Over the past years, points of connection of plasma physics to various nonlinear equations of significant importance have been explored. An initial connection can be traced back to H. Washimi and T. Taniuti [1], for example, who showed that the one-dimensional asymptotic behavior (as t → ∞ ) of small amplitude ion-acoustic waves was described by the Korteweg-deVries equation—following on a parallel track work of C. S. Gardner and G. K. Morikawa [2]. The paper of A. Jeffrey [3] provides for some systematic details on this particular connection, and it includes remarks, for example, on the work of Y. A. Berezin and V. I. Karpman [4].

In the 2007 paper [5] of J.-H. Lee, O. K. Pashaev, C. Rogers, and W. K. Schief the resonance nonlinear Schrödinger (RNLS) equation

i ψ t + ψ x x + γ | ψ | 2 ψ = δ | ψ | x x | ψ | ψ (1)

appears in connection with a discussion of one-dimensional, long magnetoacoustic waves in a cold plasma subject to a transverse magnetic field B → . Here γ , δ ∈ ℝ = the field of real numbers with δ > 1 , and | ψ | x x / | ψ | is a de Broglie quantum potential. For γ = − 1 / 2 , a complex-valued wave function solution ψ of the form

ψ ( x , t ) = ρ ( x , t ) e − i S ( x , t ) (2)

was obtained, where ρ > 0 is the plasma density and S is a real-valued velocity potential. That is, the velocity field u of the plasma is given by u = − 2 S x . In the present paper we consider for an arbitrary γ < 0 solutions of Equation (1) of the form

ψ = e R − i S (3)

for real-valued functions R ( x , t ) , S ( x , t ) . Such a function ψ is a solution if and only if the pair ( R , S ) is a solution of the Madelung fluid system

R t − S x x − 2 R x S x = 0 S t + ( 1 − δ ) [ R x x + R x 2 ] − S x 2 + γ e 2 R = 0 (4)

independently of the assumption γ < 0 .

The system of main interest for us is the nonlinear magnetoacoustic system (MAS)

ρ t + ( ρ u ) x = 0 u t + u u x + ρ x + β 2 [ ρ x x ρ − 1 2 ( ρ x ρ ) 2 ] x = 0 (5)

which describes the propagation of the aforementioned magnetoacoustic waves in the cold plasma, under some simplifying assumptions that include the uni-axial propagation assumption

B → ( x , t ) = B ( x , t ) k → ,     u → ( x , t ) = u ( x , t ) i → . (6)

Here β > 0 and i → , k → are unit vectors along the x and z axes. The system (5) is derived by way of a shallow water type approximation of the system

ρ t + ( ρ u ) x = 0 u t + u u x + B ρ B x = 0 B = ρ + ( 1 ρ B x ) x (7)

where a change of variables ( x , t ) → ( β x , β t ) is employed (under which the first two equations in (7) are invariant and third one becomes B = ρ + β 2 ( B x / ρ ) x ), and where an expansion of B of the form

B = ρ + β 2 ( ρ x ρ ) x + O ( β 4 ) (8)

is inserted into the second equation [5] [6] [7].

We will work with the following explicit traveling wave solution ( ρ > 0 , u ) of the MAS (5) given by A. Gurevich and A. Krylov (G-K) in [8]. For a choice u 0 > 0 , α 3 > α 2 ≥ α 1 ≥ 0 , define

v = def u 0 / β > 0 ,     a = def + ( α 3 − α 1 ) 1 2 / 2 β > 0 ,     κ = def ( α 3 − α 2 α 3 − α 1 ) 1 2 ∈ ( 0 , 1 ) , C = def + ( α 1 α 2 α 3 ) 1 2 = ( α 1 [ 4 a 2 β 2 ( 1 − κ 2 ) + α 1 ] [ 4 a 2 β 2 + α 1 ] ) 1 / 2 (9)

where the second expression for C in (9) follows as 1 − κ 2 = def ( α 2 − α 1 ) / ( α 3 − α 1 ) and 4 a 2 β 2 = def α 3 − α 1 ⇒ [ 4 a 2 β 2 ( 1 − κ 2 ) + α 1 ] [ 4 a 2 β 2 + α 1 ] = α 2 α 3 . Then for the standard Jacobi elliptic function d n ( x , κ ) with elliptic modulus κ [9]

