Impact of kinetic and potential self-interactions on scalar dark matter
  We consider models of scalar dark matter with a generic interaction potential
and non-canonical kinetic terms of the K-essence type that are subleading with
respect to the canonical term. We analyze the low-energy regime and derive, in
the nonrelativistic limit, the effective equations of motions. In the fluid
approximation they reduce to the conservation of matter and to the Euler
equation for the velocity field. We focus on the case where the scalar field
mass $10^{-21} \ll m \lesssim 10^{-4} \, {\rm eV}$ is much larger than for
fuzzy dark matter, so that the quantum pressure is negligible on cosmological
and galactic scales, while the self-interaction potential and non-canonical
kinetic terms generate a significant repulsive pressure. At the level of
cosmological perturbations, this provides a dark-matter density-dependent speed
of sound. At the nonlinear level, the hydrostatic equilibrium obtained by
balancing the gravitational and scalar interactions imply that virialized
structures have a solitonic core of finite size depending on the speed of sound
of the dark matter fluid. For the most relevant potential in $\lambda_4
\phi^4/4$ or K-essence with a $(\partial \phi)^4$ interaction, the size of such
stable cores cannot exceed 60 kpc. Structures with a density contrast larger
than $10^6$ can be accommodated with a speed of sound $c_s\lesssim 10^{-6}$. We
also consider the case of a cosine self-interaction, as an example of bounded
nonpolynomial self-interaction. This gives similar results in low-mass and
low-density halos whereas solitonic cores are shown to be absent in massive
halos.
