Spin-flavor oscillations of Dirac neutrinos in matter under the influence of a plane electromagnetic wave

We study oscillations of Dirac neutrinos in background matter and a plane electromagnetic wave. First, we find the new exact solution of the Dirac-Pauli equation for a massive neutrino with the anomalous magnetic moment electroweakly interacting with matter under the influence of a plane electromagnetic wave with the circular polarization. We use this result to describe neutrino spin oscillations in the external fields in question. Then we consider several neutrino flavors and study neutrino spin-flavor oscillations in this system. For this purpose we formulate the initial condition problem and solve it accounting for the considered external fields. We derive the analytical expressions for the transition probabilities of spin-flavor oscillations for different types of neutrino magnetic moments. These analytical expressions are compared with the numerical solutions of the effective Schr\"odinger equation and with the findings of other authors. In particular, we reveal that a resonance in neutrino spin-flavor oscillations in the considered external fields cannot happen contrary to the previous claims. Finally, we briefly discuss some possible astrophysical applications.


Introduction
Nowadays it is commonly believed that neutrinos possess nonzero masses and mixing between different flavor eigenstates [1].These properties of neutrinos result in transitions between neutrino flavors, which are called neutrino flavor oscillations [2].Neutrino flavor oscillations are known to happen even in vacuum, i.e., at the absence of external fields.
As constituents of the standard model, neutrinos can interact with other fermions, which a background matter is made of, by exchanging virtual W and Z bosons.This kind of interaction, although it is quite weak, can significantly influence the process of neutrino flavor oscillations resulting in the resonance enhancement of the transition probability, known as the Mikheyev-Smirnov-Wolfenstein (MSW) effect [3].The MSW effect is believed to be the most plausible solution to the solar neutrino problem [4].
Despite neutrinos are electrically neutral particles, nothing prevents them to have nonzero magnetic moments [5,6], which are of a pure anomalous origin.Neutrino magnetic moments result in the particle spin precession in an external electromagnetic field.Thus, a left polarized neutrino, which exists in the standard model, can be transformed to a right polarized particle, invisible to the detectors.If this process happens within one neutrino generation, it is called neutrino spin oscillations [5].There is a possibility for neutrinos to change both flavor and the polarization in an external electromagnetic field.In this situation, these transitions are named neutrino spin-flavor oscillations.Neutrino spin and spin-flavor oscillations were recently reviewed in Ref. [7].
Neutrino spin-flavor oscillations were studied mainly in a constant magnetic field, which is transverse with respect to the neutrino motion.However, other nontrivial configurations of the electromagnetic field, like an electromagnetic wave are of interest.This interest is inspired, e.g., by the suggestion in Refs.[8,9] to explore the neutrino evolution in intense laser pulses.Note that the study on the development of intense lasers in Ref. [10] was recognized by the Nobel committee in 2018.
Neutrino spin and spin-flavor oscillations in matter and an electromagnetic wave were previously discussed in Refs.[11,12] Recently, we demonstrated in Ref. [13] that the results of Ref. [11] are not applicable for the description of spin-flavor oscillations.In the present work, we continue the study of Ref. [13].However, besides the neutrino interaction only with a plane electromagnetic wave [13], now we account for the electroweak interaction of neutrinos with background matter.As in Ref. [13], here we suppose that neutrinos are Dirac particles.Despite multiple models for the neutrino mass generation predict that neutrinos are likely to be Majorana fermions [14], the nature of these particles is still unclear [15].This paper is organized as follows.We start in Sec. 2 with the basics of neutrino electrodynamics in background matter.Then, in Sec. 3, we find the new exact solution of the wave equation for a single neutrino mass eigenstate interacting with matter and a plane electromagnetic wave with the circular polarization.The obtained results are applied in Sec. 4 to describe neutrino spin oscillations in the considered external fields.Then, in Sec. 5, we study neutrino spin-flavor oscillations in matter and a plane electromagnetic wave, with the diagonal magnetic moments being greater than the transition one.The opposite situation, when the transition magnetic moment is dominant, is considered in Sec. 6.Some possible astrophysical applications are also briefly discussed in Sec. 6.Finally, in Sec. 7, we summarize our results.

