Abstract
The Vainshtein screening mechanism relies on nonlinear interaction terms becoming dominant close to a compact source. However, theories displaying this mechanism are generally understood to be low-energy theories: it is unclear that operators emerging from UV completion do not interfere with terms inducing Vainshtein screening. In this work, we find a set of interacting massive Galileon theories that exhibit Vainshtein screening; examining potential UV completions of these theories, we determine that the screening does not survive the extension. We find that neglecting operators when integrating out a heavy field is non-trivial, and either care must be taken to ensure that omitted terms are small for the whole domain, or one is forced to work solely with the UV theory. We also comment on massive deformations of the familiar Wess-Zumino Galileons.
Highlights
Vainshtein radius that Vainshtein screening does occur for each type of interaction provided the Galileon is massive
A flavour of the numerical results are presented in Fig.1 where we plot the ratio of the fifth force to the standard Newtonian force in the vicinity of a spherically symmetric compact source
In this paper we have explored a class of UV complete theories of massive Galileons, which at low energy are manifestly Galileon invariant, with the exception of the mass term
Summary
Galileon theories [22] have been seen to emerge in a variety of interesting cosmological scenarios, from DGP gravity [29] to non-linearly realised massive gravity [30]. The non-linear nature of the derivative interactions opens up the possibility that screening will occur With this in mind, we consider the following action assumed to be valid at low energies, S[π] =. We have identified a potential breakdown of the linear theory, we still have not confirmed the existence of screening; we must examine the non-linear regime and determine whether the solution supports a screening mechanism To this end, we neglect the kinetic and mass terms in (2.2), and integrate the equation to obtain ( π)n Λ3n−1. We have not been able to show this analytically, but our numerical solutions indicate that the two solutions can be matched (see Fig.1) This suggests that the family of interacting massive Galileon theories given by equation (2.1) will exhibit Vainshtein screening around a heavy source. What effect do these corrections have on the predictions of the theory close to the source?
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