ρ ( x , t ) = α 1 + 4 a 2 β 2 d n 2 ( a ( x − β v t ) , κ ) , u ( x , t ) = u 0 + C / ρ ( x , t ) . (10)

The choice for δ > 1 in (1) will be δ = def β 2 + 1 . As shown in [10] (also compare [5] [7]), given a solution ( ρ > 0 , u ) of the MAS (5) and the assumption γ < 0 , one can construct a corresponding solution ( R , S ) of the Madelung fluid system (4) where

R = def 1 2 log ( ρ − 2 γ ) ,     S x = def − u 2 (11)

and, moreover, a corresponding solution ( r , s ) of the reaction diffusion system (RDS)

r t − r x x + B r 2 s = 0 s t + s x x − B r s 2 = 0 (12)

where

r ( x , t ) = def e R ( x , t / β ) e ϕ ( x , t ) , s ( x , t ) = def − e R ( x , t / β ) e − ϕ ( x , t ) , ϕ ( x , t ) = def S ( x , t / β ) / β , B = def − γ / β 2 = − γ / ( δ − 1 ) > 0. (13)

In the present case of (10) therefore

r ( x , t ) = [ ρ ( x , t / β ) / ( − 2 γ ) ] 1 2 e ϕ ( x , t )                   = [ α 1 + 4 a 2 β 2 d n 2 ( a ( x − v t ) , κ ) − 2 γ ] 1 / 2 e ϕ ( x , t ) ,

s ( x , t ) = − [ ρ ( x , t / β ) / ( − 2 γ ) ] 1 2 e − ϕ ( x , t )                   = − [ α 1 + 4 a 2 β 2 d n 2 ( a ( x − v t ) , κ ) − 2 γ ] 1 / 2 e − ϕ ( x , t ) . (14)

As before, we see in (11) that S is a potential function for the velocity field u. Note also that by (3) and (11) we obtain the solution

ψ ( x , t ) = [ ρ ( x , t ) / ( − 2 γ ) ] 1 2 e − i S ( x , t ) = [ α 1 + 4 a 2 β 2 d n 2 ( a ( x − β v t ) , κ ) − 2 γ ] 1 / 2 e − i S ( x , t ) , (15)

of the RNLS equation (1).

The formulas (11), (14), (15) relate the nonlinear systems (4), (12) and the resonance nonlinear Schrödinger Equation (1) to the cold plasma system (5) with solution (10). In Section 2 we relate the solution (10) also to nonlinear systems of Broer-Kaup, Boussinesq, and Hamilton-Jacobi-Bellman and their anti-systems given by the time reversal t → − t . Here we find solutions of these systems that generalized in a non-trivial way those found in [11], for example. By choosing κ = 1 so that d n ( x , κ ) = def sech ( x ) , and choosing α 1 = 0 so that C = 0 by (9) and u = u 0 is a constant function in (10), in particular, our r in (14) and v + in (34) of section 2 reduce to the dissipaton e + and shock soliton v + in Sections 2 and 4 of [11].

Attention in Section 4 is turned to further remarks on the cold plasma-2d black hole connection set up in [10]. The main result of that section is the computation of two more plasma dilaton fields such that these combined with the one computed in [10] form a linearly independent set. This too generalizes in a non-trivial way (namely the case α 1 ≠ 0 ) a result found in [12].

Finally, in Section 5, we switch from the traveling wave solution ( ρ , u ) to a plane wave solution of the system (5). Remarkably, its dispersion relation coincides with the dispersion relation obtained from the linearization of the RNLS Equation (1) about a suitably normalized ground state solution ψ 0 .

Throughout, an attempt is made to maintain an expository style in the presentation of the material, for the sake of completeness.

