all CP-violating phases set to zero

References

  1. T. Adam et al. [OPERA Collaboration], “Measurement of the neutrino velocity with the OPERA detector in the CNGS beam,” arXiv:1109.4897 [hep-ex].
  2. C. R. Contaldi, “The OPERA neutrino velocity result and the synchronisation of clocks,” arXiv:1109.6160 [hep-ph].
  3. O. Besida, “Three errors in the article: ’The OPERA neutrino velocity result and the synchronisation of clocks’,” arXiv:1110.2909 [hep-ph].
  4. R. A. J. van Elburg, “Measuring time of flight using satellite-based clocks,” arXiv:1110.2685 [physics.gen-ph].
  5. R. Alicki, “A possible statistical mechanism of anomalous neutrino velocity in OPERA experiment?,” arXiv:1109.5727 [physics.data-an].
  6. G. Henri, “A simple explanation of OPERA results without strange physics,” arXiv:1110.0239 [hep-ph].
  7. B. Broda, “An OPERA inspired classical model reproducing superluminal velocities,” arXiv:1110.0644 [physics.data-an].
  8. H. Davoudiasl and T. G. Rizzo, “Testing the OPERA superluminal neutrino anomaly at the LHC,” Physical Review D, Vol. 84, No. 9, 2011, Article ID 091903 (3 pages), arXiv:1110.0821 [hep-ph]. \doi10.1103/PhysRevD.84.091903
  9. A. G. Cohen and S. L. Glashow, “Pair creation constrains superluminal neutrino propagation,” Physical Review Letters, Vol. 107, No. 18, 2011, Article ID 181803 (3 pages), arXiv:1109.6562 [hep-ph]. \doi10.1103/PhysRevLett.107.181803
  10. S. Mohanty and S. Rao, “Constraint on super-luminal neutrinos from vacuum Cerenkov processes,” arXiv:1111.2725 [hep-ph].
  11. Z. Lingli and B.-Q. Ma, “On the rationality of the OPERA experiment as a signal of Lorentz violation,” arXiv:1111.1574 [hep-ph].
  12. Y. Huo, T. Li, Y. Liao, D. V. Nanopoulos, Y. Qi, and F. Wang, “The OPERA superluminal neutrinos from deformed Lorentz invariance,” arXiv:1111.4994 [hep-ph].
  13. X.-J. Bi, P.-F. Yin, Z.-H. Yu, and Q. Yuan, “Constraints and tests of the OPERA superluminal neutrinos,” Physical Review Letters, Vol. 107, No. 24, 2011, Article ID 241802 (5 pages), arXiv:1109.6667 [hep-ph]. \doi10.1103/PhysRevLett.107.241802
  14. G. Cacciapaglia, A. Deandrea, and L. Panizzi, “Superluminal neutrinos in long baseline experiments and SN1987a,” Journal of High Energy Physics, Vol. 2011, No. 11, 2011, Article ID 137 (24 pages), arXiv:1109.4980 [hep-ph]. \doi10.1007/JHEP11(2011)137
  15. G. Amelino-Camelia, G. Gubitosi, N. Loret, F. Mercati, G. Rosati, and P. Lipari, “OPERA-reassessing data on the energy dependence of the speed of neutrinos,” International Journal of Modern Physics D, Vol. 20, No. 14, 2011, pp. 2623 – 2640, arXiv:1109.5172 [hep-ph]. \doi10.1142/S0218271811020780
  16. N. Nakanishi, “An interpretation of ’superluminal neutrino’ compatible with relativity in the framework of standard model,” arXiv:1111.1760 [hep-ph].
  17. S. ’i. Nojiri and S. D. Odintsov, “Could the dynamical Lorentz symmetry breaking induce the superluminal neutrinos?,” The European Physical Journal C, Vol. 71, No. 11, 2011, Article ID 1801 (3 pages), arXiv:1110.0889 [hep-ph]. \doi10.1140/epjc/s10052-011-1801-4
  18. G. E. Volovik, “Topology of quantum vacuum,” arXiv:1111.4627 [hep-ph].
  19. F. R. Klinkhamer, “Superluminal muon-neutrino velocity from a Fermi-point-splitting model of Lorentz violation,” arXiv:1109.5671 [hep-ph].
  20. G. Dvali and A. Vikman, “Price for environmental neutrino-superluminality,” Journal of High Energy Physics, Vol. 2012, No. 2, 2012, Article ID 134 (8 pages), arXiv:1109.5685 [hep-ph]. \doi10.1007/JHEP02(2012)134
  21. I. Oda and H. Taira, “Superluminal neutrinos from gauge field,” Modern Physics Letters A, Vol. 26, No. 39, 2011, pp. 2917 – 2921, arXiv:1110.0931 [hep-ph]. \doi10.1142/S0217732311037297
  22. L. Iorio, “Constraints from orbital motions around the Earth of the environmental fifth-force hypothesis for the OPERA superluminal neutrino phenomenology,” Journal of High Energy Physics, Vol. 2012, No. 5, 2012, Article ID 73 (16 pages), arXiv:1109.6249 [gr-qc]. \doi10.1007/JHEP05(2012)073
  23. B. Allés, “Relativity accommodates superluminal mean velocities,” Physical Review D, Vol. 85, No. 4, 2012, Article ID 047501 (5 pages), arXiv:1111.0805 [hep-ph]. \doi10.1103/PhysRevD.85.047501
  24. E. N. Saridakis, “Superluminal neutrinos in Hořava-Lifshitz gravity,” arXiv:1110.0697 [gr-qc].
  25. F. R. Klinkhamer, “Spontaneously broken Lorentz invariance from the dynamics of a heavy sterile neutrino,” Letters to Journal of Experimental and Theoretical Physics, Vol. 95, No. 10, 2012, pp. 497 – 500, arXiv:1111.4931 [hep-ph]. \doi10.1134/S0021364012100062
