The environment dependent dilaton in the laboratory and the solar system

We consider the environment-dependent dilaton in the laboratory and the solar system and derive approximate analytical solutions to the field theory equations of motion in the presence of a one or two mirror system or a sphere. The solutions obtained herein can be applied to qBOUNCE experiments, neutron interferometry and for the calculation of the dilaton field induced “Casimir force” in the Cannex experiment as well as for Lunar Laser Ranging. They are typical of the Damour–Polyakov screening mechanism whereby deviations from General Relativity are suppressed by a vanishingly small direct coupling of the dilaton to matter in dense environments. We specifically focus on dilaton models which are compatible with the late time acceleration of the expansion of the Universe, i.e. the cosmological dilaton. We show how future laboratory experiments will essentially test a region of parameter space with \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$A_2\simeq \lambda ^2$$\end{document}A2≃λ2 where \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$A_2$$\end{document}A2 is the quadratic coupling strength of the dilaton to matter and \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\lambda $$\end{document}λ is the steepness of the exponential runaway potential. Current constraints favour the large \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$A_2$$\end{document}A2 regime implying that the environment-dependent dilaton satisfies two of the swampland conjectures, i.e. the distance conjecture whereby the field excursion should not exceed the Planck scale and the de Sitter conjecture specifying that the running dilaton potential should be steep enough with a large \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\lambda $$\end{document}λ.


Introduction
The accelerated expansion of the Universe may require the introduction of additional degrees of freedom (see [1] for a recent review). Such new degrees of freedom, in particular light scalars, are theoretically well motivated irrespective of their role for the acceleration of the expansion of the Unia e-mail: philippe.brax@ipht.fr b e-mail: mario.pitschmann@tuwien.ac.at (corresponding author) verse. If they exist in Nature, they must either only be feebly coupling to other matter or appear in some screened form in order to prevent detection in all past experiments and observations involving scalar fifth forces. A number of screening mechanisms exist [1], the chameleon [2][3][4] and Damour-Polyakov mechanisms [5], the K-mouflage [6][7][8] and Vainshtein ones [9], allowing such hypothetical fields to remain unseen in local tests of gravity.
In the companion paper [10], gravity resonance spectroscopy [11,12], a Casimir force experiment [13] and Lunar Laser Ranging (LLR) [14] are used for the first time to put new bounds on the environment-dependent dilaton [15,16]. The LLR bounds have already been discussed for chameleon [17] and symmetron scalar fields [18]. The dilaton model conjugates two ingredients. First of all, it involves an exponentially decreasing potential as expected in the strong coupling limit of string theory [19][20][21] and second it is the simplest realisation of the least coupling principle as advocated in [5]. Hence this model is a prime example, with the symmetron, of a model subject to the Damour-Polyakov screening mechanism [22]. The experimental analysis in [10] depends heavily on the field profile of dilatons in both the one mirror or two mirror setups, where the field is either present over an infinite plane of high density or is confined between two such parallel planes. One of the purposes of this paper is to provide a detailed analysis of the environment-dependent dilaton in realistic situations which can be tested using current experiments. For instance the analysis of the LLR results as well as the screening of neutrons in Q-bounce experiments employ the dilaton solution around and inside a sphere as derived here. For a similar study applied to chameleon field theories see [23]. The symmetron field equations have been studied in a similar fashion in [24,25]. Testing screened models can be tackled from the laboratory to cosmological scales as reviewed in [26]. The parameter space of the environmentdependent dilaton has already been partially analysed in [15] where large values of A 2 , the quadratic coupling to matter, and λ, the steepness of the dilaton runaway potential, were favoured. In this paper, we provide the tools to analyse the parameter space of the environment-dependent dilaton in different contexts, in particular in laboratory experiments. As we shall see, the different experiments probe different length scales and therefore can test the dilatons with related mass scales. This is already what happens for the symmetrons [27].
The environment dependent dilaton is inspired by string theory in the strong coupling regime and therefore should satisfy the swampland conjectures [28]. This issue was considered in [29] from the cosmological point of view. Here we analyse the excursion of the dilaton in the laboratory and the solar system. We confirm that the field covers sub-Planckian distances. Moreover, the region of parameter space where the dilaton has an impact in the laboratory and the solar system is such that the de Sitter conjecture is satisfied. This guarantees that the dilaton runaway potential is steep enough. As a result, the experimental tests of the environment-dependent dilaton [10] will probe a theory which is not in the swampland.
In Sect. 2 we will provide some background information on dilatons, which will provide the relevant definitions for the field theory analysis. We consider a two-dimensional parameter subspace of the dilaton model, which is of special cosmological significance as noted in Sect. 3. Then, in Sect. 4 approximate solutions for the one mirror case will be derived, while in Sect. 5 the corresponding two mirror solutions will be given. In Sect. 6 approximate dilaton solutions are derived for a spherical source. Section 7 provides relevant information on the qBOUNCE experiment, where the dilaton-induced resonance frequency shift for the case of a single mirror has also been summarized for a large range of parameters. In Sect. 8 the induced pressure in Casimir experiments due to the dilaton field between two mirrors of the experimental setup is derived, while in Sect. 9 bounds due to LLR are given. A conclusion in Sect. 10 will be followed by Appendix A, in which the precession of the lunar perigee induced by fifth forces is obtained.

