Neutrino Dispersion Relations from a Dark Energy Model

We consider a model in which the neutrino is kinetically coupled to a scalar field and study its implications for environmentally dependent neutrino velocities. Following the usual effective field theory logic, this coupling is expected to arise in neutrino dark energy models. It leads to a Lorentz violation in the neutrino sector. The coupling of the scalar field to the stress tensor of the Earth yields terrestrial neutrino dispersion relations distinct from those in interstellar space.


Introduction
Last year the OPERA experiment announced the arrival of 16,111 Swiss neutrinos, 61 nanoseconds ahead of schedule [1]. It turns out that this announcement was incorrect [2,3] and in the past year nearly all of the long baseline neutrino experiments [4][5][6][7][8] including OPERA itself [1] have con�rmed that neutrinos travel at the speed of light to within experimental errors. But just as the velocity anomaly has disappeared, other anomalies and inconsistencies in the standard model with two or three mass neutrinos have been reinforced.
e velocity anomaly at OPERA immediately was observed to be in contradiction with the measurement of the velocities of the neutrinos from SN1987A [9,10]. ere were attempts to evade this inconsistency with arti�cial models of energy dependences [11] but these were found to be in contradiction with simple kinematic arguments [12,13]. e only models which could not be falsi�ed on theoretical grounds alone were those which radially changed the nature of spacetime [14,15] and those which introduced an environmental dependence in the neutrino mass [16], although the later was found to be inconsistent with ��h force constraints [17], which was remedied in [18,19]. In fact environmentally dependent neutrino models have been used to explain anomalies while avoiding various constraints for almost a decade [20,21].
Similarly there appears to be room to resolve today's anomalies using environmental dependence. For example, the LSND experiment [22] and MiniBooNE [23-25, 25, 26] now both report an anomalous electron (anti)neutrino surplus which excludes the standard 3-neutrino oscillation paradigm at 3.8 . Nearly all of their parameter space is ruled out by the fact that no de�cit was observed at KARMEN [27] or ICARUS [28]. While the KARMEN and LSND experiments are nearly identical, the KARMEN baseline has a much lower average density than the LSND baseline. In addition, inside of a gallium detector both the GALLEX [29,30] and SAGE experiments [31][32][33][34] report a 2.5 de�cit of neutrinos from a radioactive source. In addition, tens of short baseline [35] and 1 km baseline [36] reactor antineutrino experiments have found about a 6% �ux de�cit. Finally, at even higher densities, the expected upturn in solar neutrinos at low density has not been observed and there may even be evidence for a downturn [37,38].
One explanation for these anomalies could be sterile neutrinos; however, combining ICARUS, KARMEN, LSND, and MiniBooNE constraints one �nds a sterile neutrino mass of about 0.5 eV [28] while the gallium anomaly requires a mass about 0.8 eV or else there would be no oscillation inside of the 2 meter detectors and the solar anomaly requires a mass of a millielectron volt or less. ree �avors of sterile neutrinos are strongly excluded by cosmological constraints. While constraints arising from primordial helium abundance in HII regions are fraught with systematic errors and controversy, the last years South Pole Telescope's measurement of the CMB diffusion radius [39] alone together with standard big bang nucleosynthesis and WMAP7's measurement of the sound horizon [40] provide a reasonably de�nitive exclusion of 3 sterile neutrino models. Within the next year the new South Pole Telescope and Planck data will provide the last word on the number of �avors of light particles which were once in thermal equilibrium with the primordial plasma, providing a �rm upper bound on the number of sterile neutrinos which are sufficiently strongly coupled to explain the anomalies listed in the previous paragraph.
