Einstein-Yang-Mills wormholes haunted by a phantom field

In this article, we study wormhole spacetimes in the framework of the static spherically symmetric SU(2) Einstein-Yang-Mills theory coupled to a phantom scalar field. We show rigorously the existence of an infinite sequence of symmetric wormhole solutions, labelled by the number of zeros of the Yang-Mills potential. These solutions have previously been discovered numerically. Mathematically, the problem resembles the pure Einstein-Yang-Mills system for black hole initial conditions, which was well-studied in the 90s. The main difference in the present work is that the coupling to the phantom field adds a non-trivial degree of complexity to the analysis. After proving the existence of the symmetric wormhole solutions, we also present numerical evidence for the existence of asymmetric ones.

1. Introduction 1.1.Wormholes.Wormholes are hypothetical models of spacetime that describe traversable tunnels connecting asymptotically flat universes.Possibly the simplest example of a wormhole is the so-called Ellis-Bronnikov wormhole, modelled as the static spherically symmetric spacetime R 2 × S 2 endowed with the Lorentzian metric g = −dt ⊗ dt + r 2 0 cosh 2 (ρ)(dρ ⊗ dρ + g S 2 ), where g S 2 denotes the standard round metric of the sphere and r 0 > 0 is a free parameter.The metric g is asymptotically flat with two ends as ρ → ±∞, which is the main characterizing condition of wormholes.Static spherically symmetric wormholes were defined more generally in the pioneering work of Morris and Thorne [1], and many authors have studied them since, see e.g. the extensive book of Visser [2].Throughout this paper, we will employ the following definition of wormholes in the static spherically symmetric setting, which is essentially equivalent to the definitions of the aforementioned authors.
Definition 1.1.A (static spherically symmetric) wormhole is a spacetime with topology R 2 × S 2 , endowed with a Lorentzian metric of the form g = −e 2τ (ρ) dt ⊗ dt + r(ρ) 2 (dρ ⊗ dρ + g S 2 ) , where τ, r ∈ C ∞ (R) with r > 0, such that g is asymptotically flat with two ends, so that where m ± ∞ , τ ± ∞ ∈ R are finite, and m denotes the Misner-Sharp (or Hawking) mass m = r 2 1 − ṙ2 r 2 .If τ and r are additionally even functions of ρ, then the wormhole is said to be symmetric.
Remark.The asymptotic conditions on the metric coefficients ensure that the induced Riemannian metric on the spacelike slices {t = const.}satisfies in the standard Cartesian coordinates x i .One could obtain decay rates for the derivatives of the metric g ij by imposing additional boundedness assumptions on the derivatives of the mass m, but we do not include this in the general definition.
Note that the asymptotic flatness condition on r implies that there exists at least one point at which r has a minimum.The local minima (resp.maxima) of r are usually referred to as wormhole throats (resp.bellies).If ρ = ρ 0 describes a wormhole throat, then we have ṙ(ρ 0 ) = 0 and r(ρ 0 ) ≥ 0.
In fact, one sometimes requires that the latter is strictly positive at a throat, in which case the condition is called the flare-out condition, although it is strictly speaking not necessary (indeed, the main point is that a wormhole should describe a connection betwen two asymptotically flat universes).It should however be noted that a throat with r(ρ 0 ) = 0 is degenerate in the sense that it has vanishing surface gravity, cf.[3].
Definition 1.1 describes a wormhole as a geometric object, but the ultimate goal is of course to obtain a spacetime model.Thus, one should aim to construct wormhole geometries satisfying the Einstein field equations for some accepted matter model.In doing so, one must show some leniency in deciding which matter models which are to be considered acceptable, as wormholes require support from matter violating the null energy condition [1,2,4].Matter of this type is often called exotic, and is the main reason why wormholes are still considered to be hypothetical from a physics perspective.Possibly the most natural way of modelling exotic matter is by means of a phantom field (or ghost), which is a scalar field with a reversed sign in front of its energy density in the Lagrangian (this will be clarified in the next subsection).Such fields often appear in cosmological research, as they could explain the accelerated expansion of the universe [5].Matter models coupled to such a field will henceforth be referred to as haunted.
1.2.Haunted Einstein-Yang-Mills theory.The haunted theory of gravity that we consider in this work also carries non-abelian electromagnetic charge in the form of a Yang-Mills field, and will be referred to as the haunted Einstein-Yang-Mills (EYM) theory.Let us briefly describe the setting.Let M be a smooth n-dimensional manifold, G a compact Lie group with a bi-invariant metric ⟨•, •⟩, and P a principal G-bundle over M .We consider the haunted EYM Lagrangian where ⋄ g is a semi-Riemannian metric on M with scalar curvature R g and volume form vol g , ⋄ ω is a connection on P with curvature two-form F ω = 1 2 dx µ ∧ dx ν ⊗ F µν , ⋄ ϕ : M → R is a smooth function, called the phantom field, ⋄ the norms are given in local coordinates by Integrating the Lagrangian (3) over compact subsets of M and varying with respect to (g, ω, ϕ) leads to the (trace-reversed) Einstein field equation(s), the Yang-Mills equation, and the phantom field equation: where ⋄ d ω denotes the covariant derivative with respect to the connection ω, ⋄ ⋆ is the Hodge star operator with respect to g, ⋄ g = ∇ µ ∇ µ is the wave operator with respect to g, ⋄ the tensor field ⟨F ω ⊗ F ω ⟩ is given in a gauge and local coordinates by Note that tr g ⟨F ω ⊗ F ω ⟩ = ∥F ω ∥ 2 .The procedure of deriving the equations is standard in literature, so we omit it for brevity.The reader should perhaps only note the reversed sign in front of the scalar field term in (4a).
If the connection ω is flat, so that F ω ≡ 0, then there is no contribution of the Yang-Mills field to the system and one obtains the haunted Einstein equations, which are solved e.g. by the Ellis-Bronnikov wormhole (1).On the other hand, setting ϕ ≡ 0 yields the classical EYM system.1.3.Static spherically symmetric SU(2) ansatz.We are interested in manufacturing wormhole solutions of the system (4a-4c).Following Definition 1.1, we therefore assume that our spacetime has the four-dimensional topology M = R 2 × S 2 and is endowed with a Lorentzian metric g of the form g = −e 2τ (ρ) dt ⊗ dt + r(ρ) 2 (dρ ⊗ dρ + g S 2 ) .We must also choose a principal G-bundle over M and (more importantly) an ansatz for a connection on this bundle.Here, we wish to assume some further symmetries in order to make the problem feasible.To this end, observe that the symmetry group K = SU(2) acts naturally on the spherical factor of M by isometries.A principal G-bundle P π − → M is said to be spherically symmetric (or more generally K-symmetric) if the action of the symmetry group K = SU(2) on M admits a lift to a left action on the total space P by bundle automorphisms.As far as the gauge group G is concerned, one of the simplest non-trivial yet sufficiently rich (cf.next subsection) choices turns out to also be G = SU (2), and we will work with this choice throughout this manuscript.Now, using the general theory of K-symmetric principal G-bundles [6,7], one can show that the equivalence classes of spherically symmetric principal SU(2)-bundles over M are in one-to-one correspondence with non-negative integers 0 ≤ m ∈ Z.Using the same theory, one can also classify spherically symmetric (i.e.invariant under the left action of K = SU(2)) connections on these bundles.In fact, in the only non-trivial case1 m = 1, a gauge can be constructed so that a general spherically symmetric connection has the well-known [8,9,10] where (θ, φ) ∈ S 2 are the standard spherical coordinates coordinates, w, v, a, b are smooth functions of (t, ρ), and X, Y, Z is the standard basis for the Lie algebra su(2) given by Since we are working in the static setting, we will additionally assume that the functions w, v, a, b depend only on ρ and not on t.This leads to the following simplifications: ⋄ We may set b ≡ 0 by a gauge transformation depending only on ρ; ⋄ The Yang-Mills equation (4b) in this setting implies that w and v are constant multiples of one another so that we may also set v ≡ 0 by making a constant gauge transformation; ⋄ Similarly as in [11], it can be shown [12] that if a is not identically zero and the metric g is asymptotically flat with two ends as in Definition 1.1, then the Yang-Mills equation (4b) necessitates w ≡ 0, in which case the haunted EYM system reduces to the haunted Einstein-Maxwell system and the solutions of the equation system can be obtained explicitly [13].We therefore do not lose generality by also setting a ≡ 0. Thus we work with the so-called purely magnetic ansatz depending on a single function w.The corresponding curvature form is given by Last but not least, we also assume that the phantom field ϕ is also static and spherically symmetric, so that it only depends on ρ.For this setting, the phantom field equation (4c) admits the general solution formula which can then be inserted directly back into the Einstein field equation (4a) to eliminate ϕ from the system.