Neutrino interaction with external fields
In this section, we briefly recall how neutrinos can interact with background matter and an external electromagnetic field.We consider these interactions both in flavor and mass eigenstates bases.
Without loss of generality, we shall study the system of two massive neutrinos (ν α , ν β ) with a nonzero mixing.For example, we can take that ν α ≡ ν µ,τ and ν β ≡ ν e .These neutrinos can electroweakly interact with background matter consisting of electrons, protons, and neutrons.The background matter is supposed to be nonmoving and unpolarized.Moreover, we shall take that neutrinos have nonzero magnetic moments and can interact with the external electromagnetic field F µν = (E, B).
The matrix of the effective potentials of the neutrino interaction with matter is diagonal in the flavor basis: The explicit form of f λ in the electroneutral matter can be obtained on the basis of the results of Ref. [16] as where θ is the vacuum mixing angle, which is chosen in such a way to diagonalize the mass matrix: , where m a are the neutrino masses.The neutrino mass eigenstates ψ a , a = 1, 2, are taken to be Dirac particles.In general situation, the matrices of magnetic moments ) are nondiagonal in the mass eigenstates basis.Using Eq. ( 3), we can rewrite the Lagrangian in Eq. ( 1) in the following way: One can see that the Dirac equations for different mass eigenstates, resulting from the Lagrangian in Eq. ( 4), are coupled due to the presence of external fields.

Solution of the Dirac-Pauli equation
In this section, we study the evolution of a single neutrino mass eigenstate in matter under the influence of a plane electromagnetic wave.We write down the wave equation for a massive neutrino in these external fields and find its exact solution.
In this section, we neglect the mixing between different neutrino types.Thus, using Eq. ( 4) and omitting the index a there, we obtain the wave equation for a Dirac neutrino with the nonzero mass m and the magnetic moment µ, interacting with nonmoving and unpolarized background matter and with the external electromagnetic field, in the form, where ψ is the neutrino bispinor.The effective potential V can be obtained basing on Eqs. ( 2) and (3).We suppose that a neutrino interacts with a plane electromagnetic wave.Neglecting the dispersion of the wave, one gets that the electric and magnetic fields, E and B, depend on t − z.If the wave propagates along the z-axis, one has that B = (B x , B y , 0), and E = (B y , −B x , 0), where B x and B y are linearly independent components of the magnetic field.
We rewrite Eq. ( 5) in the Hamilton form as where α = γ 0 γ, β = γ 0 , and Σ = γ 5 γ 0 γ are the Dirac matrices.If the density of background matter is constant, we can gauge the term V /2 out: ψ → exp (−iV t/2) ψ.It is convenient to introduce the new variables u 0 = t − z and u 3 = t + z.Defining the derivatives with respect to u 0 and u 3 as ∂ 0 and ∂ 3 , one gets that Eq. ( 6) has the following integrals: where ∇ ⊥ = (∂ x , ∂ y , 0) and p ⊥ = (p x , p y , 0).Here we assume that the background matter is uniform.
Then we look for the solution of Eq. ( 6) in the form, where Note that the matrix (1 − α z ) is singular.Thus some of the components of ψ 0 obey the algebraic rather than differential equations.
It is convenient to choose the Dirac matrices in the chiral representation [17].If we define ψ T 0 = (ψ 1 , ψ 2 , ψ 3 , ψ 4 ), then only ψ 2 and ψ 3 are independent and satisfy the equations After the separation the common factor in ψ 2,3 as one gets that the spinor v = v(u 0 ) = (v 1 , v 2 ) T obeys the equation, where σ are the Pauli matrices and Here e z is the unit vector along the wave propagation.Finally, using Eqs.( 8) and (11), the general solution of the wave Eq. ( 5) has the form, where is the basis spinor.The normalization coefficient N is given by the condition |u| 2 = 1.

