Lorentzian Vacuum Transitions in Ho\v{r}ava-Lifshitz Gravity

The vacuum transition probabilities for a Friedmann-Lema\^itre-Robertson-Walker universe with positive curvature in Ho\v{r}ava-Lifshitz gravity in the presence of a scalar field potential in the Wentzel-Kramers-Brillouin approximation are studied. We use a general procedure to compute such transition probabilities using a Hamiltonian approach to the Wheeler-DeWitt equation presented in a previous work. We consider two situations of scalar fields, one in which the scalar field depends on all the spacetime variables and other in which the scalar field depends only on the time variable. In both cases analytic expressions for the vacuum transition probabilities are obtained and the infrared and ultraviolet limits are discussed for comparison with the result obtained by using general relativity. For the case in which the scalar field depends on all spacetime variables we obtain that in the infrared limit it is possible to obtain a similar behavior as in general relativity, however in the ultraviolet limit the behavior found is completely opposite. Some few comments about possible phenomenological implications of our results are given. One of them is a plausible resolution of the initial singularity. On the other hand for the case in which the scalar field depends only on the time variable, the behavior coincides with that of general relativity in both limits, although in the intermediate region the probability is slightly altered.


Introduction
The quantum theory of the gravitational phenomena, or quantum gravity, is a theory in construction which is necessary in order to shed light about the quantum effects of gravitational systems. Among the problems that require the uses of quantum gravity is the study of the microscopic origin of thermodynamic properties of black holes and those describing some cosmological phenomena in the very early universe. Another important problem is the study of the vacuum decay and the transition between vacua at early stages of the evolution of the universe. Euclidean methods have been proposed in order to compute this transition probability by using the path integral approach [1,2,3]. One of the salient features of this approach is the prediction of transitions between open universes [3]. Later an alternative procedure to compute these transitions using the Hamiltonian approach was developed [4,5]. This method incorporates the Arnowitt, Deser and Misner (ADM) Hamiltonian formalism of general relativity (GR) [6,7,8]. The vacuum is implemented through a cosmological constant which is interpreted as the vacuum energy and the transition are carried out through a bubble nucleation [9]. In this approach the transitions between Minkowski and de Sitter spaces are allowed. Very recently approach [4,5] was further developed by Cespedes et al. [10], where the vacuum is implemented by the minima of a potential of a scalar field in the curved space. In this reference it was computed the general vacuum decay transitions in the Hamiltonian formalism in Wheeler's superspace and some examples were implemented in the minisuperspace formalism for the Friedmann-Lemaître-Robertson-Walker (FLRW) cosmology. In this kind of models it was shown that the transitions between closed universes are allowed contrary to the Euclidean approximation of Coleman and De Luccia [3]. Later the formalism of [10] was extended and used to obtain the vacuum decay transition probabilities for some examples of transitions between anisotropic universes [11].
On the other hand it is well known that GR is not a renormalizable theory. Thus its application to very small distances as those associated to the early universe is expected to fail. Instead of that an important proposal to describe quantum effects of gravity is the Hořava-Lifshitz (HL) theory [12] (for some recent reviews, see [13,14,15,16] and references therein). Hořava-Lifshitz theory is a theory with an anisotropic scaling of spacetime and consequently it is not Lorentz invariant at high energies (ultraviolet (UV)). However it is a well behaved description at small distances due to the incorporation of higher order derivative terms in the spatial components of the curvature to the usual Einstein-Hilbert action giving rise to a ghost-free theory. Thus this theory is more appropriate to describe the quantum effects of the gravitational field, as the vacuum decay processes in the early stages of the universe evolution.
It is important to remark that HL theory is a theory whose low energy limit which connects with GR is troublesome. The parameters of the theory are the critical exponent z and the foliation parameter λ. This last parameter is associated with a restricted foliation compatible with the Lifshitz scaling. In the low energy limit z → 1 the Lorentz invariance is recovered. In the infrared (IR) limit the z → 1 limit is accompanied of the limit λ → 1, where the full diffeomorphisms symmetry is recovered and consequently the usual foliation of the ADM formalism is regained. In addition the higher order derivative terms in the action have to be properly neglected in order to get the correct limit. As we mentioned before the GR limit is problematic since it remains an additional degree of freedom (in some cases interpreted as dark matter) which leads to a perturbative IR instability [14,16,17,18]. The non-projectable version of the HL theory has the possibility to remove this unphysical degree of freedom. Thus it represents an advantage over the projective theory. However in the case in which one is concern with the Wheeler-DeWitt (WDW) equation, both approaches give the same result. In consequence we will work with the projectable version. In order to deal with these infrared instabilities several alternative proposals has been presented such as in [19,20], the former one was tested against gravitational waves measurements [21].