Putting everything together, we see that the haunted EYM system (4a-4c) is equivalent to where (7a) is the Yang-Mills equation and the remaining equations arise from the Einstein field equation (4a).The free parameter π 0 can be interpreted as the charge of the phantom field (6), and setting π 0 = 0 yields the classical EYM theory.In fact, one easily verifies that the equation (7d) is implied by the other three equations (7a-7c), assuming that it holds at least at one point.Hence, we may view it as a constraint on the initial conditions.
1.4.Past and present.The classical SU(2) EYM system, i.e. (7a-7d) with π 0 = 0, was extensively studied in the late 20th century, cf.[14].This was initiated by Bartnik and McKinnon [10] and Bizoń [15], when they numerically found particle-like and black hole solutions to these equations.It has since been mathematically shown that these equations in fact admit infinite sequences of particle-like and black hole solutions.This was first done in the series of papers [16,17,18] by Smoller, Wasserman et al.A complete classification of the solutions to the equations was later provided in [9] by Breitenlohner, Forgács and Maison, which also allowed for a somewhat more elegant existence proof.In a later work [19], Maison also performed a similar analysis of the SU(2) Yang-Mills-dilaton system, which can interestingly be put into a similar form as the EYM system and in fact also allows for an infinite sequence of solutions, although the proof is more involved, despite the simpler appearance of the system.As for the haunted SU(2) EYM framework, i.e. with π 0 ̸ = 0 in (7a-7d), sequences of wormhole solutions have been constructed numerically by Hauser, Ibadov, Kleihaus, Kunz [20], and the main purpose of the present manuscript is to mathematically prove the existence of these solutions.
Theorem A. For each r 0 > 0, there exists a sequence of symmetric wormhole solutions to the system (7a-7d), satisfying r (n) (0) = r 0 .The Yang-Mills potential w (n) satisfies |w (n) | → 1 as ρ → ±∞, has n zeros, and is symmetric, i.e. even or odd with the same parity as n.Furthermore: ⋄ For r 0 ≥ 1, the wormholes have a single throat at ρ = 0. ⋄ For r 0 < 1 and even (resp.odd) n, the wormholes have a non-degenerate throat (resp.belly) at ρ = 0.In particular, the wormholes have at least two throats for odd n.
Remark.By a wormhole solution of (7a-7d), we mean a solution such that the metric coefficients τ and r meet the criteria of Definition 1.1.We also recall that symmetry of a wormhole here means that the metric coefficients τ and r are even functions.
The wormhole solutions from Theorem A bear a lot of resemblance to the black hole solutions of the classical SU(2) EYM equations discussed above.In fact, the proof of Theorem A follows closely the blueprint laid forth in the already mentioned work [9], which essentially boils down to using a shooting method to construct the desired sequences of solutions.However, even though one might expect that this procedure requires only a simple modification of the already existing proofs for the classical EYM system, it turns out that the phantom field destroys certain properties that the classical EYM system has, which also makes the proofs more difficult.In particular, one of the main difficulties here is that certain quantities lose their monotonicity properties and could even oscillate, which makes the behaviour of the solutions somewhat analogous to those of the aforementioned Yang-Mills-dilaton system [19] The shooting method in our case also requires the development of certain new techniques, in particular in the proof of the existence of wormholes whose Yang-Mills potential has an odd number of zeros (the analogues of these solutions were not interesting in the context of classical EYM theory, and consequently were not studied).
1.5.First-order initial value problem.Before proceeding with a description of the proof of Theorem A, we rewrite (7a-7d) as a first-order system (following [9, §6]) by defining the new dependent variables Thus, the system (7a-7d) transforms to together with the constraint (7d) Using this constraint, we can also rewrite (9b) as Remark.Even though the equation (9f) for the phantom term ζ is decoupled from the rest of the system (9a-9e), ζ still appears in the constraint (10), and one uses this constraint repeatedly throughout the analysis.E.g. we will often use the alternate forms (11) of the equation for N .We therefore keep ζ as a dependent variable.
The system (9a-9f) is regular as long as r > 0. Hence, for any choice of initial conditions with r(0) > 0, there exists a unique local (real) analytic solution to the problem by standard ODE theory.
Note that the radial function r of a wormhole spacetime requires at least one point at which r is stationary (cf.Definition 1.1), so it is natural to assume the initial value N (0) = 0. Note that so that if r(0) + w(0) 2 > 1, then the initial conditions describe a wormhole throat.However, since the wormhole could have several throats, the stationary point could also describe a belly, so we do not enforce this condition.In fact, we will mainly focus on symmetric wormholes, and in some cases they will be symmetric around a belly rather than a throat.For the constraint (10) to be satisfied, we also need to assume which can only be satisfied if the right hand is non-negative.The initial value κ(0) is not a priori constrained in any way, other than the requirement that it should be finite (note that, for a black hole horizon, one would need κ(0) = ∞ [9, §6]).However, the analysis of the equations is considerably simplified by making the assumption κ(0) = 0, which we will do throughout the manuscript.Finally, the initial values w(0) and U (0) for the Yang-Mills potential are allowed to be arbitrary, but we assume for simplicity that |w(0)| ≤ 1 because the solutions that exit the strip |w| ≤ 1 will turn out to be ill-behaved.Thus, we supplement the system (9a-9f) with the initial conditions r(0) = r 0 , w(0) = w 0 , κ(0) = 0, such that the parameters (r 0 , w 0 , U 0 ) belong to the set of admissible initial data where we denote by the initial value of the energy, a quantity which will turn out to have useful properties.
Remark 1.2.This particular choice of initial conditions depends continuously (note the square root in the initial condition for ζ) on the initial data (r 0 , w 0 , U 0 ) ∈ I 0 , so the solutions of the initial value problem also depend continuously on the initial data.
Remark 1.3.Since we will eventually want to transform back to the original variables (τ, r, w), we finally wish to recall here that the initial value τ 0 of the temporal metric coefficient τ is kept free and instead we fix the phantom charge in order to remain compatible with ζ = π 0 /(re τ ).
Thus, the general solution to the initial value problem with initial data (r 0 , w 0 , U 0 ) ∈ I 0 satisfies the identities Solutions with either w 0 = 0 or U 0 = 0 are therefore symmetric, since in that case r, ζ are even functions, while N, κ are odd.Moreover: ⋄ If U 0 = 0, then w is even, so these are often referred to as even solutions.
⋄ If w 0 = 0, then w is odd, so these are often called odd solutions.In particular, we see here that w 0 = U 0 = 0 implies w ≡ U ≡ 0. With these symmetries in mind, we see that it suffices to study the solutions for ρ ≥ 0. 1.6.Proof summary and organization.To prove Theorem A, we wish to show the existence of initial data of the form (r 0 , w 0 , 0) and (r 0 , 0, U 0 ), for which the solution of (9a-9f,12) is defined for all ρ ≥ 0 and the dependent variables have the following limits as ρ → ∞: where 0 < α = π 0 e −τ∞ < ∞ and 0 ≤ β = 2m ∞ < ∞.The proof is based on a shooting method, in the sense that we consider infima over suitably chosen subsets of the set of initial data I 0 , with the expectation that these infima correspond to initial data describing the desired global solutions.The proof consists of three main ingredients: ⋄ Classification theorem ( §2): It turns out that, just as in the setting of [9], the initial value problem admits three possible types of solutions, classified according to the behaviour of N .In fact, N plays a more important role than the other dependent variables, since it will turn out the solution can only stop existing if N → −∞, and even in that case the remaining dependent variables stay bounded.Of particular importance will be the dichotomy between the regions N + ζ < 0 and N + ζ ≥ 0, which also demonstrates that the phantom field ζ affects the solutions in a non-trivial way.Indeed, any orbit entering the former region will turn out to be singular, whereas the orbits staying in the latter region will be well-defined for all ρ ≥ 0. The strip |w| ≤ 1 will also play a major role, and any orbit exiting it will also turn out to be singular.These facts will allow us to work in the region {N + ζ ≥ 0, |w| ≤ 1}, in which the solutions are generally well-behaved.We will then study the asymptotic behaviour of the dependent variables, depending on the behaviour of N (in particular the number of its zeros and its sign near infinity), and show that only a handful of cases can occur.One of the biggest difficulties will be the fact that, prima facie, we do not know whether the dependent variables even have limits at infinity, so that various techniques will be applied to extract these limits (note also Remark 1.6 below).An important tool for this will be a simple result called Barbȃlat's lemma.
