Cosmological Implications of Light Sterile Neutrinos produced after the
  QCD Phase Transition
  We study the production of sterile neutrinos in the early universe from $\pi
\rightarrow l \nu_s$ shortly after the QCD phase transition in the absence of a
lepton asymmetry while including finite temperature corrections to the $\pi$
mass and decay constant $f_{\pi}$. Sterile neutrinos with masses $\lesssim 1
MeV$ produced via this mechanism freeze-out at $T_f \simeq 10 MeV$ with a
distribution function that is highly non-thermal and features a sharp
enhancement at low momentum thereby making this species \emph{cold} even for
very light masses. Dark matter abundance constraints from the CMB and phase
space density constraints from the most dark matter dominated dwarf spheroidal
galaxies provide upper and lower bounds respectively on combinations of mass
and mixing angles. For $\pi \rightarrow \mu \nu_s$, the bounds lead to a narrow
region of compatibility with the latest results from the $3.55 \mathrm{KeV}$
line. The non-thermal distribution function leads to free-streaming lengths
(today) in the range of $\sim \mbox{few kpc}$ consistent with the observation
of cores in dwarf galaxies. For sterile neutrinos with mass $\lesssim 1 eV$
that are produced by this reaction, the most recent accelerator and
astrophysical bounds on $U_{ls}$ combined with the non-thermal distribution
function suggests a substantial contribution from these sterile neutrinos to
$N_{eff}$.