Background
Following [30], the dilaton potential is given by where V 0 is an energy scale related to the dark energy of the Universe and λ a numerical constant. This potential corresponds to the string theory dilaton potential in the strong coupling limit [5,20]. Together with the coupling to matter this induces an effective potential where for the environment-dependent dilaton we have [15] and hence Here, we have neglected an additional term ρ, which does not affect the equations of motion. The minimum value φ ρ in the presence of a density ρ is given by V eff,φ (φ; ρ) φ=φ ρ = 0 and reads with the Lambert W -function For large arguments the approximative relation holds: The mass μ ρ of the quantum fluctuation is therefore We employ the metric signature (+ − −−), for which the stress-energy tensor of a scalar field is while the equations of motion read in the presence of matter.
In the following, we will require that λ 1 to satisfy the de Sitter conjecture and check that the field excursion φ is always smaller than the Planck scale as requested by the swampland conjecture. We will find that these two requirements are satisfied in the interesting part of the dilaton parameter space where the models can be tested. In a nutshell, the distance conjecture will follow from the influence of the coupling to matter which forces the field to remain close to the origin in field space when matter is present.

The "Cosmological" dilaton
The parameter space of the dilaton model is 3-dimensional (V 0 , λ, A 2 ). Since we are interested only in "cosmological" dilatons, having significance in the cosmological domain, we consider only the 2-dimensional parameter subspace, for which where φ V , ρ V are the corresponding vacuum values and the density parameter 0 ∼ 0.73. This choice neglects the possible instability of the potential under radiative corrections. We take the parameter V 0 as a function of A 2 and λ such that Eq. (11) is obeyed. It is important to notice that the coupling function involves the strong coupling scale In the spirit of an effective field theory expansion of the coupling function, one must require that φ/M 1 to guarantee that terms of higher order in φ can be neglected. Similarly the exponential potential involves the scale = m Pl λ (13) and one must make sure that typically φ/ 1 to guarantee that higher order string corrections in e −nφ/ can be neglected. We will make sure that these conditions are satisfied in the following. As long as A 2 1 and λ 1, the previous conditions guarantee that the distance and de Sitter conjectures are valid.
It is straightforward to show that the condition (11) leads to The dilaton parameter space becomes effectively 2dimensional (λ, A 2 ) simplifying also the representation of experimental constraints. For illustrative purposes, in Fig. 1 the effective potential with its components is depicted for two different sets of parameter values for λ and A 2 .
Using Eq. (14) in Eq. (8) the mass μ ρ may be expressed as a function of the parameters λ and A 2 as well With these analytical expressions we can perform the limits A 2 → ∞, λ → ∞, A 2 → 0 or λ → 0 and study the behavior along curves λ ∝ √ A 2 , which all provide some qualitative insight of the relevant parameter region. This behavior is summarized in the following two Tables 1 and 2. Table 2 The limits of the two constituent parts of the effective potential Eq. (4) are summarized in this table We may summarize the findings of the tables as follows. For roughly λ ∝ √ A 2 we expect finite limits to be obtainable from experiments as long as λ is not too large since otherwise φ ρ decreases, i.e. the dilaton effectively disappears and the interaction range 1/μ ρ vanishes as well. For A 2 λ we expect no limits from experiments since φ ρ becomes small. On the other hand, for λ A 2 we also do not expect bounds since in this case either 1/μ ρ decreases without limit or φ ρ diverges and cannot act dynamically anymore. Hence, we find that the dilaton has a physical impact only within a restricted region in the A 2 , λ parameter space. Consequently, all experimental constraints have to lie within this region. As can be seen in Table 1, shorter interaction ranges correspond to larger values of A 2 and λ. Therefore, we expect LLR to probe small parameter values within this region, table top experiments correspondingly larger parameters and collider constraints still larger values. Numerical evaluations in the accompanying article [10] corroborate these findings. Notice that when λ = κ √ A 2 , the validity of the model as an effective field theory is guaranteed when κ 1 as the field values must satisfy φ M where = κ M M. These expectations are also confirmed by the actual bounds in [10].

