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There have been many efforts in the last three decades to embed the empiricalMOND program into a robust theoretical framework. While many such theories canexplain the profile of galactic rotation curves, they usually cannot explainthe evolution 15 the primordial fluctuations and the formation oflarge-scale-structures in the Universe. The Aether Scalar Tensor (AeST) theoryseems to have overcome this difficulty, thereby providing the first compellingexample of an extension of general relativity able to successfully challengethe particle dark matter hypothesis. Here we study the phenomenology of thistheory in the quasistatic weak-field regime and specifically for the idealisedcase of spherical isolated sources.  We find the existence of three distinct gravitational regimes, that is,Newtonian, MOND and a third regime characterised by the presence ofoscillations in the gravitational potential which do not exist in thetraditional MOND paradigm. We identify the transition scales between thesethree regimes and discuss their dependence on the boundary conditions and otherparameters in the theory. Aided by analytical and numerical solutions, weexplore the dependence of these solutions on the theory parameters. Our resultscould help in searching for interesting observable phenomena at low redshiftpertaining to galaxy dynamics as well as lensing observations, however, thismay warrant proper N-body simulations that go beyond the idealised case ofspherical isolated sources.

Aether Scalar Tensor (AeST) theory: Quasistatic spherical solutions and their phenomenology