We recall that a simple sufficient condition for the uniform continuity of f is that its derivative is bounded (provided that f is differentiable).⋄ Neighbourhood theorem ( §3): For each solution type, we will study the solutions with nearby initial data.Such a result will provide us with a mechanism of controlling which solution types the aforementioned infima can describe.The proof is mainly based on the fact that the solutions depend continuously on the initial data, but certain cases require a closer analysis (again, note also Remark 1.6 below).⋄ Energy theorem ( §4): We study solutions with small resp.large initial energy E 0 .This will provide us with an upper and lower bound for the shooting method.The small case E 0 = 0 will follow by a simple analysis of the initial conditions.The case when E 0 is large will, however, be much more involved.In fact, this case has not been studied in the aforementioned citations, so the proof given here involves completely new techniques developed specifically for the problem corresponding to wormhole initial conditions.With these three results in hand, Theorem A will follow by a simple shooting method argument, the details of which we leave for §5.
Remark 1.6.We would like to point out a potential gap in some of the the proofs given in [9] for the analogues of the above mentioned theorems.Therein, the authors study the asymptotic behaviour of the dependent variables using some heavy machinery of dynamical systems, namely the theory of structurally stable vector fields [22, §1.3] (particularly in their analogues of the classification and the neighbourhood theorem).This is done by viewing the Yang-Mills equation ẅ + (κ − 2N ) ẇ + w(1 − w 2 ) = 0 as a perturbation of the Yang-Mills equation in the flat limit (κ → 1, N → 1) and the cylindrical limit The latter equation is the so-called Duffing type equation, which can be studied using the elementary theory of planar autonomous ODE systems.While this certainly provides a good heuristic overview of how the solutions should behave, the author of the present manuscript does not understand how one can mathematically apply the theory of structural stability in this context.Aside from some technical difficulties such as the fact that the vector field corresponding to the equation is tangential to (at least some points of) the boundary of any compact set containing the equilibria (whereas the theory assumes transversality at the boundary), the entire theory of structural stability only applies to autonomous perturbations of autonomous planar dynamical systems.On the other hand, the idea here is to consider (κ − 2N + 1) ẇ as a small (for large ρ) perturbation of the flat Yang-Mills equation, with κ and N being interpreted as fixed externally given functions.But such a perturbation is clearly non-autonomous, so that the theory of structural stability cannot be applied directly.The author was also unable to find other references containing results that could be applied in this context.In view of this, we take on a more raw analytical approach in the present work, which arguably also simplifies the proofs.We would like to point out that the methods used in this work can also be applied in the context of the above mentioned particle-like and black hole settings, if this is indeed deemed necessary.

Classification of solutions
The goal of this section is to show the following classification result.
Theorem 2.1 (Classification theorem).Any solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 belongs to one of the following classes: (i) Singular: There exists a finite point ρ ∞ > 0 such that and the remaining dependent variables remain bounded as ρ → ρ ∞ .(ii) Asymptotically cylindrical: The solution is defined for all ρ ≥ 0, stays in the region |w| ≤ 1, and the dependent variables have the following limits at infinity: Furthermore, either ⋄ r ≡ 1 and w ≡ 0, or ⋄ r 0 < 1, (w, U ) → (0, 0) as ρ → ∞, and w has infinitely many zeros.(iii) Asymptotically flat: The solution is defined for all ρ ≥ 0, stays in the region |w| ≤ 1, and the dependent variables have the following limits at infinity: Remark.Note that rζ = π 0 e −τ , so that τ has a finite limit at infinity in case (iii) provided that π 0 ̸ = 0.By the constraint (10), this limit can be calculated as but does not seem to admit a closed form in terms of the initial conditions.
This classification is highly reminiscent of the one given in [9, Theorem 16], where the Einstein-Yang-Mills equations (with no phantom field) are studied for particle-like and black hole initial conditions.The proof in our context is, however, more involved in view of the increased complexity of the behaviour of N .In fact, the main feature of the phantom system (as opposed to the phantomless one) is that N = ṙ/r is allowed to change sign without the orbit being singular.
2.1.Trivial solutions.Note that for w 0 ∈ {−1, 0, 1} and U 0 = 0, we have that w is identically constant w ≡ w 0 and hence also U ≡ 0. In this case we can explicitly solve The remaining non-trivial equation is the Riccati type equation If (w 0 , U 0 ) = (±1, 0), then w ≡ ±1 and we can also get the explicit solutions for any r 0 > 0, corresponding to the Ellis-Bronnikov family of wormholes (1).
For solutions with w 0 = U 0 = 0, we have w ≡ 0. In this case, the Yang-Mills connection ( 5) is u(1)-valued and the SU(2) Yang-Mills theory degenerates to the classical Maxwell theory with gauge group U(1).These solutions can be computed explicitly as Note that the necessary assumption E 0 ≥ 0 implies that r 0 ≥ 1.There are two separate cases: ⋄ If r 0 = 1, then r ≡ 1 and thus N ≡ 0. This solution is asymptotically cylindrical.⋄ If r 0 > 1, then the solutions are asymptotically flat.They represent the abelian wormhole family, which has been obtained in [13] as a solution of the haunted Einstein-Maxwell system.

Proof of the classification.
To simplify the statements of certain results, we say that a region U ⊂ R 6 in the phase space is (forward) invariant if it has the following property: if there is a point ρ 0 ≥ 0 such that the solution enters U at ρ = ρ 0 , then it stays in U for all ρ ≥ ρ 0 , i.e. [∃ρ For a trivial example, we see from (9f) that the region ζ > 0 is invariant.Throughout the rest of the manuscript, we will make extensive use of certain energy functions related to the equations.In view of this, they deserve a proper definition.
Definition 2.2.The energy of the system (9c-9f) is defined as the function where the second equality follows from the constraint (10).The autonomous energy is defined as We first derive some basic inequalities.
Lemma 2.3.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .For all ρ ≥ 0 for which the solution is defined, we have Remark.The first set of inequalities implies that the temporal metric coefficient τ is non-decreasing, since κ − N = τ .Looking at the last two inequalities, one might hope that the stronger inequality κ + N ≤ 2 + ζ holds, but this is in fact not true.Indeed, numerical approximations suggest that this inequality is violated when the initial energy E 0 is large.
Lemma 2.5.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .Suppose that the solution is defined (at least) for 0 < ρ < ρ, and that N remains bounded as ρ → ρ.Then all the dependent variables remain bounded as ρ → ρ and the solution can be continued across ρ.
Remark.In [9], the authors show an analogue of Lemma 2.5 for their setting when N is lower bounded by a positive constant [9, Proposition 9] and when N is negative [9, Proposition 13], but they do not show the result when N approaches 0 from above at ρ.This last case was likely just forgotten, although strictly speaking it is also necessary for their setting.
Proof.Since N is bounded, it follows that r is also bounded by (9a).From Lemma 2.3, we directly see that ζ is bounded, and also so κ is bounded as well.So it remains only to study w and U .For this we will use the energies from Definition 2.2.Note that the energy E = 2κN − N 2 + ζ 2 is bounded and hence the autonomous energy F is bounded as well.In particular, we see that w is bounded if and only if U is bounded, so it suffices to show that w is bounded at ρ. Aiming to reach a contradiction, assume that w is unbounded at ρ.We first note that, since w is unbounded, it must enter the region |w| > 1 for some 0 ≤ ρ 0 < ρ.In view of the symmetry (w, U ) → −(w, U ) (cf.Remark 1.4), we can without loss of generality assume that w > 1.In this region, w is monotone since so ẅ| ẇ=0 > 0, and hence ẇ > 0 for w > 1.Thus |w| → ∞, and hence by the Cauchy-Schwarz inequality as ρ → ρ, which implies that ẇ is not square integrable near ρ.We will reach the desired contradiction by showing that ẇ is, in fact, square integrable near ρ.Note that Ṅ → −∞ by (9b) since κ, N, r are bounded and |w| → ∞.It follows that N decreases for ρ − δ ≤ ρ ≤ ρ if δ > 0 is sufficiently small, and in particular the limit lim ρ→ ρ N = N exists.We now consider two cases separately: (i) If N < 1 2 tanh(ρ), then we can choose δ > 0 so small that 2N − tanh(ρ) ≤ −c for ρ − δ ≤ ρ ≤ ρ and some positive constant c.By Lemma 2.3 (i), we then have , then b is bounded since r and N are, and we have for some constant c > 0, since κ − N ≥ 0 by Lemma 2.3 and F is bounded.This implies that ẇ is square integrable over ρ − δ ≤ ρ ≤ ρ.Thus, ẇ is square integrable near ρ in both cases, which gives the desired contradiction.□ On the other hand, the following result characterizes singular orbits.