Neutrino spin oscillations
Now we use the general solution of the Dirac-Pauli equation, found in Sec. 3, to describe neutrino spin oscillations in a plane wave with the circular polarization.We specify the initial condition and find the transition probability.The obtained results are compared with previous findings of other authors.Before we proceed, it is convenient to replace the total wave function ψ in Eq. ( 14) by its projection to the subspace of the linearly independent components ψ 2,3 , The basis spinor ũ, which is the analogue of u in Eq. ( 15), takes the form, ũT = (0, v 1 , v 2 , 0).This spinor is automatically normalized to one if The last condition results from the unitary dynamics of v implied by Eq. ( 12).The mean value of an operator Ô can be found as Ô = ψ † Ô ψ.
In order not to encumber the presentation, we discuss the situation of a neutrino propagating along an electromagnetic wave, i.e. p ⊥ = 0.This case is implemented if neutrinos and an electromagnetic wave are emitted by the same source.Then we consider a wave with the circular polarization, i.e.
, where B 0 is the amplitude of the wave, ω is its frequency, and g = ±1 is the sign factor corresponding to right or left polarizations.
The solution of Eq. ( 12) for a circularly polarized wave has the form, where and is the unit vector, R z is the z-component of the vector R in Eq. ( 13), and v 0 is the initial spinor corresponding to u 0 = 0.
We suppose that, at u 0 = 0, only left polarized neutrinos are presented in the space-time region outside the wave propagation.Thus, we impose the condition Σ z ũ = −ũ on the basis spinor ũ at u 0 = 0.The components of the spinor v 0 are v 1 (0) = 1 and v 2 (0) = 0.
We are interested in the appearance of right polarized particles after neutrinos interact with external fields.It is the situation, which is implemented in neutrino spin oscillations: one looks for right polarized neutrinos in a beam initially consisting of left particles of the same type.Using Eq. ( 17), one obtains that the probability for L → R transitions has the form, In general situation, P L→R in Eq. ( 20) depends on u 0 = t − z.We also note that this expression contains the dependence on the quantum number λ which does not have a clear physical meaning yet.Hence, one should express λ in terms of the neutrino energy and momentum.
The Hamiltonian of Eq. ( 6) explicitly depends on t and z.Thus the neutrino energy E and the momentum p z along the wave propagation direction are not defined.Nevertheless we can define the effective E and p z as Using Eq. ( 17), one gets that where the signs ± stay for initially left and right polarized neutrinos.A right polarized neutrino corresponds to v T 0 = (0, 1) in Eq. ( 17).Finally, using Eqs.( 21)-( 23), we have the energy of left neutrinos as and for right particles.The expansions in Eqs. ( 24) and ( 25) correspond to ultrarelativistic neutrinos with p z ≫ m.One can see that, in this case, the energies have the conventional form.However, for nonrelativistic neutrinos, the effective energies become time and z dependent.
The transition probability depends on the quantity R z given in Eq. ( 13).Using Eqs. ( 21) and (24), one gets that R z has the following form for left neutrinos: Basing on Eqs. ( 20) and ( 26), the transition probability can be rewritten as where we explicitly show the dependence on t and z.Now let us consider the quasiclassical approximation.In this limit, a neutrino moves along a trajectory, which is a straight line z = βt, where β = p z /E is the neutrino velocity.We can represent the transition probability in Eq. ( 27) in the following way: The expression for P L→R in Eq. ( 28) coincides with the result of Ref. [11], where the neutrino spin evolution in matter under the influence of a plane electromagnetic wave was treated within the quasiclassical approach from the very beginning.
5 Spin-flavor oscillations: Great diagonal magnetic moments Now we turn to the study of neutrino spin-flavor oscillations.Here we are interested in the situation of great diagonal magnetic moments.Basing on the results of Sec. 4, we derive the analytical transition probability for this type of oscillations.Using Eq. ( 4), we obtain the system of coupled Dirac equations for the neutrino mass eigenstates ψ a , a = 1, 2, where V a ≡ V aa and µ a ≡ µ aa for a = 1, 2, V ≡ V 12 , and µ ≡ µ 12 is the transition magnetic moment.