Perhaps the correct explanation for these anomalies, like the neutrino velocity anomaly reported by OPERA, is experimental error. However, it is difficult to ignore the fact that they all occur in dense environments, such as the Earth, the iron shielding of LSND, gallium detectors, and even the core of the sun. e lowest density environment in which an anomaly has been reported is ice, where a horizontal neutrino excess has been reported by AMANDA and con�rmed by IceCube [41]. However, even in that case, this is a relative excess and could easily be instead a de�cit of neutrinos which pass through the Earth at steeper angles. e de�cit saturates around 10-15 degrees, corresponding to a maximum baseline in the Earth and so could, for example, result from oscillation to a sterile neutrino which may or may not be more massive inside of the Earth.
Summarizing, it remains a logical possibility that these anomalies are caused by some beyond the standard model matter effects. Aer all, neutrinos are the only particles which can travel more than 1 km through solid rock, and so they are the only particles which may be sensitive to such new physics.
is motivates a systematic study of effective �eld theories encoding potential environmental effects on neutrinos. While a large body of literature exists on beyond the standard model interactions of conventional matter on neutrinos, in the present work we will attempt a systematic study of a different class of models, which were �rst presented as explanations for the superluminality that had been claimed by OPERA. ese are models in which neutrinos interact not with the usual standard model particles, but with a dark coherent scalar �eld which is coupled gravitationally to other matter. Such a dark scalar, if it has a �xed pro�le and �lls a small portion of the universe, so that it does not increase in volume as it expands, will in recent times contribute to the density and pressure of the universe with a nonrelativistic equation of state and so will be a source of dark matter. If on the other hand it nearly homogeneously �lls most of the universe during some period, then it will contribute to the density and pressure with an equation of state and so contribute to the dark energy during that period. For simplicity and for a connection with the literature on this subject we will simply refer to the scalar �eld as the dark energy �eld, regardless of whether it ever had an equation of state close to 1. In this note we will not attempt to use these models to solve the anomalies described above.

Neutrino Coupling and Dispersion Relations
e models which we will consider invariably modify the neutrino dispersion relations. is change necessarily violates Lorentz symmetry. We will consider spontaneous violations of Lorentz symmetry, which arise by adding terms to the Lagrangian which couple a new �eld to neutrino bilinears. e couplings and the new �eld are similar to those introduced in the neutrino dark energy model of [20], and to a large extent to those in the earlier models of [42,43], although we do not demand that the additional �eld actually provides the observed dark energy. e �eld acquires a �E� due to interactions with the Earth, which spontaneously breaks the Lorentz symmetry. In [16,44,45] such models were constructed in which the new �elds introduced were, respectively, a symmetric tensor, a vector, and a scalar. We will consider a scalar �eld Π, which as explained below will have the advantage that it requires the tuning of only a single parameter. e fact that our couplings resemble those which arise in the neutrino dark energy scenario of [20] yields a cosmological justi�cation for the exclusiveness of these terms to the neutrino sector.
In an effective �eld theory setting, it is sufficient to consider the operators of lowest dimension which preserve Lorentz invariance. e terms with no derivatives can be absorbed into rede�nitions of the �elds and parameters of the effective theory. Strong upper bounds on these terms arise, for example, on masses from beta decay and as a result these terms will be negligible at OPERA energies.
As the standard model Higgs �eld has not yet been discovered. (A new boson has been discovered, but the 6 con�dence of the discovery arises from a 2 excess which is greater than that of the standard model Higgs and so cannot be considered to be evidence for the standard model Higgs. e standard model Higgs does not yet �t the data 5 better than the standard model with no Higgs, although it may before the scheduled shut down.) For the sake of generality we will not yet restrict our attention to a particular mechanism of SU(2) gauge symmetry breaking. We will write the effective theory directly in terms of the neutrino �elds, allowing the gauge symmetry to be realized either linearly or nonlinearly. Later, in (6) we will specialize to the standard GWS symmetry breaking and we will see that this choice changes the naive dimension of our new operator, as factors of the Higgs �eld need to be added. While the absolute dimension is indeed shied, the relative dimensions of the different possible operators are not altered and therefore our interaction continues to be the dominant relevant interaction in the infrared.
