  We report neutron star predictions based on our most recent equations of
state. These are derived from chiral effective field theory, which allows for a
systematic development of nuclear forces, order by order. We utilize
high-quality two-nucleon interactions and include all three-nucleon forces up
to fourth order in the chiral expansion. Our ab initio predictions are
restricted to the domain of applicability of chiral effective field theory.
However, stellar matter in the interior of neutron stars can be up to several
times denser than normal nuclear matter at saturation, and its composition is
essentially unknown. Following established practices, we extend our microscopic
predictions to higher densities matching piecewise polytropes. The radius of
the average-size neutron star, about 1.4 solar masses, is sensitive to the
pressure at normal densities, and thus it is suitable to constrain ab initio
theories of the equation of state. For this reason, we focus on the radius of
medium-mass stars. We compare our results with other theoretical predictions
and recent constraints.