Since HL theory represents an improvement over GR in the high energy regime, it is natural that quantum gravity aspects of the theory are of great interest. Indeed, canonical quantization of the theory has been extensively studied. For example, some of the papers describing solutions of Hořava-Lifshitz's gravity in quantum cosmology in the minisuperspace are [22,23,24,25,26,27,28].
As we mentioned before HL gravity is a UV completion of GR thus it is a more suitable arena where to study the vacuum transitions in the presence of a scalar field potential. This proposal will be carried out in the present article. In order to do that we use the Hamiltonian formalism of the HL theory, in particular the WDW equation will be discussed in this context following [10,11]. We will particularly focus on the closed FLRW universe and study two types of scalar fields. First, since the anisotropic scaling of spacetime variables is a key ingredient of HL theory, we will consider a scalar field which is allowed to depend on all spacetime coordinates. Lastly we will consider also a scalar field which only depends on the time variable as it is more usual on the cosmological models.
This work is organized as follows. In Section 2 we give a brief review of the general procedure presented in [11] to study vacuum transition probabilities between two minima of a scalar field potential in the minisuperpace following the formalism of [10]. We will show that this formalism implemented for GR in [10,11] is sufficient to study vacuum transitions in a more general theory as HL theory. Section 3 is devoted to obtain the WDW equation in the context of gravity coupled to matter. In Section 4 we study the vacuum transitions in HL gravity for the scalar field depending on all spacetime variables. The IR and UV limits for the transition probabilities are discussed and compared to the GR result. Then, in Section 5 we study the transition probabilities for the scalar field depending only on the time variable and we also compare the result to the GR one. Finally, in Section 6 we give our conclusions and final remarks.

Vacuum transitions for a scalar field
In this section we review the procedure to obtain a general expression for the transition probability between two minima of the potential of a scalar field by obtaining a semiclassical solution to the WDW equation using a WKB ansatz described in Ref. [11]. We follow closely the notation and conventions given in that reference. It is a remarkable point to see that this procedure is enough to implement theories more general than GR as the HL gravity.
We start by using the well known ADM-formulation of GR [6,7,8] and consider the Hamiltonian constraint expressed in the general form where we take the coordinates in Wheeler's superspace to be Φ M with M, N = 1, ..., n (which has in general an infinite number of dimensions). These variables are the components of the three-dimensional metric, the matter field variables, etc. and are denoted collectively as Φ. Their corresponding canonical momenta are π M and the inverse metric in such space is G M N . Finally, f [Φ] is a function that represents all other additional terms as the 3 R term and the potential terms of scalar field in the WDW equation. The general WDW equation that we are going to consider is obtained after carrying out the standard canonical quantization procedure of the Hamiltonian constraint. Thus performing this procedure we get where Ψ[Φ] represents the wave functional which depends on all fields of the theory. We are interested in obtaining a semi-classical result, therefore following [10,11] we consider an ansatz of the following WKB form Ψ[Φ] = exp i S[Φ] , where S has an expansion in in the usual form Inserting Eq. (3) into Eq. (2) and focusing only on the term at the lowest order in we obtain On a certain slice of the space of fields a set of integral curves can be specified in the form where s is the parameter of these curves. The classical action appearing in the previous equation has the form It is easy to see that Eqs. (4) and (5) leads to where G M N satisfies the standard relation G P M G M N = δ N P . We note that we have a system of equations for the n + 1 variables: dΦ M ds , C 2 (s) defined by (5) and (7). Thus we can obtain a solution for such a system and then substitute the results back into Eq. (6) to obtain the classical action. Thus, in principle, we have enough information to compute the classical action, and consequently the wave functional to first order in regardless of the number of fields in superspace.
Under the ansatz that all the fields Φ M on the superspace depend only on the time variable, we can obtain a general solution to the system in terms of the volume Vol(X) of the spatial slice X of the form In this article we will consider gravity coupled to a scalar field provided of a potential which have at least a false and a true minima. Moreover we will study wave functionals such that the scalar field produces a transition between two minima of the potential.