We will be interested only in terms which cannot be reabsorbed into other terms via �eld de�nitions up to terms without derivatives. In general the modi�cations of the dispersion relation can be linear or quadratic in the new couplings; we will eventually restrict our restriction to the linear modi�cations and so to the coupling terms which lead to linear modi�cations. With all of these criteria, we are le with where , , and are tensors constructed from derivatives of Π. In our dimensional analysis scheme, in which the coefficients are constructed from a scalar �eld of dimension [ , in the last term is of higher dimensionality and so need not be considered, but we will keep it during this section for illustration as a linear energy dependence of neutrino superluminality is excluded at OPERA by less than two sigmas. Clearly these derivative terms are nontrivial only if Π is not constant. e anomalies discussed above have been seen within the Earth and Sun, while SN1987A neutrinos tightly constrain the dispersion relation in space; therefore, these derivatives need to be localized on Earth. e simplest possibility would be ifΠ was localized on Earth and vanishes in space, while Π vanishes everywhere. However, it is easy to see that if Π begins with a constant value, the spatial gradients between here and SN1987A will dominate over the temporal gradient in less than a mere 160,000 years, much less than the age of the Earth. erefore such �eld con�gurations are not logically consistent. e next simplest possibility is thatΠ is negligible but the gradient of Π lies along the Earth's radial direction . In Section 3 we will describe a prototypical example of a scalar �eld with the desired behavior. For now, it will simply be relevant that the only nonzero derivatives, and so the only nonzero components of the tensors , , and , will be those with only indices or an even number of identical tangential indices. en the dispersion relation is with th spatial component where sums over repeated indices are understood. Notice that as in the model of [44] and unlike that of [16] the dispersion relation is anisotropic. In particular, the velocity of a neutrino is Let be the radial coordinate and choose direction to be orthogonal to such that the velocity of a given neutrino is in the plane, at an angle with respect to . Considering only the leading contributions to the Lorentz-violating terms, this neutrino will travel with a fractional superluminality equal to ≃ 2 2 cos 2 + cos 2 + sin 2 + 2 cos cos 2 + sin 2 .
We recall that, since the tensors , , and are proportional to the derivative of the scalar �eld Π, coefficients without an even number of identical tangential indices (such as and ) are zero.
As mentioned above in the sequel we will ignore the last term as it is created by a higher dimensional operator in our effective �eld theory description. Notice that and only occur in the combination + 2 /2 at this precision. e terms which we have omitted are strongly suppressed, by factors of the Lorentz-violating coefficients (which we assume to be at least of the same order of magnitude as the superluminality fraction) or even by the ratio of the neutrino rest mass to its energy, and so the identi�cation of further terms or even the separate identi�cation of and will need to await a much more precise or qualitatively different experimental setting. As we can then not hope to experimentally distinguish between the effects of and , we will simply neglect in what follows. Working with the effective lagrangian with a (2) × (1) symmetry, the second operator in (1) is given by where we have de�ned the constant : and the is the Higgs doublet of the standard model. In [45] the author considers a term which couples the neutrino kinetic tensor to Π Π. However, this term is of one energy dimension greater than (6) and so is suppressed according to the usual logic of effective �eld theories.

The Model
For concreteness we will consider models in which the neutrino propagator is modi�ed by a kinetic coupling of the neutrino to a �eld which obtains a �E�, if this messenger �eld is coupled to the Earth. In [46], for example, the authors proposed that this spatial dependence can emerge in type IIB string theory model.
No such coincidence is required in models in which the messenger is coupled directly to baryon density or to the background stress tensor in such a way that it acquires a classical expectation value concentrated near massive objects. So long as this classical �eld drops off sufficiently quickly from the sources, it will affect terrestrial neutrinos and not appreciably affect supernova neutrinos. However, it is important that the �eld drops off sufficiently quickly so that the Earth's effects dominate preferably over those of the Sun and certainly over those of the center of the Galaxy. In [16] this was achieved by adding spin two �elds whose inverse mass is �xed by hand to be roughly the inverse radius of the Earth (and necessarily less than the inverse distance to the Sun), while the coupling was chosen to yield the OPERA superluminality. In this paper we will present an alternative model in which the effects of the Sun and Galaxy are suppressed not by tuning another parameter, but simply by the derivative structure of our coupling to the neutrinos.