We shall analyze the system in Eq. ( 30) in the approximation when µ a ≫ µ.There are multiple models of the neutrino magnetic moments generation.Some of the models predict the diagonal magnetic moments µ a proportional to the neutrino masses m a .In these cases, the value of µ is suppressed because of the Glashow-Iliopoulos-Maiani (GIM) mechanism [6].
We are interested in spin-flavor oscillations of the type ν βL → ν αR , i.e. when both flavor and the polarization are changed.If the above approximations are satisfied, we can derive the analytical expression for the transition probability for ν βL → ν αR oscillations.Indeed, if we neglect V in Eq. ( 30), the neutrino spin evolves independently within each mass eigenstate, as described in Sec. 4. The transitions between different neutrino flavors are solely owing to the vacuum neutrino mixing.As in Sec. 4, here we consider a neutrino beam propagating along the electromagnetic wave.
To describe the evolution of neutrinos, we use the approach developed in Ref. [21], where the initial condition problem is solved.The initial conditions corresponding to ν βL → ν αR are the following.Since there are no right polarized neutrinos initially, we choose ν αR (z, 0) = ν βR (z, 0) = 0.The wave functions of left polarized neutrinos should be chosen like ν αL (z, 0) = 0 and ν βL (z, 0) ∼ exp(ip z z).Such a choice of the initial condition for ν βL (z, 0) corresponds to a broad wave packet.The arbitrary initial wave packets are discussed in Ref. [13].Here the spin projections are defined using the operators (1 ± Σ z )/2.
The projected wave functions of mass eigenstates, given in Eq. ( 16), which satisfy the system in Eq. (30), have the form, ψa (z, t) = s=L,R exp (−iE as t + ip z z) a as ũas , ũT as = 0, v s2 , 0 , where the index s = L, R corresponds to initially left or right polarized neutrinos and the energies E as are given by Eqs. ( 24) and ( 25) with the replacements m → m a and V → V a .Since we neglect V in Eq. ( 30), the coefficients a as are constant and entirely fixed by the initial condition.Using Eq. ( 3), we get that a 1L = sin θ and a 2L = cos θ.Moreover a 1,2R = 0 since there are no right polarized particles initially.
To describe the evolution of the spinors v s in Eq. (32), we use the quasiclassical approximation from the very beginning, i.e. we suppose that z = βt, where β = 2p z /(E 1L + E 2L ) is the center of inertia velocity.Using Eq. ( 17), we get that the components of v aL evolve as where the quantities Ω a and n (a) x,z are the natural generalizations of the corresponding parameters given in Eqs.(18) and (19) with the replacements m → m a , µ → µ a , and V → V a there.The evolution of v (a) R is not important since there are not right polarized neutrinos initially.
Now, using Eq.(34), one obtains the probability for transitions ν βL → ν αR in the form, where is the amplitude of spin oscillations within one mass eigenstate, is the phase of neutrino flavor oscillations accounting for the matter contribution, Φ vac = δm 2 /4p z is the phase of neutrino oscillations in vacuum, and To derive Eq. ( 36) we use the analogues of Eqs. ( 26) and (29).
One can see that Eqs. ( 35) and (36) are the generalization of the corresponding expressions obtained in Ref. [13] for the situation when neutrinos interact not only with a plane electromagnetic wave but also with the background matter.

Spin-flavor oscillations: Great transition magnetic moment
In this section, we continue to study spin-flavor oscillations.However, unlike the case considered in Sec. 5, we discuss the situation of the great transition magnetic moment.
If µ ≫ µ a , we cannot neglect V in Eq. (30).It means that a as in Eq. ( 32) is no longer constant.Analogously to Ref. [13] we suppose that a as = a as (t − z).Our main goal is to find the behavior of a as .Moreover, in the analogue of Eq. (32), we shall use the total wave function ψ as rather than the projection ψas .Hence we look for the solution of Eq. ( 30) in the form, We consider neutrinos propagating along the wave in Eq. (37).Since a as is time dependent for both s = L and s = R, we should account for the time evolution of the basis spinors u aL,R .For this purpose we choose two linearly independent initial spinors v 0 for a = 1, 2, v 0L = (1, 0) T and v 0R = (0, 1) T , which contribute to Eq. ( 17).Substituting Eq. (37) to Eq. ( 30) and taking into account that ∼ exp (−iE as t + ip z z) u as is the solution of the diagonal part of the system in Eq. ( 30), i.e. without V, one gets the equation for the coefficients a as in the form, Using Eq. ( 15), we obtain the following mean values: Then we adopt the quasiclassical approximation, in which ∂ 0 = (1 − β) −1 ∂ t , where β is the mean velocity of the neutrino wave packet, defined in Sec. 5.