One can use these wave functionals in order to compute the transition probability with the standard interpretation that these transitions are due to a tunneling between the two minima of the potential involved in the transition. In order to be more precise, in the semi-classical approximation the probability to produce a transition between two vacua at φ A and φ B is the decay rate which can be written as where ϕ I denotes all other fields defined on the superspace except the scalar field, Ψ(ϕ I 0 , φ B , ϕ I m , φ A ) is the wave functional associated to the path which starts in ϕ I (s = 0) = ϕ I 0 , and where the scalar field takes the value φ B . Moreover the path ends in ϕ I (s = s M ) = ϕ I m , where the scalar field is denoted by φ A . Furthermore β and χ are the constants of the linear superposition. In the previous equation we will consider just the dominant contribution of the exponential terms. Then in the WKB approximation at first order Γ yields where the choice of the signs ± indicates the dominant terms in the expression (10). Thus we finally arrive at the transition probability given by It is worth mentioning that the formalism developed in [10,11], originally for GR, is general enough to include other gravitational theories, since it only depends on a Hamiltonian constraint written in the general form (1). In the next sections we will show that it can perfectly include higher derivative generalizations of GR as the HL theory. It would be interesting to study at what extent this formalism can be used for more general theories.

Wheeler-DeWitt equation for Hořava-Lifshitz gravity coupled to matter
In this section we will discuss the action in HL theory as well as the action that consider the coupling to a scalar field. We will consider a metric describing a FLRW universe and a scalar field depending on the time variable as well as the spatial variables, and we will obtain the WDW equation for such a system. Although in the context of cosmology it is usual to use a time dependent field only, in this case we will allow the scalar field to depend also on the spatial variables since the anisotropic scaling of both sets of variables is a key ingredient for the theory. This type of dependence has been used previously in the context of cosmology for HL. For example it was used in Ref. [29] to study perturbations coming from a scalar field. However, for completeness and correspondence with the cosmological models, we will also study the case when the field will only depend on the time coordinate in Section 5. Let us begin by considering the gravitational part of the general action in projectable HL gravity without a cosmological constant and without detailed balance. This action can be written as [22,30,31] where N is the lapse function, R ij the Ricci tensor with i, j = 1, 2, 3 the spatial indices, R the Ricci scalar, K ij the extrinsic curvature, M p the Planck mass, D denotes covariant derivative with respect to the three-metric h ij and h denotes its determinant, all g n (n = 2, ..., 8) are positive dimensionless running coupling constants and the parameter λ runs under the renormalization group flow. GR is in principle obtained in the limit λ → 1 and g n → 0. However this is not actually fulfilled because of the perturbative IR instability and the presence of an unphysical degree of freedom as mentioned in the introduction.
Let us take the FLRW metric with positive curvature that describes a closed homogeneous and isotropic universe. This metric is written as where as usual 0 ≤ r ≤ π, 0 ≤ θ ≤ π and 0 ≤ ψ ≤ 2π. In the context of the ADM formalism, we note that for this metric and therefore we will work with a projectable version of HL gravity. Substituting these values in the action (13) we obtain that for this metric the gravitational action reads where a dot stands for the derivative with respect to the time variable. The integral for the spatial slice has been performed, that is In order to couple a scalar field φ(t, x i ) (where x i denotes collectively the three spatial variables) to this theory we need to consider actions that are compatible with the anisotropic scaling symmetries of the theory and UV renormalizability. In fact, the general scalar action in HL gravity is found to contain up to 6 order derivatives. This action is written in the form [32] where the function F (φ) is given by with ∆ denoting the three-metric laplacian and V (φ) is the potential for the scalar field. The constant c 1 is the velocity of light in the IR limit, whereas the two other constants are related to the energy scale M as There are three more possible terms that can be part of (19) constructed as products of derivatives, but we restrict ourselves to the terms just described.