We consider a model with the neutrino dark energy term (6) coupling the neutrino to a scalar �eld with or without 4 ISRN High Energy Physics a minimal Galileon coupling [47] given by the boundary DGP model [48]: e coefficient , which can be taken to be zero, is a parameter of dimension [ 3 ] which parameterizes the nonlinear Galileon interaction. is the trace of the stress tensor of all of the matter, except for the scalar. e coupling of Π to the stress tensor could in principle lead to ��h forces beyond experimental bounds, as described in a very similar setting in [17], however, a quick calculation shows that only the product of the coefficient of this coupling and the coefficient in (6) appears in the neutrino − ; therefore any reduction of the coefficient of the stress tensor coupling which may be mandated by ��h force constraints can be compensated by an opposite rescaling of . While the Lagrangian itself has higher derivative terms, terms in the equations of motion have at most two derivatives acting on each Π, which allows the existence of ghost-free solutions such as that which we will use.
e Galileon interaction term is useful because it reduces short distance singularities, via the Vainshtein mechanism [49], at least in the presence of spherically symmetric stress tensor sources. More precisely, for an external source of mass there will be a distance scale [48]: at which the behavior of the Π �eld changes. We can choose the Galileon coupling such that this distance is either larger than or smaller than the radius of the Earth . For concreteness, in the rest of this paper, we will chose to be sufficiently small so that , and so we will set = in the rest of this section. A small value of is useful for, among other things, avoiding the potential formation of closed timelike curves [50]. However, will again become important for distance scales smaller than ; for example, it may be invoked for neutrino phenomenology in neutron stars and, depending on its value, in the cores of massive stars.
Let us now calculate a static, spherically symmetric �eld con�guration Π( ) in the presence of a nonrelativistic matter source with density ( ). e Π equation of motion is then is is easily integrated to yield where ( ) is the density contained in the object up to a radius , and we have �xed the constant of integration by imposing that Π is differentiable at the origin.
One can now easily �nd the second derivatives of Π, which appear in the coupling (6). Choosing our coordinates such that = = at a given point, while terms with mixed derivatives vanish. In particular, in the Earth's crust where and are, respectively, the average densities of the crust and of the Earth as a whole. More generally, (14) may be applied to a point at any radius in a background with an arbitrary spherically symmetric density pro�le if one identi�es with the density at radius and with the average density at radii less than . (6) modi�es the dispersion relation for the neutrinos, for example, allowing their velocity to deviate from the usual relativistic form. In the language of [16] this corresponds to a modi�cation of the effective metric in which the neutrinos propagate. e neutrino velocity at an angle with respect to the radial direction is given by inserting (7) into (5):

SN1987A. e equation
where ⟨ ⟩ is the Higgs VEV. In the case of even the longest baseline neutrino experiments to date, cos 2 ( ) 1 and so we will ignore the �rst term. �sing (14) one �nds where we have used 5 5 gm/cm 3 . For example, the OPERA result 3 1 −5 would be reproduced if is is much smaller than the energies of the OPERA neutrinos, which means that this effective �eld theory approach is invalid for deviations from relativistic dispersion relations as large as those reported by OPERA. e effective �eld theory approach can only be trusted below the cutoff energy. Of course, this �t is only reasonable if the main source of the dark energy �eld is the Earth. In other words, the main contribution to Π must arise from its coupling to the Earth, and not, for example, the Sun or the matter in our Galaxy. In the case of a distance object, the term in (13) vanishes, while the other terms are simply the ratio of the total mass to the distance cubed. erefore, at the surface of the Earth, the contribution of the Sun (with respect to that of the Earth) is suppressed by a factor of 10 −8 and that of the Galaxy by 10 −25 ; thus, it is reasonable to ignore these contributions. In the case of the model in [16] the corresponding dependence would lead to a dominant contribution from the Sun and Galaxy, and so these contributions are eliminated by hand by choosing the mass of their new �eld to be of order of the inverse radius of the Earth.