In this section, we consider the situation when µ a ≪ µ.It means that the components of the vector n a , which defines the neutrino spin evolution, have the following values: n (a) x = 0 and n (a) z = 1.We can use Eq. ( 17) to compute the mean values of the spinors v as in Eq. (39) assuming that the electromagnetic wave has the circular polarization.Then we define the effective wave function Ψ T = (a 1R , a 1L , a 2R , a 2L ), which obeys the Schrödinger equation, Here where we take that neutrinos are ultrarelativistic particles.Let us introduce the new wave function ΨT = (ã 1R , ã1L , ã2R , ã2L ) as Ψ = U Ψ, where Here Φ ± = Φ vac ± (1 − β)gω/2.The wave function Ψ obeys the equation One can see that the effective Hamiltonian H in Eq. ( 43) generalizes the analogous effective Hamiltonian derived in Ref. [13] for the nonzero interaction of neutrinos with background matter.Moreover, if set (1 − β) → 1 and ω → 0 in Eq. ( 43), we reproduce the effective Hamiltonian for neutrino spin-flavor oscillations in matter under the influence of a transverse magnetic field derived in Ref. [22] using the relativistic quantum mechanics approach.The solution of the Schrödinger equation in Eq. ( 43) results in the algebraic characteristic equation of the forth order, which implies quite cumbersome expressions for eigenvalues and eigenvectors.That is why we again suppose that V ≪ |V a |, as in Sec. 5, to proceed with the analytical solution.The validity of this approximation will be discussed below.
In this case, the evolution of Ψ can be represented in the form, where are the eigenvalues of the Hamiltonian H in Eq. ( 43) and are the eigenvectors.Equation (44) should be supplied with the initial condition of the form, ΨT (0) = (0, sin θ, 0, cos θ) , which means that there are only neutrinos of the type ν βL initially.Using Eqs. ( 44)-( 47), one gets that the coefficients a 1,2R are expressed in the following way: The values of a 1,2L are not important for our purposes since we are interested in spin-flavor oscillations when both flavor and helicity change.
The behavior of the transition probability in Eq. ( 50) is shown in Fig. 1(a) for ν eL → ν τ R oscillations channel versus the distance z ≈ t passed by the neutrino beam.We suppose that the electromagnetic wave has the following characteristics: B 0 = 10 18 G and ω = 10 13 s −1 .The neutrino energy and the transition magnetic moment are taken to be E ν ≡ p z = 1 keV and µ = 10 −11 µ B , where µ B is the Bohr magneton.As mentioned in Ref. [13], these parameters can model neutrino spin-flavor oscillations in the vicinity of a highly magnetized pulsar.To estimate the mean velocity of neutrinos β we assume that the neutrino masses are on the level of 1 eV [24].
The motivation for the choice of the matter density value in Fig. 1 is the following.We can consider neutrino spin-flavor oscillations in the vicinity of a compact astrophysical object surrounded by an accretion disk.For example, properties of a gamma-ray burst (GRB) can be explained by the matter accretion to a central object.In this model of GRB, the matter density of a hydrogen plasma in the inner part of an accretion disk can reach 10 26 cm −3 [27] or be even higher [28].Such values of n e are close to these used in our simulations (especially see Fig. 2 below).Note that this model of GRB predicts a high neutrino emissivity by an accretion disk [27,28].