In addition to the solutions (11), (14) of the Madelung fluid and RD systems (4), (12), and the RNLS solution (15) of (1), all of which were constructed by way of the G-K solution (10), we consider now solutions of nonlinear systems of Broer-Kaup (B-K), Boussinesq, and Hamilton-Jacobi-Bellman (H-J-B), and of their time reversal ( t → − t ) systems. Here, again, the G-K solution (10) of the MAS (5) plays an underlying, subtextual role.

It was pointed out in Section 2.1 that various formulas presented in this paper (and in the paper [10]) simplify drastically in case α 1 = 0 ; in general α 1 ≥ 0 . Here we find in this case, in particular, a concrete expression for the potential function S ( x , t ) (and thus also for the function ϕ ( x , t ) ) appearing in some of these formulas.

For α 1 = 0 , u ( x , t ) = u 0 = β v , by (9) and (10), is a constant function: C = 0 . By (11), S x = − β v / 2 , γ e 2 R = def − ρ / 2 , and

R x x + R x 2 = 1 2 [ ρ x x 2 − 1 2 ( ρ x ρ ) 2 ] (53)

by straight-forward differentiation of R. By Maple, for example, the differentiation of ρ on the r.h.s. of (53) can be carried out. For ρ given by (10) and w = def a ( x − β t ) , the result is that this r.h.s. is a 2 κ 2 [ 2 s n 2 ( w , κ ) − 1 ] , or a 2 [ − 2 d n 2 ( w , κ ) + 2 − κ 2 ] by (29). As we have chosen δ in (1) to be β 2 + 1 , we see that the second fluid equation in (4) therefore gives

0 = S t − β 2 a 2 [ − 2 d n 2 ( w , κ ) + 2 − κ 2 ] − β 2 v 2 4 − ρ 2 = S t − β 2 a 2 ( 2 − κ 2 ) − β 2 v 2 4 (54)

since ρ / 2 = 2 a 2 β 2 d n 2 ( w , κ ) by (10), for α 1 = 0 . That is, S t ( x , t ) is the constant function β 2 a 2 ( 2 − κ 2 ) + β 2 v 2 / 4 , or

S ( x , t ) = [ β 2 a 2 ( 2 − κ 2 ) + β 2 v 2 4 ] t + f ( x ) , (55)

for a function of integration f ( x ) . Using again that S x = − β v / 2 , we see that f ′ ( x ) = − β v / 2 ⇒ f ( x ) = − β v x / 2 + c 0 , for some constant c 0 . Thus, in the end, for α 1 = 0 we can choose the potential function S ( x , t ) and the associated function ϕ ( x , t ) in (13) to be given by

S ( x , t ) = β 2 [ a 2 ( 2 − κ 2 ) + v 2 4 ] t − β v x 2 + c 0 , ϕ ( x , t ) = def S ( x , t / β ) / β = [ a 2 ( 2 − κ 2 ) + v 2 4 ] t − v x 2 + c 0 β (56)

for a constant c 0 .

These expressions for S ( x , t ) and ϕ ( x , t ) can be plugged into formulas (14), (15), and (51), for example—taking α 1 = 0 there, to further explicate the solutions r , s , ψ , A + ; keep in mind the assumption γ < 0 :

r ( x , t ) = 2 a β − 2 γ d n ( a ( x − v t ) , κ ) e ϕ ( x , t ) s ( x , t ) = − 2 a β − 2 γ d n ( a ( x − v t ) , κ ) e − ϕ ( x , t ) ψ ( x , t ) = 2 a β − 2 γ d n ( a ( x − v t ) , κ ) e − i S ( x , t ) A + ( x , t ) = log ( [ 4 a 2 β 2 d n 2 ( a ( x − v t ) , κ ) ] − 2 γ ) + 2 ϕ ( x , t ) (57)

for ϕ ( x , t ) , S ( x , t ) given in (56). We also have the formulas for σ ( x , t ) and v ± ( x , t ) in (35) in case α 1 = 0 . In (57), 2 β / − 2 γ = 2 / B , by (13).