And so what about neutrinos from SN1987A? e fractional superluminality for these neutrinos needs to be less than 10 −9 . is is easily satis�ed, as one can see by directly calculating the change in arrival time, or else simply noting that nearly all of the trip is in interstellar space, where is of order 10 −30 . In fact, examining (13) more closely, one sees that during the �rst part of their trip the neutrinos are actually subluminal. e subliminality constraints on SN1987A neutrinos are very weak, as they depend upon assumptions about the propagation of light in the various media between here and the large Magellanic cloud.

KamLAND.
KamLAND lies between 55 nuclear reactors, which supply it with antineutrinos. e electron neutrinos oscillate into muon neutrinos. If the energy difference between an electron and muon neutrino is Δ , the probability that a given electron neutrino is still an electron neutrino aer traveling a distance is where is the mixing angle between these two �avors. Using the dispersion relation (2) one readily �nds, for an energy neutrino, that the latter phase is where 2 is the difference between the squared masses of the two relevant neutrino mass eigenstates and the and superscripts denote the Lorentz-violating neutrino couplings to the two �avors, respectively. is can be easily applied to models that had been proposed for the neutrino velocity anomaly. Inserting coef-�cients 2 + 2 which are su�ciently large to �t the �PERA data, together with an energy 5 MeV typical of reactor neutrinos seen above the background at KamLAND, one �nds that neutrinos oscillate about every 5 nanometers. is is much smaller than the resolution at KamLAND, and so KamLAND would in this case �nd an energy-independent survival probability. is is in grave contradiction with KamLAND's results in [51] which present two full averaged neutrino oscillations. Higher order terms, such as the term, lead to an even shorter wavelength but with an dependence which cannot cancel that of previous terms. erefore, a cancellation in such terms, in order to be consistent with KamLAND's results, must be imposed order by order in , and in fact also order in order in s( , which is small but still larger than the ratio of the energy to the neutrino mass. Such a cancellation is not possible with the terms in the lowest orders of the effective action considered in this note.

Solar Neutrinos and the MSW
Effect. �ur model modi�es the neutrino dispersion relations not only near the Earth, but near any massive body. In fact the effect is even more pronounced near the Sun, although unlike the model of [16] the modi�cation of the fractional neutrino velocity in the core of the Sun is still quite small. is modi�cation means that experimental signatures for our model may already be apparent in the solar neutrino data, and in particular solar neutrino data provides a nontrivial experimental check on the viability of our proposal. e velocity of solar neutrinos cannot be determined directly, as one does not know the time at which they were emitted. However, the interaction of neutrinos with the Sun leads to a further modi�cation of their dispersion relations which has an observed effect on neutrino oscillation, called the MSW effect [52][53][54]. is leads one to ask whether the modi�cation to the neutrino dispersion relation which we propose modi�es the experimental signatures of the MSW effect, in particular whether it modi�es the energy dependence of the electron neutrino survival probability.
In this subsection we will modify a textbook [55] derivation of the solar electron neutrino survival probability, applying the superluminal dispersion relation of our model. We will calculate the change in the survival probability for neutrinos of low enough energy such that their �avors are converted adiabatically, as is the case for observed solar neutrinos. While we will �nd that this effect is much too small to be observed for solar neutrinos, we will note that it is potentially large enough to be observed some day for supernova neutrinos.
e relevant electroweak interaction of neutrinos with leptons and baryons can be described by the Lagrangian density term of the form Δℒ 0 (20) If we consider only two �avors (as is reasonable for rough calculations involving solar neutrinos) we can express the interaction parameter as where and are the electron and neutron densities, respectively. We consider, for simplicity, neutrinos which travel radially outwards from the center of the Sun, in the direction which we will call . Recall from (14) that the main contribution to the superluminality fraction arises from where ⊙ x is value of the Lorentz-violating (LV) coefficient de�ned in (7) inside of the Sun. ⊙ ( and ⊙ 0 ( are the solar density at radius and the mean density at radius less than , respectively. e dependence will usually be le implicit.