Since the three-metric derived from the FLRW metric is just a scale factor times the metric of the three-sphere S 3 , we can use the spherical harmonic functions defined in this space to expand our scalar functions [33,34]. These functions can be defined in our spatial three-metric as eigenfunctions of the laplacian of the form where n is an integer. They obey the orthonormality condition Since these functions form a complete basis, we can expand any scalar function defined on the sphere in terms of them as Therefore, using this basis, we can expand the scalar field as where the fields φ nlm (t) are real functions depending only on the time variable. We can also expand the scalar field potential as where the funcions V nlm (t) depends on all the functions φ nlm (t) in general. Substituting (24) and (25) back into the action (18) we obtain that for the FLRW metric the field part of the action is written as where β n = n(n + 2) and are constants. Finally, by considering together both actions (16) and (26) we obtain that the full lagrangian describing HL gravity coupled to a scalar field is We have in this case that the degrees of freedom are the fields {a, φ nlm }. Their canonical momenta turn out to be and, as it is usual, the lapse function is non-dynamical since π N = 0. Therefore, we obtain that the Hamiltonian constraint takes the form

Vacuum transitions in Hořava-Lifshitz gravity
Now that we have obtained the Hamiltonian constraint of the HL gravity coupled to a scalar field depending on all spacetime variables, let us study the probability transition between two vacua of the scalar field potential. We note that the form of the Hamiltonian constraint (30) as obtained in the previous section is of the same general form as the one considered in (1) taking the coordinates on superspace to be {a, φ nlm }.
The inverse metric is given by where 1 nlm denotes a vector with length equal to all the possible values that the set {n, l, m} can have and with 1 in all its entries. In this case then we also have Therefore, the general procedure to obtain a solution of the WDW equation presented in Section 2 is applicable to the WDW equation obtained after quantizing the Hamiltonian constraint (30) in HL gravity. In order to study transitions between two vacua of a scalar field potential, we consider that all fields V nlm appearing in the expansion of the potential (25) have the same minima, namely one false minimum at φ A nlm and one true minimum at φ B nlm , and therefore, the two minima of the scalar field φ(t, x i ) comes only from its time dependence. Therefore, the transition probability in the semi-classical approach between these two minima is given by Eq. (12).
Following [11] we can choose the parameter s such that for the interval [0,s − δs], where s = 0 is the initial value, the field remains close to its value at the true minimum φ B , and for the interval [s + δs, s m ] the field remains very close to its value at the false minimum φ A , that is, we choose the parameter s such that But in this case, taking the expansion (24) and since the spherical harmonics are an orthonormal set, the latter implies that and similarly for the potentials Therefore, using the general form of the action (6) we obtain in this case and Consequently, the logarithm of the probability (11) is given in this case by We note that the last term of Eq. (38) can be written as with a potential defined by We note that this term has the same form as the one considered in Refs. [10,11] regarding the portion of the integral in which the scalar field can vary, therefore we can also interpret this term as a tension term taking Moreover, we note that the term that contains c 1 in (38) with Although this function has no minima in the points considered, it is a function of the scalar fields that can be interpreted as a new effective potential with the form of a mass term. Therefore, applying the same logic used in [11] to such terms, we can define a new contribution for the tension term as Similarly, we define for the two remaining terms and the two contributions to the tension terms as On the other hand, in order to do the two first integrals in (38) where all scalar fields are constants we use the general solutions (8) and (9), then after changing the integration variables from s to a according to ds = da where where we have defined the function and it is worth noting that in the above result the sign ambiguity on the left hand side comes from the arguments leading to Eq. (11) whereas the one on the right comes from the fact that the general solution (8) and (9) for the system of equations gives a solution for C 2 (s) wich produces a sign ambiguity in Eq. (48). Therefore both ambiguities are independent to each other.
As it is well known the IR limit of HL gravity for an FLRW metric is achieved in the limit λ → 1 and a >> 1, and corresponds to GR with an extra degree of freedom albeit with the instability problems mentioned in the introduction section. We note that the kinetic term for the scale factor in (28) is In the GR case considered in [11] it is given by because the 2π 2 term in that case is a global multiplicative factor to the full lagrangian and therefore it can be ignored. Thus, in order to obtain the same kinetic term in both cases in the limit λ → 1, we consider units such that 2π 2 M 2 p = 1. This choice of units will allow us to compare directly the transition probability to the one obtained in GR.
Then, we finally obtain for the logarithm of the transition probability We note that in contrast to the results obtained using GR for all the types of metrics considered in [11] this transition probability is described by five parameters, and by extremizing the latter with respect toā we can at most reduce them by one. It is also important to note that the above integrals cannot be done explicitly for any values of the α i constants. Nonetheless, it is an expression valid for any value of the potentials and interestingly it is a general expression that does not depend on having to consider the different modes contributing to the expansion in Eq. (24) separately.