Lemma 2.6.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .
(i) The region {|w| > 1, w ẇ > 0} is invariant and any solution that enters it also enters the region N + ζ < 0. (ii) The region N + ζ < 0 is invariant and any solution that enters it is singular, cf.Theorem 2.1 (i).
Proof.Suppose that the orbit enters the region {|w| > 1, w ẇ > 0}.In view of the symmetry (w, U ) → −(w, U ) (cf.Remark 1.4), we can assume without loss of generality that there is a point ρ 0 ≥ 0 with w(ρ 0 ) > 1 and ẇ(ρ 0 ) > 0. Note that for w > 1, so ẅ| ẇ=0 > 0, which shows that w must keep increasing and hence the region {w > 1, ẇ > 0} is invariant, so (w, ẇ) remains there for all ρ ≥ ρ 0 .Next, we want to show that the orbit enters N + ζ < 0, so we study the orbit while it resides in the region 3. Note that the orbit exists as long as it stays in this region in view of Lemma 2.5.By Lemma 2.3, we have Put T = (w 2 − 1)/r > 0 and calculate (cf.[9, Proposition 11]) Thus, |T U | increases strictly and uniformly for sufficiently large ρ, so the solution eventually reaches (and stays in) the region In this region, (11) gives so N uniformly decreases for large ρ, and thus it eventually reaches the region N + ζ < 0 (recall from Lemma 2.3 that ζ approaches zero), proving (i).Now to prove (ii), put Since κ, ζ ≥ 0, we see that ξ decreases in the region ξ < 0 and consequently this region is preserved once reached.In particular, if the orbit enters it, we have ξ ≤ −ξ 2 , implying that ξ → −∞ at some finite point ρ = ρ ∞ , which in turn implies that N → −∞ as ζ is bounded (note that none of the other variables can explode before N → −∞ in view of Lemma 2.5).Finally, we show that the other dependent variables remain bounded near the singular point ρ ∞ .This will also imply that r → 0 at ρ ∞ e.g. by (9b).To this end, we adapt the techniques from [9, Proposition 13].In fact, we only present the proof of the boundedness of w, as the boundedness of other variables follows in essentially the same way as in the citation, with only minor modifications.
Since w is trivially bounded if it remains in the strip |w| ≤ 1 for all ρ < ρ ∞ , we consider only the case when w enters the invariant region {|w| > 1, w ẇ > 0}, and, as above, we assume without loss of generality that w > 1, ẇ > 0. Put η = −r(N + ζ) = −rξ.For sufficiently small δ, we have N + ζ < 0 and thus η > 0 for ρ ∞ − δ < ρ < ρ ∞ .We will show that wη −ε is bounded near ρ ∞ for 0 < ε < 1  2 .This will imply that w is bounded because the constraint (10) gives so that η increases and in particular stays away from zero near ρ ∞ .We have where the last inequality follows since w > 1 and η > 0. Now by the Cauchy-Schwarz inequality, we get so it suffices to show that the two integrals on the right-hand side are finite as ρ → ρ ∞ .For the first integral, we can estimate (because η increases) and since all the integrands on the right hand side are non-negative, their separate integrals must all be finite, in particular the one involving U .For the second integral, we write so that the integral of η near ρ ∞ is finite, and Hölder's inequality implies and the latter is finite since r > 0 is decreasing.Thus, w is bounded near ρ ∞ , as desired.□ In view of Lemma 2.6, we may assume for the rest of the proof of Theorem 2.1 that the solution remains in the regions N + ζ ≥ 0 and |w| ≤ 1.
Lemma 2.7.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .Assume the solution satisfies N + ζ ≥ 0 and |w| ≤ 1 for all ρ ≥ 0 for which it exists.Then the solution is well-defined for all ρ ≥ 0, and furthermore: (i) the integral ∞ 0 N exists and has finite negative part, (ii) r has a non-zero limit at infinity, which is finite if and only if N → 0, (iii) all other dependent variables remain bounded as ρ → ∞.
Remark.We would also like to point out that, a priori, N could oscillate, i.e. the integral could be of the form ∞ − ∞, so the existence in (i) is a non-trivial matter.In part (iii), we make no claims about the existence of limits at infinity -this will be studied in the subsequent lemmata.
Proof.By the bounds in Lemma 2.3, we see that |N | stays bounded as long as N + ζ ≥ 0, and therefore the solution is well-defined for all ρ ≥ 0 by Lemma 2.5.
By the monotone convergence theorem and Lemma 2.3, we have lim On the other hand, since N + ζ ≥ 0 by assumption, we also see by the monotone convergence theorem that lim where the integral on the right-hand side could be infinite.Thus, where we may take the limit on each term separately since they both have definite sign, and the negative part, i.e. the integral of ζ, has finite limit.Note that this also implies that the negative part of the integral of N is finite and in particular the (Lebesgue) integral of N over [0, ∞) exist (but could be infinite).Now equation (9a) implies so that r has a limit at infinity, which is non-zero because the integral of N cannot be negatively infinite.For the second claim in (ii), note that if N → 0, then the constraint (10) shows that lim inf since also ζ → 0 and κ is bounded due to the inequality κ + N ≤ 2 + √ E 0 .This implies that r cannot be unbounded (note that |w| ≤ 1 for N + ζ ≥ 0 by Lemma 2.5) and hence has a finite limit by the preceding part of the lemma.On the other hand, if r has a finite limit, then so does log r r0 = ρ 0 N , and since Ṅ is bounded by (9b), it follows that N → 0 by Barbȃlat's lemma (Lemma 1.5).
For (iii), we first note that that κ where the first inequality follows by assumption and the second inequality follows from Lemma 2.3.It follows that the energy (15) is bounded.Furthermore, |w| ≤ 1 because the assumption N + ζ ≥ 0 implies that w cannot exit this region, cf.Lemma 2.6 (i).Since r stays away from zero at infinity by the already proven part of the lemma, we see that is bounded, and thus so is Now we wish to consider three cases separately: (i) N has infinitely many zeros, (ii) N has finitely many zeros and N < 0 after the last zero, (iii) N has finitely many zeros and N > 0 after the last zero.
Before dealing with each of these cases, we would like to prove some preparatory results.First, we provide a lemma which would thematically be a better fit for the next section, but we will use it in this section as well, so we state and prove it somewhat ahead of time.
Suppose that N ever reaches zero again in the region |w| ≤ 1, so that there exists ρ > 0 with N > 0 and |w| ≤ 1 for 0 < ρ < ρ, as well as N (ρ) = 0. Then r increases on this range and r(ρ) > r 0 ≥ 1, giving, by the same estimate as above, that Ṅ (ρ) > 0. This is a contradiction, so that we must have N > 0 for all ρ > 0. □ The next result tells us that the condition N → 0 as ρ → ∞ is in fact a characterizing property of asymptotically cylindrical orbits.Lemma 2.9.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .If N → 0 as ρ → ∞, then the solution is asymptotically cylindrical, cf.Theorem 2.1 (ii).