In the case of the OPERA experiment, since the neutrino velocity is nearly perpendicular to the radial direction, the main contribution to the superluminality was proportional to the value of the LV coefficient inside of the Earth ⊕ = In the center of the Sun, ⊙ 0 (0 = ⊙ (0 , and hence ⊙ and ⊙ are equal: where ⊕ is the superluminality inside of the Earth's crust (for tangential motion), ⊙ is the density in the center of the Sun, and ⊕ 0 is the average density of the Earth. In order to calculate ⊙ 0 at a generic point, we need the approximate density pro�le of the solar core: On the boundary of solar core ( = 0.2 ⊙ ), is means that at the center of the Sun the neutrinos are superluminal but at higher radii they slow and by the boundary of the core they are subluminal. Crucially, at every radius the dimensionless LV parameter ⊙ is much smaller than one, and so we can use it to perturbatively expand all quantities of interest. Including the interaction term , in the ultrarelativistic limit our dispersion relation (2) becomes where we have de�ned the mass matrix e subscript LV indicates that the dispersion relation is Lorentz violating. e evolution of a neutrino planewave wavefunction in the electroweak interaction basis is given by multiplication by where we have de�ned the matrix , which can be evaluated using (26): e matrix has the same form as in the Lorentzinvariant (LI) case, but now LV ≃ (1+ ⊙ instead of ≃ . In our two-�avor approximation, the mixing angle and the difference between the two eigenvalues can be found diagonalizing matrix : where and = / is the electron fraction. e terms proportional to the identity matrix affect neither the difference Δ 2 between the eigenvalues of nor the rotation angle 2 which diagonalizes it Δ 2 | LV = Δ 2 cos (2 − LV 2 + s 2 (2 , Expanding in ⊙ , (32) yield where = (cos 2 − 2 + s 2 2 and is obtained from LV by replacing the Lorentz-violating dispersion relation with the usual one: Taking Δ 2 10 5 eV 2 , sin(2 ) 0. , using the typical values for the solar core ⊙ 80 g/cm 3 , 1, and | | 1 MeV, the fractional difference between the Lorentzviolating and the Lorentz-invariant effective mass squared difference is which is much smaller than the fractional uncertainties in the values of Δ 2 and sin(2 ) 2 . Moreover, since the solar radius is much larger than the oscillation length, the surviving probability of an electron neutrino detected on the Earth is (neglecting the effect of the matter in the Earth) In our LV case we �nd (2 ) ) cos (2 ) sin 2 (2 ) sin 2 (2 ) √ +cos (2 ) sin 2 (2 ) In the case of solar neutrinos = ⊙ ∼ 10 4 and so we obtain a correction to the neutrino survival probability of order 10 5 , which is well within the experimental errors of solar neutrino observations and also within the uncertainties within which the relevant parameters are known. us, no deviation with respect to solar neutrino experiments is expected.
If, on the other hand, the MSW effect is observed for supernova neutrinos then the adiabatic conversion assumed here is unreliable. However, the high density involved leads to a of at least order unity, and so the corresponding correction to the conversion rate in this model will be appreciable, perhaps allowing for the exclusion of the model.