As it is explained in [10,11] the choice of s as in (33) is useful to obtain exact solutions for the transition probabilities that leads to the same solutions as the ones obtained using euclidean methods. But there is also room to consider s in different ways. For example, we can also choose s as the distance in field space. This choice allows us to show that we can have classical transitions just because the metric in superspace for the WDW equation considered here coming from the Hamiltonian constraint (30) is non-positive definite, as is the case for all the metrics considered in [11]. Now that we have computed the transition probability for HL gravity in general, let us consider its two limits of importance, namely, the infrared and the ultraviolet limit. The first enable us to compare directly with the result found by using GR and the latter allows us to highlight the contributions for high energies that marks the importance of HL gravity.
Taking the IR limit of (54), that is, taking λ → 1 and a >> 1, we obtain Therefore, we find in the infrared an expression quite similar to the GR result plus one degree of freedom extra coming from the c 1 term in the action for the scalar field (26) as expected. In order to compare directly our result to the result obtain for GR we can for the moment set c 1 = 0, then the last result simplifies to that is the same result obtained for GR in [10,11]. The only difference comes in the choice of a 0 , since for consistency of the integral approximation we have here that a 0 >> 1, therefore it cannot be chosen to be zero. Thus, the difference between this result and the GR one are only constants. We also note that the potential appearing in this expression is not the potential found originally in the scalar field action, rather it is an effective potential appearing after integration of the harmonic functions. Considering the thin wall limit δa → 0 and extremizing the above result with respect toā we obtain Then substituting it back into Eq. (57) and choosing the plus sign in the right-hand side we obtain Therefore, in this limit the transition probability is finally described in terms of just one parameter (considering a 0 as a constant). If we take a 0 = 0 in (57), consider the thin wall limit and rename V 0 → V and T 0 → T , we obtain the result found in [10,11] for GR then, extremizing we obtain Thus, finally the logarithm of the transition probability in GR is written in terms of just one parameter as 3 We can see from (61) that since V A > V B choosing the plus sign on the right hand side of (60) implies that T > 0 always. The same is true regarding T 0 . As we know from [10,11] this choice of sign allows us to obtain the results found using the euclidean approach in [35]. It can be proven that the right hand side of (62) is always positive and therefore, in order to have a well defined probability defined by (12) we choose the plus sign in the left hand side as well. We note however from (58) and (61) that in order to have a well defined tension we need the terms inside the square roots to be positive. If both potential minima are negative, we see that this is indeed satisfied for all values ofā. However, if at least one of the potential minima is positive, we see that the tension will only be well defined untilā is big enough, that is, in this case, the tension term is well defined and consequently the expressions (59) and (62) are valid only in an interval from 0 until an upper bound forā.
Let us study now the ultraviolet limit, this is found when a << 1. In this limit Eq. (54) simplifies to (63) We note however that since all g n are positive, and the V 3 function defined in (45) is also positive for both minima, the first term is purely imaginary. Therefore, it does not contribute to the transition probability at all and it can be ignored. Thus, we finally obtain in this limit However this expression does not have an extremal with respect toā. Then in this case the probability is described by three independent parameters. For consistency with the GR result we will choose the plus sign in the left hand side of the latter equation, therefore, we note that in order to have a well defined probability we need the overall sign of the right hand side to be positive. Thus, we can choose both T 2 and T 3 to take always positive values. We can see from the GR result (60), or after extremizing (62), that in any case P (A → B) → 1 whenā → 0,. However for the UV limit of HL presented in (64) we have in the contrary P (A → B) → 0 whenā → 0 and then the probability increases as a increases. Therefore in this case the UV behaviour is completely different for both theories. Now that we have studied the two limits of interest. We proceed to compare the full result for the transition probability valid for allā (54) to the GR result. As we have said, for consistency with GR we are going to choose the plus sign in the left hand side and the minus sign in the right and use the thin wall limit, therefore we will consider If we want to vary (65) we will obtain an expression involving the tension terms and the functions F (α A,B 1 , α A,B 2 , α A,B 3 , V A,B ,ā). However, since those functions are defined on terms of square roots we need the terms inside to be non-negative in order to have well defined tension terms, that is we need that at all for any value ofā and in that case (65) would not have an extremal. In any case, we see that the extremizing procedure is very dependent on the many parameters of the theory and does