Proof.We first note that r has a finite limit 0 < r ∞ ≤ 1 by Lemma 2.7 (ii).Furthermore, the energy (15) tends to 0 (since κ is bounded and ζ → 0).Now the autonomous energy (16) satisfies ∞ .For any ρ 0 ≥ 0, we also have If ρ 0 is selected so large that κ − 2N ≥ c for ρ ≥ ρ 0 and some constant c > 0 (this is possible since lim inf κ ≥ 1 and N → 0), then we see by the monotone convergence theorem that and hence ẇ is square-integrable near infinity.Since is bounded (note that ẇ is bounded because F and w are), we see that ẇ2 is uniformly continuous, and hence ẇ → 0 by Barbȃlat's lemma (Lemma 1.5).Thus U → 0, as well as κ → 1 by Lemma 2.4.Now (1 − w 2 ) 2 = 2 ẇ2 − F has a limit at infinity, and hence w also tends to some limit |w ∞ | ≤ 1 by continuity.By equation (9c), we must have ∞ ), and any other choice of w ∞ would contradict ẇ → 0. But w ∞ = ±1 is impossible since that would imply the absurdity F → 0 = −r 2 ∞ .It follows that w → 0, and from E → 0 we also get r → 1. Next, we observe that the only asymptotically cylindrical solution with r 0 ≥ 1 is the trivial orbit with r ≡ 1 and w ≡ 0 by Lemma 2.8 (since otherwise N > 0 and r > 1 for ρ > 0 with |w| ≤ 1, and we cannot have r → 1).On the other hand, for r 0 < 1 the trivial solution w ≡ 0 has E 0 < 0 and thus is not admissible.Therefore it only remains to show that w truly has infinitely many zeros in the case r 0 < 1.To this end, we consider the polar angle defined by and extended smoothly across zeros of w.Note that this is well-defined because (w, ẇ) stays away from the origin, since w ̸ ≡ 0. A simple calculation yields Now since 2|w ẇ| ≤ w 2 + ẇ2 , But the right hand side of the latter inequality tends to 0, so lim sup θ ≤ − 1 2 , implying that θ → −∞, and thus w necessarily crosses zero infinitely many times.□ With Lemma 2.9 in hand, we can now continue the proof of Theorem 2.1, by tackling the different cases depending on the number of zeros of N , as already hinted.
Lemma 2.10.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .If N has infinitely many zeros, then the solution is asymptotically cylindrical, cf.Theorem 2.1 (ii).
Proof.Let ρ n be the increasing sequence of zeros of N .Note that ρ n must be unbounded by Lemma 2.5 and the fact that the region N < −ζ is invariant, so that N can only have zeros while staying in the region −ζ ≤ N ≤ 1.Since r tends to some limit at infinity by Lemma 2.7 (ii), we may use the constraint (10) which is finite since w is bounded by Lemma 2.7 (iii).This implies that the limit of r is finite, and thus N → 0 by Lemma 2.7 (ii).Hence, we may apply Lemma 2.9 to conclude.□ Lemma 2.11.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .Assume there is a point ρ 0 ≥ 0 such that N (ρ 0 ) = 0 and N (ρ) < 0 for ρ > ρ 0 .Then the solution is singular, cf.Theorem 2.1 (i).
Proof.In view of Lemma 2.6, we only need to show that N exits the region −ζ ≤ N < 0. Aiming to reach a contradiction, assume that N remains in this region for all ρ > ρ 0 .Then we also have |w| ≤ 1 in view of Lemma 2.6 (i).Furthermore, we see that N → 0 as ρ → ∞ (since ζ → 0), and hence r → 1 by Lemma 2.9.But N is negative for ρ > ρ 0 , so we must have r > 1 on this range, in particular also at ρ = ρ 0 where N (ρ 0 ) = 0 and so implying that N > 0 for sufficiently close ρ ≥ ρ 0 , which is a contradiction.□ Lemma 2.12.Consider a solution of the initial value problem (9a-9f, 12) with respect to fixed initial data in I 0 .Assume there is a point ρ 0 ≥ 0 such that N (ρ) > 0 for all ρ > ρ 0 .
(i) If r is bounded, then the solution is asymptotically cylindrical, cf.Theorem 2.1 (ii).
(ii) If r is unbounded, then the solution is asymptotically flat, cf.Theorem 2.1 (iii).
Proof.Part (i) follows trivially from Lemma 2.9 since N → 0 by Lemma 2.7 (ii).For part (ii), we first show that U → 0. We consider separately the cases where w has finitely or infinitely many zeros.
If w has finitely many zeros, then there is a ρ ≥ 0 such that, without loss of generality, 0 < w(ρ) ≤ 1 for ρ ≥ ρ.Define the function where we integrate by parts in the last equality.Note that w is bounded and r → ∞, so that the first term on the right-hand side tends to 0, while the final integral also has a finite limit since it is a bounded increasing function of ρ.Thus v has a finite limit as infinity, and since v = U is bounded by Lemma 2.7 (iii) and (9d), it follows from Barbȃlat's lemma [21] that v = U → 0 in this case.
If w has infinitely many zeros, then so does U and we can find a sequence ρ k → ∞ with U (ρ k ) = 0. Since κ − N ≥ 0, we see that the energy satisfies and hence where in the end we let k → ∞.Since trivially lim inf E ≥ 1 (because r is unbounded and w is bounded), we see that E → 1.This implies that 2U 2 → 0 in this case as well.By Lemma 2.4, we now get κ → 1.From the constraint (10), we see that and hence N → 1. Next, we wish to show that ẇ → 0. Note that this does not follow directly from the fact that U = ẇ/r → 0 since r is unbounded.It is not even clear, prima facie, whether ẇ is bounded -this does not follow from Lemma 2.7 (iii), since we do not consider ẇ as one of the dependent variables.
If w ∞ = 0, we need to show that the solution is the trivial w ≡ 0. In fact, we see that F → −1, and since F is non-decreasing for large ρ and F ≥ −1, we necessarily have F ≡ −1 which implies w ≡ 0. The discussion in §2.1 also implies that in this case r 0 > 1.
Finally, we need to study the limits of rζ and r(1 − N 2 ) at infinity.Note that d dρ log(rζ) = N − κ ≤ 0 by Lemma 2.3, so rζ is non-increasing and by the monotone convergence theorem.Therefore, to show that rζ has a finite positive limit, it suffices to show that the integral on the right-hand side converges.By (11), Hence, the claim will follow if we can show that of U and ζ are square integrable near infinity, since N → 1.But the integrability of U 2 follows trivially from the integrability of ẇ2 = (rU ) 2 (since r → ∞), whereas the integrability of ζ 2 follows directly from the bound ζ 2 ≤ E 0 sech 2 (ρ), cf.Lemma 2.3.On the other hand, we have and the integral converges as ρ → 0 since the quantity in the parentheses converges the finite quantity (1 − w 2 ∞ ) 2 − α 2 .Therefore r(1 − N 2 ) has a finite limit at infinity by dominated convergence, and this limit must be non-negative since N → 1 and N ≤ 1 (cf.Lemma 2.3).□ We now have essentially all the ingredients necessary to complete the proof of Theorem 2.1.To summarize, the pieces of the puzzle can be put together as follows.In Lemma 2.5 we showed that the solution can be continued as long as N remains finite, and in particular the only way that a solution stops existing at a finite point ρ = ρ ∞ is if N → ∞ (and r → 0), which is precisely the behaviour describing the singular orbits from Theorem 2.1 (i).In Lemma 2.6 we showed that such singular behaviour happens precisely when the solution enters the region N + ζ < 0, and we also showed that the solution enters this region if it exits the strip |w| ≤ 1.This allowed us to assume that the solution satisfies N + ζ ≥ 0 and |w| ≤ 1, in which case it must be globally defined by Lemma 2.5 and the bounds from Lemma 2.3.In Lemma 2.7 we showed that the remaining dependent variables remain globally bounded and, most importantly, that r has a limit (which may be infinite) at infinity.The remainder of the proof then revolved around studying the different possible behaviours of N , depending on its number of zeros: ⋄ In Lemma 2.10 we treat the case when N has infinitely many zeros, and show that the solution is then asymptotically cylindrical as in Theorem 2.1 (ii); ⋄ In Lemma 2.11 we treat the case when N has finitely many zeros and is negative after the last zero, in which case the solution is singular as in Theorem 2.1 (i); ⋄ In Lemma 2.12 we treat the final case when N has finitely many zeros and is positive after the last zero, in which case the solution asymptotically cylindrical Theorem 2.1 (ii) if r is bounded, and asymptotically flat as in Theorem 2.1 (iii) if r is unbounded.Since this exhausts all the possible cases, the proof of Theorem 2.1 is complete.