Experimental Signatures
Once one has included the interaction term (6) to explain superluminal neutrino velocities here on Earth, one needs to deal with its consequences throughout our universe. In particular, it may become appreciable inside of various astrophysical objects. In the case of a spherically symmetric object, (14) tells us that the superluminality at a radius only depends on the density at that radius and the average density at lower radii 0 . is may seem peculiar, since there is no Gauss' law for Π. Indeed, any choice of boundary conditions for Π implies that its value in the core of an object depends on the pro�le at higher radii. However, in our model, and not in that of [16,44], the superluminality only depends on the second derivatives of Π, which is independent of the constants of integration and so of these boundary conditions. is freedom in choosing boundary conditions is necessary for many cosmological applications of the Π �eld, such as the dark energy model of [20] and Galileon cosmologies.
In the core of a spherically symmetric object, in which the density is approximately constant, the deviation from the relativistic dispersion relations is easily approximated. Up to geometrical factors whose magnitude and sign depend on the direction in which the neutrino travels, the fractional superluminosity of neutrinos is simply given by the ratio of the deviation on Earth to the ratio of the average density of the Earth to that of the object's core. For example, in the case of the core of our Sun, whose density varies between 4 and 30 times that of the Earth, the OPERA velocity anomaly would predict a neutrino fractional subluminosity or superluminosity of order between 10 4 and 10 3 . is change in the neutrino's dispersion relation affects its propagator and so may in principle have observable consequences on the various fusion processes occurring in our solar core, perhaps allowing for an exclusion or veri�cation of our model. is is in contrast with the model of [16], in which neutrino superluminality is of order 1 at the surface of the Sun and persists at greater depths including the outer core, where a signi�cant amount of fusion occurs.
However, even in our model the superluminality consistency with OPERA's claim would have led to order 1 deviations from relativity whenever the density reaches about 2 × 10 5 g/cm 3 . is level is easily surpassed, for example, in the cores of older massive stars which fuse carbon or heavier elements [56] and is even reached in white dwarves. us in these situations one may expect drastic departures from the standard Lorentz-invariant quantum �eld theory predictions for amplitudes and decay rates involving the neutrino propagator, potentially affecting, for example, models of the helium �ash. is fact also implies that such models are in general incompatible with anomalies as large as those reported by OPERA.
Another crucial distinction between our model and that of [16] is that our neutrino velocity is direction dependent; radially traveling neutrinos on the surface of the Earth are subluminal. For shallow angles such as those of current accelerator neutrino experiments, the deviation from the relativistic dispersion relations in our model is reasonably independent of the angle, there is only a correction of order of the angle ( /2 ) squared. On the other hand, in the second model of [44], the superluminality is proportional to the cosine of the angle with respect to a preferred direction, which given the symmetries of the problem will likely correspond to the Earth's radial direction.

Electron Superluminality
In addition to the experimental constraints described above one may add that bounds on terrestrial electron 8 ISRN High Energy Physics superluminality are extremely tight. At LEP [57], synchrotron radiation measurements at GeV energies yield a maximum fractional superluminality ( of 5 × 10 15 . is implies that either the neutrino superluminality disappears before the electroweak scale, or else some conspiracy of other effects prevents it from being transmitted to the electron. In [11] the authors noted, as was shown in [42,43], that in the case of a coupling † 0 , a one-loop mixing generates the operator † 0 which leads to a superluminality for electrons which is suppressed by at most 2 2 with respect to that of neutrinos and so is 5 orders of magnitude above the LEP bound quoted above. More complicated breaking models, such as the coupling to sterile neutrinos [11,42,43] and supersymmetric completions [11], are able to push these effects onto higher derivative operators. However, generically this merely increases the exponent of the suppression. One might hope that there exist �avor-asymmetric Lorentz-violating terms which evade the neutrino oscillation constraints from KamLAND. In this case one could simply declare that Lorentz-violation only occurs for muon and perhaps tau neutrinos, hoping that their mixing with electrons is sufficiently suppressed to avoid the LEP synchrotron bound. ere are a number of reasons why this approach fails, but we have seen (Section 4.2) that our terms certainly do not allow such an evasion of the �avor neutrality constraints.