not allow us to obtain well defined tension terms in general, in particular we never have access to the UV region. Therefore, in order to avoid these difficulties we are going to compare the results obtained before the extremizing procedure takes place, that is we will use for the comparison the GR result (60) choosing the signs already mentioned and the HL result (65). Since the HL expression depends on many independent parameters and the integrals cannot be made for any values of the constants involved, we are going to evaluate numerically this expression. Since in the IR limit we saw that after extremizing T 0 and T are always positive, we are going to take positive values for these parameters. On the other hand, in the UV limit we saw that we can take T 2 and T 3 also to be positive. Finally in order to obtain a well defined probability, we are also going to choose positive values for the remaining free parameter T 1 . Thus, we will take positive values for all the tension terms. In Figure 1 we show a plot of the transition probabilities coming from the two theories. We choose units such that 24π 2 = 1. For the GR result (blue line) we choose V A = 1, V B = 0.1 and T = 2. We note that in this case the first term in (60) is negative, therefore, we need to choose a value for T great enough to obtain a well defined probability. We see the behaviour outlined earlier, that is, the probability goes to 1 in the limitā → 0 and then it decreases asā increases going to zero. For the HL plots we choose , T 0 = 2 and c 1 T 1 = c 2 T 2 = c 3 T 3 = 1, we plot the probability for three different values of λ to see how this parameter affects the behavior. In this case we choose a 0 = 0.000001 in order to compute the integral numerically, however, we know from the UV analysis, that a 0 = 0 can be chosen without any problem and the general form will be unaltered. In this case, we also have that the first term in (65) is negative and increases with λ, therefore, we also need to make sure that the tensions chosen are big enough to have a well defined probability. This figure shows the behavior that we described earlier by studying the different limits of interest. That is, in the IR region the probability falls in the same manner as the GR result. We note thatā has to be big enough so the first term can be positive and then contribute to the probability, therefore, the different values of λ only affects the curve in the IR region and as λ increases, the probability increases since this term have the opposite sign that the tension terms. In the UV region the parameter λ has no impact at all and then, everything is defined by the tension terms. As we have said earlier, the probability goes to 0 asā → 0 and then it increases withā. We note that this behavior comes from the c 2 and c 3 terms, that is, it comes from the extra terms in the action for the scalar field (18) and it can be interpreted as the fact that HL avoids the singularity and predicts these type of transitions to occur in a UV regime (smallā) but not too close to the singularity. Then the probability starts to decrease and then it goes into the IR behavior just described. We note that the general form of the plot will be maintained regardless of the values of the parameters, we only have to make sure that they are chosen in a way that the tension terms dominates so we can have a well defined probability. However, specific things as the maximum height or the point in which both plots match is completely determined by the parameters and therefore, we cannot say something about them in general.

Figure 1: Transition probability in units such that
for GR (blue line) and HL with a scalar field depending on all spacetime variables with λ = 0.5 (red line), λ = 1 (green line) and λ = 2 (yellow line). For HL we choose a 0 = 0.000001 but the same form is expected for a 0 = 0.
In the present section we have obtained a general formula (65) for the transition probability when the scalar field depends on all spacetime variables. The integrals involved cannot be done in an analytic form however a numerical computation was performed and we showed a plot comparing the results with the one coming from GR. As we pointed out earlier the UV behavior is found to be completely opposite. This result depends on the extra terms in the action for the scalar fields, however these terms are only present if we take a field that depends on the spatial variables. Therefore, in the next section we are going to study a scalar field depending only on the time variable.
Phenomenological remarks Before we end this section let us discuss some phenomenological aspects regarding our results. The theory of Hořava-Lifshitz has received a lot of attention and much work has been done since its first proposal from the theoretical as well as the phenomenological point of view. For example in [36,37,38] the viability of the different versions of the theory have been tested against various experimental (or observational) data sets coming from different sources such as CMB and BAO collaborations. It is found that the theory is in good agreement with such data and therefore it supports the importance of considering it as a viable theory. It is also interesting to point out that in these works they always work with an FLRW metric with a non-zero curvature since the flat metric gives the same predictions as in General Relativity. Thus the importance of studying such metrics as the one we studied in the present article is also supported by these works.