Neighbourhood theorem
In this section, we will study the set of admissible initial data and particularly its subsets generated by the classification in Theorem 2.1.We will hereafter fix r 0 > 0, and a given subset Y ⊂ I 0 we will write We also introduce the following notation, which slightly differs from the categorization in Theorem 2.1, but it will turn out to be more convenient throughout this section.Definition 3.1.We define the following subsets of I 0 : ⋄ For the singular orbits, i.e. those with r → 0 and N → −∞ at some finite ρ, we define the subsets (denoting by n the number of zeros of w for ρ > 0): ⋄ E n as the set of escaping singular orbits, for which w escapes the strip |w| ≤ 1. ⋄ C n as the set of crashing singular orbits, for which w stays in |w| ≤ 1.We also put C = ∞ n=0 C n .⋄ O as the set of oscillatory orbits, defined for all ρ > 0 with (w, ẇ) → (0, 0).⋄ R n as the set of regular orbits, defined for all ρ > 0 with (|w|, ẇ) → (1, 0), and such that w has n zeros for ρ > 0.
By Theorem 2.1, we see that the sets R n , E n , C , O form a disjoint partition of I 0 .We also observe that all orbits in R n are asymptotically flat.For orbits in O(r 0 ), we have that: ⋄ if r 0 > 1, then w ≡ 0 and the orbit is asymptotically flat, ⋄ if r 0 = 1, then w ≡ 0 and the orbit is asymptotically cylindrical, ⋄ if r 0 < 1, then w ̸ ≡ 0 and the orbit is asymptotically cylindrical.Finally, we note that C (r 0 ) = ∅ for r 0 ≥ 1, cf.Lemma 2.8.
Our current goal is to show the following result, which tells us how the orbits near a given orbit type behave.Theorem 3.2 (Neighbourhood theorem).Fix r 0 > 0 and let x 0 = (w 0 , U 0 ) ∈ I 0 (r 0 ).Define the slices and δ > 0 is sufficiently small, we have If we also have w 0 ̸ = 0, then (ii) If x 0 ∈ O(r 0 ), then for any n ≥ 0 we can choose δ > 0 so small that the y 0 -orbit has at least n zeros of w for ρ > 0, whenever 0

If we also have w
Remark 3.3.This result is an analogue of [9, Propositions 30 and 32] for the wormhole setting.Part (i) essentially says that C (r 0 ) and each E n (r 0 ) are open relative to the lines where either w 0 is fixed, or U 0 is fixed and w 0 ̸ = 0.In parts (ii) and (iii), one can actually get a stronger result.In fact, one can show that oscillatory and regular orbits are locally unique (cf.[9,Propositions 31 and 33]).This fact is, however, non-essential for the proofs in §5, nor does it improve the statements of the corresponding theorems, so we omit them. 3Finally, we would like to point out that the proof of part (iii) given in [9, Lemma 20] for their setting again invokes the theory of structurally stable vector fields, which we have already commented on in Remark 1.6.The proof given here naturally avoids this.Remark 3.4.Throughout the proofs in this section, we will repeatedly use some basic facts about ordinary differential equations.The solution flow depends continuously on the initial data (w 0 , U 0 ) ∈ I 0 (r 0 ), as we have already observed in Remark 1.2.Furthermore, classical results [23, Theorem 3.2] ensure that the maximal forward point of existence ρ > 0 of the solution is a lower-semicontinuous function of the initial data.This is important to us because we would like to compare the values of an orbit with its nearby orbits near the end of its existence.
Consider now an orbit with initial data x 0 = (w 0 , U 0 ) ∈ I 0 .The x 0 -orbit is either singular and hence defined up to some finite ρ ∞ , or it exists for all ρ ≥ 0. As already noted, we can choose δ > 0 so that the solutions with initial data y 0 such that |y 0 − x 0 | ≤ δ are defined up to any ρ < ρ ∞ in the former case, or up to ρ as large as we would like in the latter case.
By further shrinking δ > 0 if necessary, we can also ensure that the values of the dependent variables at ρ differ by no more than any given ε > 0, since the solutions depend continuously on the initial parameters.Moreover, if the x 0 -orbit is defined for all ρ ≥ 0 and a continuous function of its dependent variables, call it ξ, tends to some limit L, then we can for any ε, K > 0 find ρ > 0 (depending only on ε) so large and δ > 0 so small that ξ(ρ, y 0 ) differs from L by no more than ε on the interval ρ ≤ ρ ≤ ρ + K. Indeed, we can first choose ρ so large that |ξ(ρ, x 0 ) − L| ≤ ε/2 for ρ ≥ ρ, and δ small enough that orbits with initial data in {|y 0 − x 0 | ≤ δ} are defined at least up to ρ + K. Then ξ is continuous on the compact set so it is also uniformly continuous there.By shrinking δ further if necessary we then get |ξ(ρ, Finally, we note that if w(ρ, x 0 ) has (exactly) n zeros for 0 < ρ < ρ and w(ρ, x 0 ) ̸ = 0 (in particular w ̸ ≡ 0), then for sufficiently small δ and initial data y 0 with either y 0 ∈ U δ (r 0 , x 0 ), or y 0 ∈ W δ (r 0 , x 0 ) with w 0 ̸ = 0, the corresponding solution w(ρ, y 0 ) has (exactly) n zeros for 0 < ρ < ρ.To see this, let {ρ k | k = 1, . . ., n} be the n zeros of w(ρ, x 0 ) on 0 < ρ < ρ.If w 0 = 0 we also put ρ 0 = 0 and let k run from 0 to n instead.Then ẇ(ρ k , x 0 ) ̸ = 0 since otherwise we would have w ≡ 0 (cf.Remark 1.4), and we can by continuity find δ, γ > 0 so small that ẇ(ρ, for each k and all y 0 -orbits (note that γ can be chosen uniformly because k runs over a finite set).In particular, w(ρ, y 0 ) is strictly monotone in each I k .On the other hand, so it also has a positive minimum on K and we may select ε > 0 strictly smaller than this minimum.Then, finally, we shrink δ further if necessary to make |w(ρ, y 0 ) − w(ρ, x 0 )| < ε, which also ensures that, for each fixed y 0 , the corresponding ρ → w(ρ, y 0 ) has no zeros on K, and has exactly one zero in each I k by monotonicity and the intermediate value theorem (note that the zeros are no longer necessarily located at ρ k for the y 0 -orbits).This gives the claim if w 0 ̸ = 0. On the other hand, if w 0 = 0, then we note that the zero at ρ 0 = 0 stays located at ρ = 0 for the nearby y 0 -orbits, since we only consider y 0 ∈ U δ (r 0 , x 0 ) in this case, and consequently the number of zeros for ρ > 0 remains unaffected. 4roof of Theorem 3.2.Assume first that x 0 ∈ E n (r 0 ) \ {0} and choose δ > 0 so small and ρ so close to the singular point that (N + ζ)(ρ, y 0 ) < 0 and w(ρ, y 0 ) > 1, and w has exactly n zeros for the desired initial data y 0 ∈ U δ (r 0 , x 0 ) or y 0 ∈ W δ (r 0 , x 0 ) with w 0 ̸ = 0 (cf.Remark 3.4).All of the y 0 -orbits are then singular by Lemma 2.6, and w(ρ, y 0 ) cannot gain any more zeros for ρ > ρ because it stays in the region |w| > 1.It follows that y 0 ∈ E n (r 0 ).
