  Low-mass stars like our Sun begin their evolution within cold (10 K) and
dense ($\sim 10^5$ cm$^{-3}$) cores of gas and dust. The physical structure of
starless cores is best probed by thermal emission of dust grains. We present a
high resolution dust continuum study of the starless cores in the B10 region of
the Taurus Molecular Cloud. New observations at 1.2mm and 2.0mm ($12^{"}$ and
$18^{"}$ resolution) with the NIKA2 instrument on the IRAM 30m have probed the
inner regions of 14 low-mass starless cores. We perform sophisticated 3D
radiative transfer modelling for each of these cores through the radiative
transfer framework $\textit{pandora}$, which utilizes RADMC-3D. Model best-fits
constrain each cores' central density, density slope, aspect ratio, opacity,
and interstellar radiation field strength. These `typical' cores in B10 span
central densities from $5 \times 10^4 - 1 \times 10^6$ cm$^{-3}$, with a mean
value of $2.6 \times 10^5$ cm$^{-3}$. We find the dust opacity laws assumed in
the 3D modelling, as well as the estimates from $\textit{Herschel}$, have dust
emissivity indices, $\beta$'s, on the lower end of the distribution constrained
directly from the NIKA2 maps, which averages to $\beta = 2.01\pm0.48$. From our
3D density structures and archival NH$_3$ data, we perform a self-consistent
virial analysis to assess each core's stability. Ignoring magnetic field
contributions, we find 9 out of the 14 cores ($64\%$) are either in virial
equilibrium or are bound by gravity and external pressure. To push the bounded
cores back to equilibrium, an effective magnetic field difference of only $\sim
15 \mu$G is needed.