On the other hand, in the vacuum decay process studied by using the euclidean method, discussed in [3], the process is described by the nucleation of true vacuum bubbles and its corresponding expansion. This could lead to phenomenological predictions regarding this kind of phase transitions occurring at some point in the evolution of the universe. However, as it was pointed out in [10] the process studied by using a Hamiltonian approach in the minisuperspace is limited. In fact, in the transition studied there is no notion of bubble nucleation, we can only compare two configurations of three-metrics and then interpret its ratio as a transition probability. Therefore, it is speculated that this formalism is not describing the same process as the euclidean method. It is believed that it may describe a generalization of the tunneling from nothing scenario, that is, we are obtaining probability distributions of creating universes from a tunneling event between two minima of the scalar potential. If we take seriously this interpretation then the scale factorā appearing in the expression found for the transition probability would correspond to the value that the scale factor of the created universe would have at the time of creation (its corresponding 'size'). Then, the plot in Figure 1 would tell us that in Hořava-Lifshitz gravity, in the case in which the scalar field depends on the spatial variables, the universe would be created with a scalar factor different from zero and therefore we would avoid the singularity contrary to GR which predicts a singularity at the beginning of the universe. This of course would have potential phenomenological consequences in the physics of the early universe and its corresponding evolution. Therefore, although we are in an speculating phase this kind of transitions are worth studying with more detail.

Transitions for a time dependent scalar field
In the previous sections we studied a scalar field depending on all coordinates of spacetime and found a transition probability whose behavior differs completely in the UV regime comparing to the GR result. However, in cosmology it is more common to study a scalar field depending only on the time variable as it is the case in [32,39,40]. Therefore, in this section we will consider such a dependence for the scalar field and study the vacuum transition probability between two minima of the potential. In this case, the scalar field action (18) reduces to where we have redefined the scalar field potential appearing in (19) as V 2 → V so it coincides with the usual scalar potential in the action. Since now we have a global factor of 2π 2 as in the action of the gravitational part (16), we can omit this factor. Then, the lagrangian this time is given by Therefore we have only two degrees of freedom a and φ, their canonical momenta are and the Hamiltonian constraint takes the form Comparing this last expression to the general form considered in Eq. (1), we note that in this case the coordinates in superspace are {a, φ} with inverse metric and we also have In order to study transitions between two minima of the potential, we choose the parameter s as in expression (33), then following a similar procedure as in the previous section we obtain in this case that choosing units such that M p = 1 (as in the GR case) and in the thin wall limit the logarithm of the transition probability is written as whereᾱ 2 = 6(3g 2 + g 3 ),ᾱ 3 = 12(9g 4 + 3g 5 + g 6 ), the function F is defined in (51) and as we have mentioned in Section 4 the sign ambiguities in the last expression are independent. Now that we have computed the transition probability in general, we move on to study its behavior in the limiting cases considered before. For the IR behavior we consider λ → 1 and a >> 1 in the above expression, the result is the same as in (57) with the same subtlety about a 0 as discussed in the previous section. On the other hand in the UV limit we have a << 1. However in this limit we obtain Γ → 0 as a → 0. Therefore, we note that the general behavior of these results is the same as the GR result in both extreme cases. In fact, we can variate (73) with respect toā to obtain Substituting it back in (73) we obtain finally Thus, the transition probability is also written in terms of just one parameter as in the GR result. Therefore, the only difference between GR and HL in this case is that the transition probability changes by acquiring two more terms in the square root before integration making the integral not possible to be performed in general and a global factor depending on λ in (76). The qualitative behavior in both the IR and UV limit is unaltered. In order to compare the result of this section with that of GR in general, not only on the limiting cases, we note that as in the last section the extremizing procedure leading to Eq. (75) gives rise to some restrictions for the validity of (76). In particular, it is never well defined whenā is small. Therefore, we are going to use the result (73) and choose the minus sign in the right hand side so in the IR limit it coincides with the GR result and on the left hand side we will choose the plus sign in accordance with the GR result as well. We will compare it with the GR result (60) with the sign choices made in the above section. In both cases we will take the tension T as an independent positive parameter and take values big enough so we can have a well defined probability and compute the integrals numerically. In Figure 2 we show such comparison. We choose units such that 24π 2 = 1, with V A = −1, V B = −10,ᾱ 2 =ᾱ 3 = 5 and T = 5. For the HL result we show plots for three values of λ and choose a 0 = 0.000001 in order to perform a numerical computation of the integrals, however doing the UV limit we note that a 0 = 0 is possible and it has the same behavior. This figure shows the limiting behavior that we described earlier, that is, in the IR and in the UV limits all curves behaves in the same way, it is in the middle region where their behavior is modified. In particular we note that in the beginning the HL probability is smaller than the one of GR and the contribution of the λ parameter is not noticeable, however when the first term in (73) is big enough, the contribution of the first term is big enough to separate the curves, and as in the case considered in the previous section, as λ increases the probability increases. Finally, the three probabilities fall as in the GR case.