  26. W. Winter, “Constraints on the interpretation of the superluminal motion of neutrinos at OPERA,” Physical Review D, Vol. 85, No. 1, 2012, Article ID 017301 (5 pages), arXiv:1110.0424 [hep-ph]. \doi10.1103/PhysRevD.85.017301
  27. B. C. Lacki, “Olber’s paradox for superluminal neutrinos: Constraining extreme neutrino speeds at TeV – ZeV energies with the diffuse neutrino background,” Journal of Cosmology and Astroparticle Physics, Vol. 2012, No. 1, 2012, Article ID 054 (14 pages), arXiv:1111.3045 [hep-ph]. \doi10.1088/1475-7516/2012/01/054
  28. S. Liberati, S. Sonego, and M. Visser, “Faster-than- signals, special relativity, and causality,” Annals of Physics, Vol. 298, No. 1, 2002, pp. 167 – 184, arXiv:gr-qc/0107091. \doi10.1006/aphy.2002.6233
  29. A. A. Michelson and E. W. Morley “On the relative motion of the Earth and the luminiferous ether,” American Journal of Science, Vol. 34, No. 203, 1887, pp. 333 – 345.
  30. R. J. Kennedy and E. M. Thorndike, “Experimental establishment of the relativity of time,” Physical Review, Vol. 42, No. 3, 1932, pp. 400 – 418. \doi10.1103/PhysRev.42.400
  31. H. E. Ives and G. R. Stilwell, “An experimental study of the rate of a moving atomic clock,” Journal of the Optical Society of America, Vol. 28, No. 7, 1938, pp. 215 – 219. \doi10.1364/JOSA.28.000215
  32. L. Brillouin, “Wave propagation and group velocity,” Academic, New York, USA, 1960.
  33. T. Cheng and L. Li, “Gauge theory of elementary particle physics,” Clarendon Press, Oxford, 1984.
  34. D. Colladay and V. A. Kostelecký, “Lorentz-violating extension of the standard model,” Physical Review D, Vol. 58, No. 11, 1998, Article ID 116002 (23 pages), arXiv:hep-ph/9809521. \doi10.1103/PhysRevD.58.116002
  35. V. A. Kostelecký and M. Mewes, “Lorentz and CPT violation in neutrinos,” Physical Review D, Vol. 69, No. 1, 2004, Article ID 016005 (25 pages), arXiv:hep-ph/0309025. \doi10.1103/PhysRevD.69.016005
  36. Q. G. Bailey and V. A. Kostelecký, “Lorentz-violating electrostatics and magnetostatics,” Physical Review D, Vol. 70, No. 7, 2004, Article ID 076006 (10 pages), arXiv:hep-ph/0407252. \doi10.1103/PhysRevD.70.076006
  37. B. Altschul, “Vacuum Cerenkov radiation in Lorentz-violating theories without CPT violation,” Physical Review Letters, Vol. 98, No. 4, 2007, Article ID 041603 (4 pages), arXiv:hep-th/0609030. \doi10.1103/PhysRevLett.98.041603
  38. K. Nakamura et al. [Particle Data Group Collaboration], “The review of particle physics,” Journal of Physics G, Vol. 37, No. 7A, 2010, Article ID 075021, available at http://pdg.lbl.gov. \doi10.1088/0954-3899/37/7A/075021
  39. E. W. Otten and C. Weinheimer, “Neutrino mass limit from tritium beta decay,” Reports on Progress in Physics, Vol. 71, No. 8, 2008, Article ID 086201 (36 pages), arXiv:0909.2104 [hep-ex]. \doi10.1088/0034-4885/71/8/086201
  40. K. Hirata et al. [KAMIOKANDE-II Collaboration], “Observation of a neutrino burst from the supernova SN 1987a,” Physical Review Letters, Vol. 58, No. 14, 1987, pp. 1490 – 1493. \doi10.1103/PhysRevLett.58.1490
  41. M. J. Longo, “Tests of relativity from SN 1987a,” Physical Review D, Vol. 36, No. 10, 1987, pp. 3276 – 3277. \doi10.1103/PhysRevD.36.3276
  42. E. Komatsu et al. [WMAP Collaboration],
    “Five-year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Cosmological interpretation,” The Astrophysical Journal Supplement Series, Vol. 180, No. 2, 2009, pp. 330 – 376, arXiv:0803.0547 [astro-ph]. \doi10.1088/0067-0049/180/2/330
  43. F. R. Klinkhamer, “Superluminal neutrino, flavor, and relativity,” Physical Review D, Vol. 85, No. 1, 2012, Article ID 016011 (4 pages), arXiv:1110.2146 [hep-ph]. \doi10.1103/PhysRevD.85.016011
  44. D. Marfatia, H. Päs, S. Pakvasa, and T. J. Weiler, “A model of superluminal neutrinos,” Physics Letters B, Vol. 707, No. 5, 2012, pp. 553 – 557, arXiv:1112.0527 [hep-ph]. \doi10.1016/j.physletb.2012.01.028
Comments 0
Request Comment
You are adding the first comment!
How to quickly get a good reply:
  • Give credit where it’s due by listing out the positive aspects of a paper before getting into which changes should be made.
  • Be specific in your critique, and provide supporting evidence with appropriate references to substantiate general statements.
  • Your comment should inspire ideas to flow and help the author improves the paper.

The better we are at sharing our knowledge with each other, the faster we move forward.
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...
302645
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel

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