One mirror
In this section, we treat the case of a single mirror filling the infinite half-space z ≤ 0. The 1-dimensional equation of motion reads (see Eq. (10)) Multiplication by φ and integration with respect to z gives with the integration constant z 0 and leads to where φ 0 = φ(z 0 ), the + sign is for φ ≥ 0, while the − sign holds for φ ≤ 0.

The vacuum region
First, we consider the case of low density ρ V corresponding to the medium above the mirror and search for a solution that asymptotically for z → ∞ goes as implying φ → 0. We find for z 0 = 0 and z → ∞ from Eq. (17) Using Eq. (20) in Eq. (18) gives Approximating the effective potential around its minimum at the vacuum value φ V , we find to leading order with the mass of the quantum fluctuation in vacuum Inverting the relation straightforwardly leads to

The high density region
Here, we consider the case of high density ρ M as inside the mirror. Clearly, for and hence φ → 0. Therefore, we find for z 0 = 0 and z → −∞ from Eq. (17) Using Eq. (27) in Eq. (18) gives Proceeding analogously to the case of vacuum, we finally obtain with the mass of the quantum fluctuation in the mirror

Boundary conditions
Using the boundary conditions we find The second boundary condition is trivially satisfied.
As already argued, we see in Fig. 2 that the field excursion is sub-Planckian. Moreover, these dilaton solutions are instrumental in analyzing the results of qBOUNCE experiments as outlined in Sect. 7.

Two mirrors
In this section, we treat the case of two parallel infinitely thick mirrors separated at distance 2d in z-direction with z = 0 being the center between the two mirrors.

The vacuum region
Here, we consider the case of low density ρ V , as between the mirrors and choose z 0 = 0. Due to the symmetry of the setup, the derivative of the field has to vanish there yielding for Eq. (18) where φ 0 = φ(0). Approximating the potential around φ 0 yields with the positive constants leads to Integration and some transformations lead to the solution

The high density region
We can read off the solution inside the mirrors directly from the corresponding solution in the one mirror case Eq. (34) where is the field value at the surfaces of the mirrors.

Boundary conditions
Using the boundary conditions at the mirror surface gives φ d as a function of φ 0 which together with the second boundary condition gives an equation, which defines φ 0 implicitly since D 0 and μ 0 both are functions of φ 0 .

Final solution
Summarising, we obtain the solution where φ d as a function of φ 0 is given by and φ 0 is solution to A prototype solution is plotted in Fig. 3. The induced pressure inside the planes is P = −4.73 × 10 −4 pN/cm 2 (see Sect. 7). Once again we see in Fig. 3 that the field excursion is sub-Planckian. These dilaton solutions will be use to evaluate the pressure in Casimir experiments.