Final Remarks
In the present article we have studied the transition probabilities for an FLRW metric in Hořava-Lifhitz gravity using a WKB approximation to the WDW equation. The general procedure proposed in [10,11] was found to be applicable to this case. We used HL theory without detailed balance and consider an FLRW metric with positive spatial curvature.
We considered two types of scalar fields. First, since the anisotropic scaling between space and time variables is a key ingredient of HL theory, we considered a scalar field which depends on all spacetime variables. This type of dependence is useful to study cosmological perturbations coming from scalar fields [29]. On the other hand, since in cosmology it is customary to propose an ansatz in which the scalar field depends only on the time variable, we studied this kind of dependence as well. For both cases we found analytic expressions for the logarithm of the transition probabilities in the thin wall limit.
For the scalar field depending on all spacetime variables the transition probability (65) was found to depend on five different parameters coming from the new terms present in the action for gravity as well as the action from the scalar field in HL theory. There is only the possibility to reduce just one of these parameters after an extremizing procedure but such procedure is not well defined for all values of the scale factor. Taking the IR limit we found that one degree of freedom extra coming from the scalar field action survives, which is a common issue regarding the IR limit of HL theory. However, if we ignore this contribution, we can obtain a expression that differs from the GR result just by constants. In the opposite limit, that is, in the UV limit we found that the probability is described in terms of three independent parameters and it vanishes in the limitā → 0. This is opposite to the GR result in which the probability goes to 1 in that limit. We interpret this result as a way in which HL theory avoids the spatial singularity atā = 0 and predicts these transitions to occur on the UV regime but away from the singularity. We note that this behavior comes from the terms in the scalar field action with spatial derivatives and therefore, it is only possible in the case in which the scalar field depends on the spatial variables. In order to visualize these behaviors we plotted the transition probabilities coming from GR and HL theory. Such plots were presented in Figure 1. For the HL results the integrals involved were done numerically and we saw that in all cases the probability begins at zero withā = 0, then it increases withā until at some point it starts to decrease and then it behaves as in the GR case. We noted that the first behavior in the UV region is independent of the λ parameter and it is only on the IR where the dependence on this parameter is noticeable making the probability increase as λ increases.
For the scalar field depending only on the time variable the logarithm of the transition probability found have the same number of independent parameters as the GR result, that is, after extremizing we only have one parameter left. However, it also has dependence on the many constants g n appearing in the extra terms in the gravity action for HL theory as well as in the parameter λ. The behavior of the probability in this case is found to be the same as the GR result in both the IR as well as the UV limits. In fact, in the IR limit we obtain the same expression as the one coming from the scalar field with dependence in all spacetime variables when we ignore the degree of freedom that survives this limit and in the UV regime we also have that the probability goes to 1 in the limitā → 0. Therefore, with a cosmological ansatz, the behavior in the UV regime found by using GR is unaltered. However in the intermediate region, the probability is of course modified. In order to visualize the difference in this region we plotted the transition probabilities coming from GR and HL theory and showed them in Figure 2. In this case we also carried out a numerical computation of the integrals involved in the HL result. We noted that at first the probability of HL is smaller than GR and the contribution from the λ parameter is not noticeable. However, when the scale factor is big enough this contribution is important and as in the latter case, the probability increases with λ. It is interesting to note that using HL theory instead of GR for a cosmological ansatz of the scalar field does not have a dramatic change on the transition probability at least at the semi-classical level we used in this article through the WKB approximation.
It is worth pointing out that we have used a WKB approximation and kept only up to first order in the expansion. However, this level of semi-classical approximation is sufficient to obtain the transition probabilities and we can safely explore the UV regime of both GR as well as HL theory, since the transition probabilities are well behaved functions in the UV. It was shown that in the case when the scalar field is only dependent on the cosmological time, GR and HL theories give very similar predictions in the WKB approximation. However, the case with a dependence on time and position coordinates for the scalar field, yields very different behavior from the GR case even in the WKB approximation. It would be interesting to work out higher order contributions from the WKB approximation, which presumably will have the contribution of quantum fluctuations.
It is important to remark as well that we considered closed universes in the HL theory and obtained well defined transition probabilities. Therefore, one of the important results obtained in Ref. [10] that asserts that this type of transitions can be carried out keeping the closeness of the spatial universe can certainly be extended to include the Hořava-Lifshitz theory of gravity as well.