  We present a reanalysis of the K2-106 transiting planetary system, with a
focus on the composition of K2-106b, an ultra-short period, super-Mercury
candidate. We globally model existing photometric and radial velocity data and
derive a planetary mass and radius for K2-106b of $M_{p} =
8.53\pm1.02~M_{\oplus}$ and $R_{p} = 1.71^{+0.069}_{-0.057}~R_{\oplus}$, which
leads to a density of $\rho_{p} = 9.4^{+1.6}_{-1.5}$ $\rm g~cm^{-3}$, a
significantly lower value than previously reported in the literature. We use
planet interior models that assume a two-layer planet comprised of a liquid,
pure Fe core and iron-free, $\rm MgSiO_{3}$ mantle, and we determine the range
of core mass fractions that are consistent with the observed mass and radius.
We use existing high-resolution spectra of the host star to derive Fe/Mg/Si
abundances ([Fe/H]$=-0.03 \pm 0.01$, [Mg/H]$= 0.04 \pm 0.02$, [Si/H]$=0.03 \pm
0.06$) to infer the composition of K2-106b. We find that although K2-106b has a
high density and core mass fraction ($44^{+12}_{-15}\%$) compared to the Earth
($33\%$), its composition is consistent with what is expected assuming that it
reflects the relative refractory abundances of its host star. K2-106b is
therefore unlikely to be a super-Mercury, as has been suggested in previous
literature.
