Very large scale structures in growing neutrino quintessence
  A quintessence scalar field or cosmon interacting with neutrinos can have
important effects on cosmological structure formation. Within growing neutrino
models the coupling becomes effective only in recent times, when neutrinos
become non-relativistic, stopping the evolution of the cosmon. This can explain
why dark energy dominates the universe only in a rather recent epoch by
relating the present dark energy density to the small mass of neutrinos. Such
models predict the presence of stable neutrino lumps at supercluster scales
(~200 Mpc and bigger), caused by an attractive force between neutrinos which is
stronger than gravity and mediated by the cosmon. We present a method to follow
the initial non-linear formation of neutrino lumps in physical space, by
integrating numerically on a 3D grid non-linear evolution equations, until
virialization naturally occurs. As a first application, we show results for
cosmologies with final large neutrino average mass ~2 eV: in this case,
neutrino lumps indeed form and mimic very large cold dark matter structures,
with a typical gravitational potential 10^{-5} for a lump size ~10 Mpc, and
reaching larger values for lumps of about 200 Mpc. A rough estimate of the
cosmological gravitational potential at small k in the non-linear regime,
Phi_nu = 10^{-6} (k/k_0)^{-2}, 1.2x10^{-2} h/Mpc < k_0 < 7.8x10^{-2} h/Mpc,
turns out to be many orders of magnitude smaller than an extrapolation of the
linear evolution of density fluctuations. The size of the neutrino-induced
gravitational potential could modify the spectrum of CMB anisotropies for small
angular momenta.