Dilaton field of a sphere
In this section we consider the dilaton field as caused by a static massive sphere surrounded by vacuum with radius For a certain parameter regime this interaction between neutron and dilaton becomes strong. In this case, the neutron affects the background dilaton field as generated by the mirrors of the experimental setup in a non-negligible way, which in turn weakens the effect on the neutron, viz. screening of the neutron sets in (see also [31]). Since we treat the dilaton as a classical field theory, a consistent description of its coupling to a quantum mechanical system is beyond our reach. Therefore, we employ a semi-classical treatment in which the neutron's probability distribution times its mass acts as the source of the dilaton as defined in Eq. (81).
Concerning Lunar Laser Ranging, we approximate the Sun, Earth and Moon as spherical sources of dilatons with homogenous density and employ the solutions derived in this section.
The spherically symmetric field equation is given by with the boundary conditions Inside the sphere we have density ρ S . The corresponding minimum of the field value is We expand For the field equation we find Introducing the field ϕ Eq. (57) takes on the simpler form From the general solution for ϕ we obtain the particular solution for φ, which is convergent for r → 0 and satisfies the boundary condition φ (0) = 0: where C I is some constant to be determined later.
In the vacuum outside the sphere we approximate where μ V is given by Eq. (24). For the field equation we find With the field ϕ the field equation again simplifies to The general solution of which provides the φ solution convergent for r → ∞ and satisfying the boundary condition where C O is some constant to be determined next.
The dilaton field has to satisfy the following boundary conditions at the surface of the sphere which provides explicit expressions for C I and C O . After some elementary algebraical manipulations we obtain the relations In order to quantify the amount of "screening" of a sphere, we introduce a formfactor, which we interpret as a "screening charge" Q. The interaction of the sphere with its surrounding is given by its outer field. Clearly, with decreasing radius R the sphere becomes increasingly "unscreened" since the dilaton field inside the sphere decreases towards its minimum throughout the volume of the sphere. On the other hand, for large sphere radii the dilaton field reaches its minimum already before the center of the sphere, it is no longer "sourced" by the whole volume of the sphere, which becomes "screened". An unscreened sphere has R 1/μ S . Hence, we expand C O in powers of μ S R to obtain for an "unscreened" sphere We define the "screening charge" Q as the ratio With this definition, see Fig. 4, for "screened" bodies with μ S R → ∞ , 1 , for "unscreened" bodies with μ S R → 0 .
The acceleration experienced by a pointlike test body, which does not disturb the field, in the outer field of the sphere has been derived in [25] for a generic scalar φ in the nonrelativistic limit as In all models of consideration A(φ). Consequently, we find for the force on a particle caused by a scalar φ to leading order In the case of dilatons Eq. (3) holds and we finally obtain for the dilaton force on a point particle and, respectively, for the acceleration Asymptotically, for large r we obtain justifying the definition of Q as a "screening charge". The screening effects make the field excursion sub-Planckian as seen in Fig. 4. The dilaton solutions will be used for the results about the qBOUNCE experiment and Lunar Laser Ranging in the following sections.