An analogous argument can be applied when x 0 ∈ C (r 0 ) \ {0} to conclude that the nearby y 0 -orbits are singular (but in this case w(ρ, y 0 ) could gain zeros for ρ > ρ, which is why we refrain from counting them in the first place).Furthermore, the energy ( 15) is non-increasing for N ≤ −ζ and satisfies so w cannot cross the lines |w| = 1 in this region and consequently y 0 ∈ C (r 0 ) \ {0}.Now consider the oscillatory case (ii) of Theorem 3.2.If r 0 < 1, the x 0 -orbit has infinitely many zeros of w while w ̸ ≡ 0, so the result follows trivially by continuity with respect to initial data, cf.Remark 3.4 (alternatively, one can use a similar argument as in the case r 0 = 1 below, if one prefers).For r 0 ≥ 1, we first note that the orbits with initial data y 0 in the punctured ball 0 < |y 0 − x 0 | ≤ δ cannot be in O(r 0 ) or C (r 0 ), as follows from Theorem 2.1 and the fact that no orbit can crash for r 0 ≥ 1, cf.Lemma 2.8.To show that these have arbitrarily many zeros, we consider the polar angle of (w, ẇ) defined by and extended smoothly across zeros of w.Note that this is well-defined since the orbits starting in the punctured ball 0 < |y 0 − x 0 | ≤ δ cannot reach the fixed point (w, ẇ) = (0, 0).A simple calculation yields (cf.( The idea is to show that the right-hand side is sufficiently small on an arbitrarily large interval, which will imply arbitrarily many zeros of w.Note that: ⋄ If r 0 = 1, then necessarily x 0 = (1, 0, 0) and w ≡ 0, N ≡ 0, κ = tanh(ρ) → 1. ⋄ If r 0 > 1, then necessarily x 0 = (r 0 , 0, 0) and w ≡ 0, while κ → 1 and N → 1 since these orbits are asymptotically flat, cf.§2.1.Hence, in both cases we can for any K > 0 find ρ > 0 sufficiently large (independent of K) and δ > 0 so small that (cf.Remark 3.4) for ρ ≤ ρ ≤ ρ + K and all y 0 -orbits with |y 0 − x 0 | ≤ δ, where the first inequality holds with the minus sign for r 0 = 1, and with the plus sign for r 0 > 1.It therefore follows that θ(ρ, y 0 ) ≤ − 1   4   for ρ ≤ ρ ≤ ρ + K and |y 0 − x 0 | ≤ δ, implying that But the right-hand side can be made arbitrarily (negatively) large, which implies arbitrarily many zeros of w.Finally, we consider part (iii), so let x 0 ∈ R n (r 0 ) \ {0}.We first want to make sure that, for nearby orbits, N and κ stay near 1.Since E 0 is bounded on |y 0 − x 0 | ≤ δ, we see that for any given ε ≤ 1 and sufficiently large ρ depending on it, all orbits with initial data in |y 0 − x 0 | ≤ δ have E 0 (y 0 ) sech(ρ) ≤ 2ε and (κ + N )(ρ, y 0 ) ≤ 2(1 + ε) for all ρ ≥ ρ, where the latter inequality follows by the former and Lemma 2.3.Since the x 0 -orbit is asymptotically flat, it has r → ∞ and N → 1, so we may further increase ρ and shrink δ if necessary to ensure that 1 ε for all orbits with initial data in |y 0 − x 0 | ≤ δ.As long as N ≥ 0 and |w| ≤ 1, we then have r ≥ r(ρ, y 0 ) ≥ 1 ε , and equation (9b which shows that N increases in the region N < 1 + ε − 2 √ ε and in particular stays positive if ε is sufficiently small.There are two options, as long as |w| ≤ 1: Hence, for any ε > 0, we can choose ε small enough that for all ρ ≥ ρ as long as |w| ≤ 1, and all orbits with initial data y 0 in |y 0 − x 0 | ≤ δ, as desired. Since the x 0 -orbit has exactly n zeros of w and |w| → 1, we can again shrink δ and increase ρ to ensure that the y 0 -orbits such that either y 0 ∈ U δ (r 0 , x 0 ), or y 0 ∈ W δ (r 0 , x 0 ) with w 0 ̸ = 0, satisfy (1 − w(ρ, y 0 ) 2 ) 2 ≤ ε and have exactly n zeros of w for 0 < ρ < ρ, cf.Remark 3.4.The autonomous energy (16) satisfies In particular, this shows that F is non-decreasing for ε < 1/3, so for ρ ≥ ρ with |w| ≤ 1.Now there are three options for the y 0 -orbit (we omit y 0 as an argument henceforth), where we assume without loss of generality that w and ẇ are negative at ρ, in view of the symmetry (w, U ) → −(w, U ): (i) w continues decreasing but stays in the region |w| ≤ 1, hence the orbit is in R n (r 0 ), (ii) w continues decreasing and enters the region w < −1, hence the orbit is in E n (r 0 ), (iii) w decreases until it reaches a minimum at some point ρ 1 ≥ ρ, so ẇ(ρ 1 ) = 0 and −1 < w(ρ 1 ) < 0, and then turns back towards the region w > 0. To complete the proof of (iii), we thus need to show that w enters the region w > 1 in case (iii), so the orbit is in E n+1 (r 0 ).The argument below is, in essence, very similar to [17,Proposition 4.8].Define b > a ≥ ρ 1 as the first points such that w(a) = − 1 − √ ε and w(b) = 0.These are well-defined because ẇ increases and ẇ > 0 in the region w < 0 for ρ > ρ 1 by (9c), so w also increases uniformly in that region.Then for a ≤ ρ ≤ b, the right-hand side of ( 20) is non-negative, so we may take the square root and estimate for ρ ≥ b.The right-hand side depends continuously on ε and tends to 4 √ 2 3 as ε → 0. This implies that F is lower bounded by a positive constant for ρ ≥ b when ε is sufficiently small.Hence, the same is true for ẇ, implying thats w keeps increasing uniformly and eventually enters the region w > 1, as desired.□ Remark.We would like to point out that in [18, Proposition 3.5], the authors prove the analogue of part (ii), r 0 > 1, of Theorem 3.2 for their setting.However, their proof is much more involved, because they treat r as the independent variable, so they cannot use continuous dependence on initial data since the initial point for the x 0 -orbit is a singular point of the system in those coordinates.However, this singularity only appears as a consequence of using r as a coordinate, and in our system we do not face the same difficulties, so the proof is much simpler.

Energy theorem
Having studied neighbourhoods of different types of orbits, we also wish to understand how the extremal parts of the set I 0 look like.This can viewed as a compactness result, as it will provide us with appropriate upper and lower bounds for the shooting method.Theorem 4.1 (Energy theorem).Fix r 0 > 0, let (w 0 , U 0 ) ∈ I 0 (r 0 ) and Remark.In part (ii), the required magnitude of E 0 depends on r 0 .The heuristic idea behind part (ii) is that if the initial velocity ẇ0 of w is chosen large enough (this is in fact equivalent to chosing the initial energy E 0 large enough since r 0 is fixed), then w escapes the strip |w| ≤ 1.Even though this seeems intuitively obvious, the proof is surprisingly difficult.The first issue is that, a priori, the orbit could crash arbitrarily fast for large E 0 , before w escapes the strip |w| ≤ 1.The second difficulty is that, even if the orbit does not crash, equation (9d) implies that the larger E 0 is, the faster U decreases, so it could become negative arbitrarily fast, in particular if κ − N becomes large.The crux of the issue here is that we do not have a bound for κ that is uniform in E 0 (in particular, the bound from Lemma 2.3 is not good enough).
Proof of Theorem 4.1 (i).Let E 0 = 0 and recall that ζ 0 = √ E 0 = 0.By (9f), we then see that ζ ≡ 0. In view of this, Lemma 2.6 implies that the region N < 0 is invariant and the orbit is singular if it enters it.
, so that either N < 0 for ρ > 0, or else (r 0 , w 0 , U 0 ) = (1, 0, 0) ∈ O, cf.§2. 1.This shows that the non-trivial solutions with E 0 = 0 are singular, so it only remains to show that they crash rather than escape the strip |w| ≤ 1.But this follows immediately since |w 0 | < 1 (note that E 0 = 0 prohibits |w 0 | = 1), and w cannot cross the lines |w| = 1 in the region N ≤ −ζ ≡ 0, cf.(19).□ As already hinted, the proof of Theorem 4.1 (ii) is much more involved.We will need the following lemma, which allows us to control r uniformly for all choices of initial parameters with fixed r 0 .Lemma 4.2.Fix r 0 > 0. For each ε > 0, there exists a δ > 0 such that, for any solution of the initial value problem (9a-9f, 12) with respect to initial data x 0 = (w 0 , U 0 ) ∈ I 0 (r 0 ), we have Remark.The main point of the result is that δ can be chosen independently of (w 0 , U 0 ).Proof.By Lemma 2.3, we know that N ≤ 1, so we only need a lower bound that is uniform for (w 0 , U 0 ) ∈ I 0 (r 0 ).To this end, we compare the equations (9a, 9b) for (r, N ) with a simpler system.For r 0 < 1, consider the solution of the initial value problem5 ṙ = r N , r(0) = r 0 , and define (r, N ) = (r 0 , 0) if r 0 ≥ 1, solution of ( 21) if r 0 < 1.
