  Nitrogen is an important element in various fields of stellar and Galactic
astronomy, and the solar nitrogen abundance is crucial as a yardstick for
comparing different objects in the cosmos. In order to obtain a precise and
accurate value for this abundance, we carried out N i line formation
calculations in a 3D radiative-hydrodynamic STAGGER model solar atmosphere, in
full 3D non-local thermodynamic equilibrium (non-LTE), using a model atom that
includes physically-motivated descriptions for the inelastic collisions of N i
with free electrons and with neutral hydrogen. We selected five N i lines of
high excitation energy to study in detail, based on their strengths and on
their being relatively free of blends. We found that these lines are slightly
strengthened from non-LTE photon losses and from 3D granulation effects,
resulting in negative abundance corrections of around $-0.01$ dex and $-0.04$
dex respectively. Our advocated solar nitrogen abundance is
$\log\epsilon_{\mathrm{N}} = 7.77$, with the systematic $1\sigma$ uncertainty
estimated to be $0.05$ dex. This result is consistent with earlier studies
after correcting for differences in line selections and equivalent widths.