The function P ν eL →ν τ R (z) is a rapidly oscillating one.It is the typical feature of a neutrino system which experiences spin-flavor oscillations in matter and an electromagnetic field with different oscillations frequencies induced by matter and an electromagnetic field; cf.Refs.[13,21].That is why, here, we show only the upper envelope function and the averaged transition probability.The upper envelope function is built using the spline interpolation of the maxima of P ν eL →ν τ R (z).The transition probability P ν eL →ν τ R (z) is shown only in the inset in Fig. 1(a) for small z.One can see in Fig. 1(a) that the transition probability for the considered oscillations channel reaches only a tiny value ∼ 10 −3 .This fact can be explained by the great value of Φ vac for ν eL → ν τ R oscillations, which is about 2 orders of magnitude greater than other entries in H in Eq. (43).Hence Ω 1,2 ≫ µB 0 (1 − β) and A 1,2 ≪ 1 in Eq. ( 51).Now we compare the exact solution, given in Eqs. ( 50) and (51), of the approximate effective Schrödinger Eq. ( 43), where we put V = 0, with the numerical solution of the exact Eq. ( 43).Should one have the solution ΨT (t) = ( Ψ1 , Ψ2 , Ψ3 , Ψ4 ) of Eq. ( 43), supplied with the initial condition in Eq. ( 47), the transition probability for ν βL → ν αR oscillations can be found as Equation ( 52) can be verified with help of Eqs. ( 42) and (49).In Fig. 1(b), we show the transition probability for ν eL → ν τ R oscillations based on Eq. (52) calculated using the numerical solution of Eq. ( 43) with V = 0.The transition probability P ν eL →ν τ R (z) corresponds to the same parameters of the neutrino system and the external fields, which are used in Fig. 1 43) with V = 0 represents a qualitatively correct description of ν eL → ν τ R oscillations.Now we consider ν eL → ν µR oscillations channel.In this situation, we cannot neglect V in Eq. (43) since θ ≡ θ ⊙ = 0.6 is not small.That is why Eqs.(50) and (51) are not applicable and we have to use the numerical solution of Eq. (43) from the very beginning.
In Fig. 2(a), we show the transition probability P ν eL →ν µR (z), the upper and lower envelope functions, and the averaged transition probability.The values of the parameters of the external fields and the neutrino system, except δm 2 and θ, are the same as in Fig. 1.One can see in Fig. 2(a) that the averaged transition probability oscillates near 5% value.It is much greater than in Fig. 1(a).This feature can be explained by the fact that all the entries of H in Eq. ( 43) are of the same order of magnitude for ν eL → ν µR oscillations unlike the ν eL → ν τ R channel, in which Φ vac is dominant.
In Fig. 2(b), we depict P ν eL →ν µR (z) for lower matter density n e = 10 27 cm −3 , which is very close to the value in the inner part of an accretion disk predicted by the model of GRB in Ref. [28].The transition probability in this case reproduces the result in Ref. [13], where spin-flavor oscillations ν eL → ν µR were described at the absence of the matter contribution.Comparing Figs.2(a) and 2(b), one can see that the lower matter density is, the higher transition probability is.Thus, one does not expect the appearance of a resonance in neutrino spin-flavor oscillations in matter under the influence of a plane electromagnetic wave, as claimed in Ref. [11].The highest transition probability can be observed when neutrinos do not interact with background matter.
To highlight the difference between our results and the findings of Ref. [11] we present the transition probability for ν βL → ν αR , which can be derived on the basis of Eq. ( 21) in Ref. [11].It has the form, where take into account that, for ν eL → ν µ,τ R oscillations channel, A(θ) = (1 + cos 2θ)/2 [30] and f νe − f νµ,τ = √ 2G F n e ; cf Eq. ( 2).One can see in Eq. ( 53) that the amplitude of the transition probability would become ∼ 1 if ∆ = 0.This fact contradicts to out results both in Eqs. ( 50) and (51) and the numerical simulations shown in Figs. 1 and 2. This inconsistency can be accounted for by the incorrect generalization of the Bargmann-Michel-Telegdi equation for the description of neutrino spinflavor oscillations.In general situation, when one studies spin-flavor oscillations of Dirac neutrinos, an effective Schrödinger equation cannot have a 2 × 2 Hamiltonian.Typically, in this kind of problems, one deals with the system of 4 differential equations, e.g., as in Eq. (40) or Eq.(43).