Some concluding remarks about the case α 1 = 0 pertain to the conservation laws (16) and (17). These laws imply that rs and r x s x + B ( r s ) 2 / 2 are conserved quantities that give rise to constants of motion

I = def ∫ − ∞ ∞ r s d x ,     J = def ∫ − ∞ ∞ [ r x s x + B ( r s ) 2 / 2 ] d x . (58)

In [16], for example, where α 1 = 0 , κ = 1 (and β = 1 ), the mass M = def − I and energy E = def 2 J constants, in particular, are computed, where the notation e + , e − there (as in [5] [6] [11]) corresponds to r , s here; also – Λ / 4 there corresponds to B = def − γ / β 2 in (13) here. We state the results in terms of our notation, but we also express M and E in terms of the Gurevich-Krylov solution ρ ( x , t ) in (10). First note that by (10), (29), (33),(36)

[ ρ x ρ ( x , t / β ) ] 2 = [ − 8 a 3 β 2 tanh ( a ( x − v t ) ) sech 2 ( a ( x − v t ) ) 4 a 2 β 2 sech 2 ( a ( x − v t ) ) ] 2 = 4 a 2 tanh 2 ( a ( x − v t ) ) = 4 [ ( v + v − ) ( x , t ) + v 2 4 ] (59)

for α 1 = 0 , κ = 1 . Then by (18), (22), (27), (59) r x s x = r v + s v − = − σ v + v − , ( r s ) 2 = σ 2 ⇒

[ r x s x + B ( r s ) 2 / 2 ] ( x , t ) = − σ ( x , t ) [ v + v − − B 2 σ ] ( x , t ) = ρ ( x , t / β ) 2 γ [ 1 4 ( ρ x ρ ) 2 ( x , t / β ) − v 2 4 − B 2 ρ ( x , t / β ) − 2 γ ] . (60)

The result is that

M = def − ∫ − ∞ ∞ ( r s ) ( x , t ) d x = def ∫ − ∞ ∞ ρ ( x , t / β ) − 2 γ d x = 4 a β 2 − γ , E = def 2 ∫ − ∞ ∞ [ r x s x − γ 2 β 2 ( r s ) 2 ] ( x , t ) d x

      = 2 ∫ − ∞ ∞ ρ ( x , t / β ) − 2 γ ( 1 4 ( ρ x ρ ) 2 ( x , t / β ) − v 2 4 ) − ρ ( x , t / β ) 2 8 γ β 2 d x       = − 8 a 3 β 2 3 γ − 2 a β 2 v 2 γ , (61)

using that

∫ − ∞ ∞ sech 2 ( a ( x − v t ) ) d x = 2 a ,       ∫ − ∞ ∞ sech 4 ( a ( x − v t ) ) d x = 4 3 a , ∫ − ∞ ∞ ( tanh 2 sech 2 ) ( a ( x − v t ) ) d x = 2 3 a , (62)

where the latter integral formula in (62) is used to compute the integration of r x s x in the definition of E. Namely, as we have just noted, r x s x = − σ v + v − so by (36) again

( r x s x ) ( x , t ) = 4 a 2 β 2 2 γ sech 2 ( a ( x − v t ) ) [ a 2 tanh 2 ( a ( x − v t ) ) − v 2 4 ] . (63)

An exact connection of the cold plasma system (5) to a two-dimensional Jackiw-Teitelboim (J-T) black hole was investigated in [10], with the resonance NLS Equation (1) serving as a bridge. An explicit change of variables was set up which transformed a plasma metric associated with the system (5) to a J-T metric. This transformation, moreover, provided for a direct calculation of a plasma dilaton field, which with the plasma metric and an appropriate cosmological constant constitutes a solution of the J-T gravitational field equations [17] [18]. The results of [10] represent an extension to the non-trivial case α 1 ≠ 0 of results in [12] —a case discussed in Sections 2 and 3 here. As indicated in the introduction, two more plasma dilaton fields will be computed in this section, to obtain a set of three linearly independent ones altogether.

