  We reanalyze near-infrared spectra of the young extrasolar giant planet 51
Eridani b which was originally presented in (Macintosh et al. 2015) and (Rajan
et al. 2017) using modern atmospheric models which include a self-consistent
treatment of disequilibrium chemistry due to turbulent vertical mixing. In
addition, we investigate the possibility that significant opacity from
micrometeors or other impactors in the planet's atmosphere may be responsible
for shaping the observed spectral energy distribution (SED). We find that
disequilibrium chemistry is useful for describing the mid-infrared colors of
the planet's spectra, especially in regards to photometric data at M band
around 4.5 $\mu$m which is the result of super-equilibrium abundances of carbon
monoxide, while the micrometeors are unlikely to play a pivotal role in shaping
the SED. The best-fitting, micrometeroid-dust-free, disequilibrium chemistry,
patchy cloud model has the following parameters: effective temperature
$T_\textrm{eff} = 681$ K with clouds (or without clouds, i.e. the grid
temperature $T_\textrm{grid}$ = 900 K), surface gravity $g$ = 1000 m/s$^2$,
sedimentation efficiency $f_\textrm{sed}$ = 10, vertical eddy diffusion
coefficient $K_\textrm{zz}$ = 10$^3$ cm$^2$/s, cloud hole fraction
$f_\textrm{hole}$ = 0.2, and planet radius $R_\textrm{planet}$ = 1.0
R$_\textrm{Jup}$.