In view of the symmetry (w, U ) → −(w, U ) and the fact that large E 0 necessitates large U 2 0 , we can without loss of generality assume that U 0 is positive (on the other hand, w 0 could be negative, but satisfies |w 0 | ≤ 1).We begin by observing that (9c) can equivalently be written as d dρ and an integration gives Observe that E 0 → ∞ if and only if U 0 → ∞ (since r 0 is fixed and |w 0 | ≤ 1), and so for sufficiently large E 0 , we have 1 2 ≤ U 0 /ζ 0 ≤ 1.Thus, using also the bounds (22), we can estimate the first term in (24) as for 0 ≤ ρ ≤ ρ.For the second term in (24), we note that rζ does not increase, since where we use the bounds (22) and also the assumption ρ ≤ δ < 1.It follows that, for 0 ≤ ρ ≤ ρ, where we also use the estimate (x + y) 2 ≤ 2(x 2 + y 2 ) to achieve the second inequality and again the bounds (22) for the first one.If we define ϕ(ρ) = ρ 0 ζ, then we see by integrating the first inequality in (25) that 6 Though these assumptions seem arbitrary at the moment, particularly the latter one, their significance will become apparent as we go along.
since |w| ≤ 1 and ρ ≤ δ < 1.On the other hand, since ζ = −κζ by (9f), we get d dρ where we also use the second inequality from (25).Since κ(0) = 0, an integration gives where the second step follows since ζ decreases, whereas in the last step we use (26) to obtain the positive constants a = 2 8 3 r0 , b = 1 + 16 r0 , both depending only on the fixed r 0 .Using ζ = −κζ again, we may then integrate to get and solving for ζ yields the lower bound By (25), w is monotone (at least) as long as r0 8 ζ − 4 > 0 (and 0 ≤ ρ ≤ ρ).By (27), this is achieved (at least) for where the limit is taken as E 0 → ∞.In particular, we see that w is monotone on 0 ≤ ρ ≤ ρ for sufficiently large E 0 , since ρ ≤ δ, and δ is less than half of the limit above, cf.(23).Integrating now (27) for the final time, we get But ϕ(ρ) is bounded as E 0 → ∞ by (26), so this inequality generates a contradiction unless ρ → 0, which in turn implies that ρ < δ for sufficiently large E 0 and completes the proof.□ Remark.The proof actually shows that the orbit escapes the strip |w| ≤ 1 arbitrarily fast as E 0 → ∞, just as one would intuitively expect.However, we do not need this fact so it is not a part of the statement of Theorem 4.1.

Construction of symmetric wormholes
Having performed the analysis of the previous two sections, we finally have all the ingredients to show the main existence result (Theorem A) of this manuscript.The theorem will follow by reflection using the symmetries discussed in Remark 1.4 and the following result.
Theorem 5.1.Fix r 0 > 0. For each n ≥ 0, there exist initial parameters has no analogue for the black hole nor particle-like setting.The final part of the theorem is not really relevant for the construction of wormholes, but it comes at virtually no additional cost.In any case, it is interesting to know that non-trivial oscillatory orbits exist for r 0 < 1, while w In Figure 1, we present a visualization of the set of admissible initial data, where either U 0 = 0 or w 0 = 0 are kept fixed.The reader can use these figures as a visualization guide throughout the proof.
Proof.We construct the sequences inductively.As in the statement, we will assume that for the even orbits (i.e.those with U 0 = 0), we have w 0 ≥ 0, and for the odd orbits (i.e.those with w 0 = 0), we have U 0 ≥ 0. This is possible due to the symmetry (w, U ) → −(w, U ).Note that the boundary condition E 0 = 0 of the set I 0 (r 0 ) of initial parameters can only be reached if r 0 ≤ 1.We set The idea is now to perform a shooting method along the lines W (r 0 ) = I (r 0 ) ∩ {w 0 ̸ = 0, U 0 = 0}, U (r 0 ) = I (r 0 ) ∩ {w 0 = 0, U 0 ̸ = 0}.
(but reflected) properties of its forward counterpart.In particular, for the (0, U (n) 0 )-orbit, w has 2n + 1 zeros (n on each half of the real line, and an additional one at ρ = 0), and w → ±(−1) n as ρ → ±∞.Now, for each n ≥ 0, set Since τ 0 is still free (cf.Remark 1.3), we can choose it so as to make τ (n) → 0 at ±∞, since rζ tends to some finite limit by Theorem 2.1.Then we see that these functions describe symmetric wormhole solutions, as desired in Theorem A. Finally, we note that for r 0 ≥ 1 the variable N has only a single zero located at ρ = 0 by Lemma 2.8, and this point describes a non-degenerate wormhole throat.On the other hand, when r 0 < 1 and n is even (resp.odd), then Ṅ0 > 0 (resp.Ṅ0 < 0) by (9b), so the initial point ρ = 0 describes a non-degenerate wormhole throat (resp.belly).□ Remark 5.2.Our results have the obvious weakness of not being able to specify the total number of zeros N has for r 0 < 1.One may hope to be able to control the number of zeros of N in the neighbourhood theorem and subsequently the shooting method in a similar way we control the number of zeros of w, but this is unfortunately not possible.The main culprit for this is the fact that nothing prohibits N from having double zeros, i.e. points such that N = 0 and Ṅ = 0.In particular, if an orbit has a double zeros of N , then for the nearby orbits this zero could bifurcate into several zeros, or even completely disappear.Even though we cannot prove this using our current techniques, the numerics indicate that the solutions with r 0 < 1 have exactly one non-degenerate throat for even n, and exactly two non-degenerate throats for odd n.Nevertheless, Lemma 2.10 ensures at the very least that N has only a finite zeros for the regular solutions, and in particular the wormhole solutions with r 0 < 1 have at most finitely many throats/bellies.

Asymmetric wormholes
In [20, §4], it was proposed that it might be interesting to study also asymmetric solutions, i.e. those not possessing the symmetry ρ → −ρ.In fact, our numerical analysis suggests that there exist such wormhole solutions, having n zeros of w for ρ > 0 and m zeros for ρ ≤ 0. In Table 1, we list our numerical findings of initial data describing such solutions.We also plot the corresponding solutions for certain choices of n and m in Figure 2. Figure 2. Asymmetric wormhole solutions for r 0 = 0.75.Plotted using the initial data given in Table 1.The plots of the other dependent variables are not particularly inspiring so they are omitted.
In view of this, we conjecture the following asymmetric extension of Theorem A.
Remark.Note that the even (resp.odd) solutions obtained in Theorem A would in this notation have n = m (resp.m = n + 1), which is why our numerical results only display asymmetric solutions with m − n ≥ 2.
Let us present also some analytical details that could be used to prove Conjecture 6.1.First, we note that Theorem 5.1 can in fact easily be extended.(w 0 ) (dotted), for r 0 = 0.75.Every intersection between a solid and a dashed curve represents initial data describing a wormhole.The intersections with w 0 = 0 are precisely the odd solutions from Theorem A. a given number of zeros (with r 0 and either w 0 or U 0 fixed), cf.[9, end of §8] and Remark 3.3.We therefore leave the statement merely as a conjecture.
To end the asymmetric discussion, we would also like to recall that we have assumed the initial value κ(0) = 0 throughout the manuscript.This is, however, not a necessary condition, and κ(0) could be chosen freely.One should be careful in doing so, because that would require a modification of the proof of the classification given in Theorem 2.1.Note also that such wormholes would necessarily be asymmetric, so that one should probably first have a good understanding of how these can be constructed for the simpler case κ(0) = 0. 7. Declarations 7.1.Acknowledgements.The author would like to express his gratitute to his PhD advisor, Anna Siffert, for suggesting the problem and for the helpful discussions surrounding it.Many thanks also to Gustav Holzegel for suggesting improvements to the text as well as certain results.7.2.Funding.While working on this project, the author was funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany's Excellence Strategy EXC 2044-390685587, Mathematics Münster: Dynamics-Geometry-Structure.At the time of publishing, the author is funded by the Österreichischer Wissenschaftfonds (FWF) within the project P 36862.The author is grateful to both sources of funding.

Figure 1 .
Figure 1.A (qualitative) visualization of the set I 0 of admissible initial data with U 0 = 0 (left) and w 0 = 0 (right).The thick solid lines represent the set where E 0 = 0, the dashed lines represent the set of oscillatory orbits O, and the thin solid lines represent the regular orbits R n .

7. 3 . 7 . 4 .
Data availability.The numerical data used for the plots in §6 can be obtained through DOI: 10.48550/arXiv.2310.14367or by contacting the author.Conflicts of interest.The author has no conflicts of interest.