Conclusion
In the present work, we have studied neutrino spin and spin-flavor oscillations in matter under the influence of a plane electromagnetic wave with the circular polarization.Neutrinos are supposed to be massive Dirac particles with nonzero mixing between different neutrino flavors, and possessing arbitrary matrix of magnetic moments.We have started in Sec. 2 with reminding the basic features of neutrino interaction with background matter and an electromagnetic field.
In Sec. 3, we have found the new exact solution of the Dirac-Pauli equation for a massive neutrino with a nonzero magnetic moment interacting with matter under the influence a plane electromagnetic wave.Previously, the solution of the wave equation for a Dirac fermion with an anomalous magnetic moment interacting with a plane electromagnetic wave in vacuum, i.e. at the absence of the electroweak background matter, was known (see, e.g., Ref. [31]).
In Sec. 4, we have applied the solution obtained in Sec. 3 for the description of neutrino spin oscillation in the considered external fields.We have studied the process ν L → R , that is the neutrino spin precession within one neutrino mass eigenstate.The probability P L→R for transitions of this kind has been derived.We have demonstrated that, in the quasiclassical approximation, the expression for P L→R in Eq. ( 28) coincides with the result of Ref. [11], where the neutrino spin evolution in the external fields was studied within the quasiclassical approach from the very beginning.
Then, we have turned to the consideration of spin-flavor oscillations.For this purpose we have formulated the initial condition problem.This approach for the description of neutrino flavor and spin-flavor oscillations in constant external fields has been developed in Ref. [21] earlier.
First, in Sec. 5, we have discussed the case of great diagonal magnetic moments.This situation takes place when a transition magnetic moment is suppressed by the GIM mechanism.If one considers the ν e → ν τ oscillations channel, i.e. relatively small vacuum mixing angle, we can find the analytical transition probability for spin-flavor oscillations of neutrinos with great diagonal magnetic moments in matter and an electromagnetic wave; cf.Eqs. ( 35) and (36).However, the situation of great diagonal magnetic moments is not very interesting from the point of view of phenomenology since the GIM mechanism is valid if µ a ∼ m a [6].It makes µ a to be very small for reasonable neutrino masses [24].Therefore A a ≪ 1 in Eq. (36) and, hence, P βL→αR ≪ 1 in Eq. ( 35).
We have also considered the case of the great transition magnetic moment in Sec. 6.In this situation, we have derived the effective Schrödinger Eq. ( 43) and have found its exact solution for the ν e → ν oscillations channel neglecting V in Eq. ( 43).Comparing Eqs. ( 50) and (51), as well as Eqs.( 35) and (36), with the analogous transition probability derived in Ref. [11], one can see that the results of Ref. [11] are not applicable for the description of neutrino spin-flavor oscillations in the considered external fields.The reason for the discrepancy of our results and those in Ref. [11] has been analyzed in Sec. 6.Then, we have examined the numerical solution of Eq. ( 43) and revealed that the obtained exact solution qualitatively describes ν eL → ν τ R oscillations.
Finally, basing on Eqs. ( 43) and (52), we have numerically studied ν eL → ν µR oscillations in matter with different densities.The transition probabilities have been plotted in Fig. 2. One can see in Fig. 2 that, if one accounts for the high matter density in neutrino spin-flavor oscillation in a plane electromagnetic wave, it diminishes the averaged transition probability.Thus one does not expect the appearance of a resonance in spin-flavor oscillations in the considered external fields, predicted in Ref. [11].
At the end of this section, we mention that described neutrino spin-flavor oscillations in background matter and a plane electromagnetic wave can take place in the vicinity of a highly magnetized compact astrophysical object, emitting intense electromagnetic radiation, being surrounded by dense matter, and being a source of neutrinos.It can be, e.g., a pulsar with a dense accretion disk.The estimates of the parameters of the neutrino system and the external fields, corresponding to the implementation of these spin-flavor oscillations in astrophysical media, are given in Ref. [13] and Sec. 6.