The J-T gravitational field equations are a system of equations

R ( g ) + 2 Λ = 0 ∇ i ∇ j Φ + Λ Φ g i j = 0 ,       1 ≤ i , j ≤ 2 (64)

of which a solution consists of a triple ( g , Φ , Λ ) where g is a pseudo Riemannian metric with local components g i j , R ( g ) is its Ricci scalar curvature, Φ is a real-valued function of the local coordinates ( x 1 , x 2 ) in which g is expressed (called a dilaton field), Λ is a cosmological constant (and therefore the scalar curvature is a constant), and where, locally, the Hessian is given by

for the Christoffel symbols of g, of the second kind.

For example, the J-T (Lorentzian) black hole solution of the system (64) is given in the coordinates by with

for fixed real numbers, being a black hole mass parameter. Here, and we point out that the sign convention for scalar curvature that we adopt here (and in [10] [12]) is spelled out on page 182 of [19], for example. Thus, for example, our is the negative of that employed in [17] [18]. We will also write for the J-T metric given in (66).

As a second example, we consider the plasma metric constructed in [10] by way of the G-K solution in (10) of the MAS (5). Here the local coordinates, with the notation here not to be confused with the same notation for the solution in (10):

where (again) C is given (9). Obviously this metric is more complicated in structure. For (so that again) and for the choice (as in [5] [6]) it reduces to the metric (6) in [12], where the notation b there corresponds to here. Some remarks herewith are offered to provide some clarification regarding the “raisons d’être” of the plasma metric formula (67).

The classical continuous Heisenberg model realized on a single sheeted hyperboloid

with equations of motion

is equipped with a canonical metric

of constant scalar curvature. The bracket in (69) is just the commutator of two matrices and, and the in (70) are simply Minkowski inner product expressions: for,.

On the other hand, one can construct Lax pairs for this Heisenberg model, and Lax pairs for the reaction diffusion system (12), and establish a gauge equivalence of these two nonlinear systems [16]. More precisely, in our specific setup,

for a (complex) spectral parameter. The equations of motion assertion (69) is equivalent to the assertion that satisfies the zero curvature condition (zcc)

Similarly, a pair of functions is a solution of the RDS (12) if and only if satisfies the zcc

Gauge equivalence means that for some,

which in turn means that one can show that the Heisenberg metric in (70) can be expressed in terms of r and s. The result (a key result) is that

Since the scalar curvature of has the value 2, as we have noted, it is convenient to work with the metric with scalar curvature. Now by definition (18), so by (27)

By formulas (34) then

and by definition (22), by (77). That is, by (75), (76)

The computation of (by (75)) is more involved. By (18) and (22) again, , which can be computed by (27) and (34) again. The end result is that

In the very specialized case of, is given exactly by Equation (63). Formulas (76), (78), (79) (for C given in (9)), which give the structure of the metric were also obtained in [10], by a different method. This metric is non-diagonal:. In Section 3 of [10] a suitable change of variables was constructed by which was transformed exactly to the plasma metric g in (67), which is diagonal. For this, is required to be sufficiently large:

and for, (80)

with the single condition

for. (81)

A clarification regarding how the plasma metric in (67) arises is now established. Also, as we have seen.

We move on now to the main result in [10], which will allow, in particular, for a direct computation of plasma dilaton fields and thus for solutions of the field Equations (64). That main result states that the change of variables for

transforms the cold plasma metric in (67) precisely to the J-T black hole metric in (66), for m and M there given by

Another (more compact) expression is given in (99) for the black hole mass parameter M here, which is indeed positive for

which we assume. Of course the second condition (84) is automatic for and the first condition, in fact the condition, implies the first condition in (80).

Going back to the earlier equations and, we conclude from the equality of these scalar curvatures that m must be given by (83), and moreover that by the first field equation in (64) the cosmological constant must be given by

throughout this paper, and we see that the cosmological constant is negative. The dilaton field for the second set of equations in (64), for the plasma metric, can be derived immediately from the J-T dilaton field in (66):

as in [10]. There are, however, two other J-T dilaton fields, that are also solutions of the second set of equations in (64) for the metric, and therefore by way of the transformation in (82) there are in addition plasma dilaton fields, for the plasma metric which were not computed in [10], which we compute here.

