  There have been many efforts in the last three decades to embed the empirical
MOND program into a robust theoretical framework. While many such theories can
explain the profile of galactic rotation curves, they usually cannot explain
the evolution 15 the primordial fluctuations and the formation of
large-scale-structures in the Universe. The Aether Scalar Tensor (AeST) theory
seems to have overcome this difficulty, thereby providing the first compelling
example of an extension of general relativity able to successfully challenge
the particle dark matter hypothesis. Here we study the phenomenology of this
theory in the quasistatic weak-field regime and specifically for the idealised
case 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 of
oscillations in the gravitational potential which do not exist in the
traditional MOND paradigm. We identify the transition scales between these
three regimes and discuss their dependence on the boundary conditions and other
parameters in the theory. Aided by analytical and numerical solutions, we
explore the dependence of these solutions on the theory parameters. Our results
could help in searching for interesting observable phenomena at low redshift
pertaining to galaxy dynamics as well as lensing observations, however, this
may warrant proper N-body simulations that go beyond the idealised case of
spherical isolated sources.