Dilaton-induced frequency shift in qBOUNCE
Here, we derive a discrete set of limits for the qBOUNCE experiment [11, 12,32] using the solutions obtained herein. In this experiment, ultra-cold neutrons are dropped in Earth's gravitational potential and reflected by a neutron mirror, which has been reported for the first time in [33]. The energy eigenstates are discrete and allow to apply the method of resonance spectroscopy. In [12] the basic setup is described. In the Rabi version of the experiment, spectroscopy has been realized with energy resolution 3×10 −15 peV [27].
The experimental setup is such, that ultracold neutrons pass three regions, while being reflected on polished glass mirrors. In [27], the resonance spectroscopy transitions between the energy ground state E 1 = 1.41 peV and the excited states E 3 = 3.32 peV as well as E 4 = 4.08 peV have been demonstrated. First, the neutrons pass region I which acts as a state selector for the ground state |1 having energy E 1 . A polished mirror at the bottom and a rough absorbing scatterer on top at a height of about 20 μm serve to select the ground state. Neutrons in higher, unwanted states are scattered out of the system. This region has a length of 15 cm. Subsequently, in region II, a horizontal mirror performs harmonic oscillations with a tunable frequency ω, which drives the system into a coherent superposition of ground and excited states. The length of this region is 20 cm. Finally, region III is identical to the first region and hence acts again as a ground state selector.
The quantum mechanical description of a neutron above a mirror in the gravitational potential is given by the Schrödinger equation [34]. After separation into free transversal and bound vertical states it reads The characteristic length scale and energy scale E 0 = 3 h 2 m N g 2 /2 are given by the mass m N of the neutron and the acceleration of the Earth g. With the substitution Eq. (76) becomes Airy's equation From the effective dilaton potential we can deduce the semi-classical neutron-dilaton coupling There are some subtleties involved here of a nature similar as in the case of the symmetron. We refer to [24] for further information. The corresponding quantum mechanical perturbation potential is given by and leads to a resonance frequency shift to first order (see e.g. [35]): Likewise, the first order correction to the wavefunctions reads (see e.g. [35]) energies should be replaced as follows where Q is given in Eq. (69). The whole parameter space of dilatons can be efficiently constrained using the results obtained herein. The corresponding analysis has been carried out in parallel to this work [10], where the solutions obtained here for a one mirror setup are used to exclude regions of the dilaton parameter space. Nevertheless, in Table 3 we summarize the resonance frequency shift for a range of dilaton parameters near the experimental sensitivity in the case of a single mirror.
As can be seen in this table, the deviation can be larger than the experimental uncertainty of order 3 × 10 −15 eV for cases where for instance A 2 = 10 40 and λ = 10 30 corresponding to M 10 −2 GeV and 10 −3 eV, i.e. the dark energy scale. As a result the forthcoming results in [10] will test an interesting range of scales for both particle physics and cosmology.

Dilaton-induced pressure in CASIMIR experiments
Here, we consider limits that can be obtained by the Casimir And Non-Newtonian force EXperiment (Cannex) [13] (see also [37][38][39]). This experiment consists of two parallel plates in a vacuum chamber and has been devised to measure the Casimir force and hypothetical fifth forces. A dilaton field would induce a pressure between those plates, which can be measured with high precision.
We approximate the setup in one dimension along the zaxis as follows. Between the upper surface of the fixed lower mirror at z = 0 and the lower surface of the movable upper mirror at z = d there is vacuum. Then follows the upper mirror with thickness D and above that at z > d + D there is vacuum again. In order to obtain the induced pressure for the Cannex setup, we can apply the force induced on a point particle by dilatons in Eq. (71). We obtain Consequently, the pressure in z-direction is given by The corresponding integral is a surface term and hence trivially carried out with the final result This agrees with (see e.g. [25]) where T = g μν T μν and which reduces for a static field configuration of φ to In all models of consideration . For dilatons Eq. (3) holds and we finally obtain the dilaton-induced pressure For φ(d) we employ the value φ d at the mirror surface of the corresponding two mirror solution given in Eq. (50), while for φ(d + D) we can use the value φ 0 at the mirror surface of the one mirror solution given in Eq. (36) instead. Finally, we obtain for the pressure This results can be used to carry out a numerical analysis [10] where the exclusion regions of the dilaton parameter space are obtained from the Cannex experiment as we expect a sensitivity of |P z | ≤ 1 nPa.

Dilaton constraints by lunar laser ranging
In this section we analyze bounds on dilatons due to Lunar Laser Ranging (LLR), which provides three separate constraints [14] due to 1. the Nordvedt effect, which relates to a difference between the free fall acceleration of the Earth and Moon towards the Sun (equivalence principle violations), 2. deviations from the inverse-square law at distances comparable to the Earth-Moon separation and 3. time-variation of G.
Since the dilaton interaction is time-independent, it cannot induce a time-variation of the effective coupling G. Hence, only the first two constraints can lead to dilaton bounds and will be analyzed here.