In fact, one can take

so that (as in (86))

which means that we need to find expressions for and, given the definitions (82), (83). For convenience, write for now for. Let

Then, as is easily checked, w has factorization for

which, in turn, can be written as

The argument in [12], for example, leading up to Equation (55) there verifies this assertion. Therefore

On the other hand, given the definitions (82), (83), one has by Maple, for example, that

for C (as usual) in (9). Using that and (by (29)), one can write. In the end,

for

Next, note that in (83)

for the same constant A in definition (11) of [12]:

Also in (83)

It follows that M can also be expressed as

where. Then

for C and A in (95) and (97), respectfully. In summary, the formulas for and in (94) and (100) provide for the computation of the plasma dilaton fields, in (88) for the plasma metric in (67).

As usual, all formulas simplify considerably in case:

by (94), (95), (97), and (100), which gives

Apart from the constant factors and, the dilaton fields in (102) (obtained for) are exactly the ones computed in [12], by a different method; see Equation (10) and Equation (11) there.

The traveling wave solution in (10) of the magnetoacoustic system (5) has been of central interest, of course. Equation (15), with as in (11), relates this solution to the solution of the resonance NLS equation (1). There is another instance, or another sense, in which solutions of (5) and (1) are related, of which some brief remarks are added in this section.

The bond between the system (5) and Equation (1) is illustrated further in [20], for example, where it is shown that they share a dispersion relation. More precisely, in place of the traveling wave solution in (10), consider a plane wave solution of (5) of the form

for constants, wave frequency, and wave number k. A proof of the dispersion relation

for the system (5) is given in [20]. There it is also shown that this dispersion relation coincides exactly with the dispersion relation for the RNLS Equation (1), for a linearization of the latter equation about the ground state (condensate) solution

of it, for the choice. The dispersion relation for Equation (1) is stated (without proof) in [6], for.

The focal points of interest of this paper have been the nonlinear system (5), which describes the propagation of magnetoacoustic waves in a cold plasma in the presence of a transverse magnetic field, the particular traveling wave solution of this system given by Gurevich-Krylov in (10), and the construction of new solutions of other nonlinear systems—elliptic function solutions that we have in fact expressed in terms of the solution. These other nonlinear systems considered were that of a Madelung fluid, a reaction diffusion system (which played a distinct, unifying role throughout the paper), systems of Broer-Kaup, Boussinesq, Hamilton-Jacobi-Bellman, and the Jackiw-Teitelboim system of gravitational field equations. An elliptic function solution of the resonance nonlinear Schrödinger Equation (1) is also expressed in terms of the solution in Equation (11) and Equation (15).

Regarding the gravitational field equations (see (64)), in particular, some black hole solutions () were presented where is a pseudo-Riemannian metric (given in (67)) of constant Ricci scalar curvature 4B (for and in (1) and (5)), the are dilaton fields (given by (86), (88), (94), (100), (102)), and is a (negative) cosmological constant. To obtain these solutions we used a fundamental result in [10] where an explicit change of variables was set up (which is given in definition (82) here) that transforms precisely to the Jackiw-Teitelboim black hole metric in (66), for the values of m and M there given in (83).

Brief remarks in Section 5 further narrate a nexus between the magnetoacoustic system (5) and the resonance NLS Equation (1)—this by way of the dispersion relation (104).

The results presented here, generally speaking, provide for a non-trivial extension of a few selected results obtained in [11] [12], for example. On the other hand, as pointed out in Section 3, we have not considered an extension in the direction of two-soliton solutions of Broer-Kaup and Boussinesq systems, for example, as discussed in [11]; also see [5] [6] [16].

This paper, like that of reference [10], has drawn inspiration from the work of the authors in the references [5] [7], and [21].

The authors declare no conflicts of interest regarding the publication of this paper.

D’Ambroise, J. and Williams, F.L. (2020) Relating Some Nonlinear Systems to a Cold Plasma Magnetoacoustic System. Journal of Modern Physics, 11, 886-906. https://doi.org/10.4236/jmp.2020.116054