Constraints due to the Nordvedt effect
For the first LLR test we consider the acceleration of the Earth ( ♁ ) and Moon ( ) towards the Sun ( ). For the Earth we find 74 where r AU is the vector pointing from Sun to Earth, a G is the acceleration due to the Sun's gravitational field and a φ ♁ the acceleration due to the dilaton field of the Sun and given by Eq. (74), which holds for a test particle in an outer field without screening. The screening of the Earth is taken into account by the second charge factor Q ♁ . Likewise, the acceleration of the Moon is given by where r AU is again the vector pointing from Sun to Earth, which is approximately the vector pointing from Sun to Moon. Then, a G is the acceleration due to the Sun's gravitational field and taken equal for Earth and Moon, such that any difference in acceleration between Earth and Moon, viz. an equivalence principle violation, is attributed to the dilaton field. For the equivalence principle violation quantified by the Eötvos parameter we find in the case of dilatons Typically this is constrained at the η em ≤ 2 × 10 −13 level by the LLR experiment [40].
9.2 Constraints due to deviations from the inverse-square law For the second LLR test we consider the precession of the lunar perigee caused by fifth forces. The corresponding Eq. (124) is derived in Appendix A and reads It is derived in Appendix A.
Here, δ f (R) is the acceleration caused by dilatons at the maximum Earth-Moon separation R, and given by 74 Using Eq. (101) in Eq. (100) leads to the central relation to be compared with experimental results of order 6 × 10 −12 .
The results of the numerical analysis for both tests are reproduced in the accompanying paper [10]. Typically the range of excluded values for A 2 and λ will be such that a region of parameter where A 2 10 10 will be excluded. More details will be given in [10].

Conclusion
We have derived approximate analytical solutions to the dilaton field theory in the presence of a one or two mirror system as well as for a sphere. The 1-dimensional equa-tions of motion have been integrated in each case. The analytical results obtained herein provide the necessary input for the numerical study carried out in parallel to this work [10]. The latter provides bounds on dilatons by using results from three "experiments". First, from qBOUNCE we obtain results by employing bouncing ultracold neutrons, second, Cannex provides bounds by measuring induced pressures between parallel plates and third, from Lunar Laser Ranging we obtain additional bounds in the astrophysical regime.
We have shown here that the dilaton models will be mostly tested in the region of parameter space where λ ∼ √ A 2 . The constant λ determines the steepness of the dilaton runaway potential whilst A 2 is the quadratic coupling constant to matter. Moreover, the different experiment will test different typical values of the parameter space. Solar system experiments such as Lunar Laser Ranging measuring the violation of the equivalence principle in the Sun-Earth-Moon system is mostly sensitive to values of A 2 ∼ 10 10 corresponding to masses of the dilaton in the solar system around 10 −23 eV, i.e. with an interaction range of the order of 100 astronomical units. Similarly laboratory experiments are sensitive to values of λ of the order of 10 30 corresponding to a mass which is typically around 10 −3 eV and a sub-millimeter range. The fact that the tests of the dilaton select an interaction range adapted to the typical size of the experiment is already what happens in the symmetron case [27]. Finally, all the dilaton models which can be tested experimentally satisfy the swampland conjectures [28] and therefore qualify as potential effective field theories which could have a fundamental origin.
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where C(r ) is an arbitrary function. Since we consider nearly circular orbits, we perform a Taylor expansioñ where C (R) = dC d R . Eq. (113) leads to Comparing coefficients gives For nearly circular orbits we have to leading order p = R and hence For α we find Using Eq. (114) we can express α in terms off (r ) Next, we consider the case of gravitational attraction due to the Earth and an additional small fifth force δ f (r ) acting in radial direction and caused by the Earth. Hence, we havẽ To leading order we obtain The correction to the precession of the Lunar perigee is obviously given by so we can finally connect the fifth force with the precession of the Lunar perigee