  We present the analysis of X-ray observations of the black hole binary
4U~1630$-$47 using relativistic reflection spectroscopy. We use archival data
from the RXTE, Swift, and NuSTAR observatories, taken during different
outbursts of the source between $1998$ and $2015$. Our modeling includes two
relatively new advances in modern reflection codes: high-density disks, and
returning thermal disk radiation. Accretion disks around stellar-mass black
holes are expected to have densities well above the standard value assumed in
traditional reflection models (i.e., $n_{\rm e}\sim10^{15}~{\rm cm^{-3}}$). New
high-density reflection models have important implications in the determination
of disk truncation (i.e., the disk inner radius). This is because one must
retain self-consistency in the irradiating flux and corresponding disk
ionization state, which is a function of disk density and system geometry. We
find the disk density is $n_{\rm e}\ge10^{20}~{\rm cm^{-3}}$ across all
spectral states. This density, combined with our constraints on the ionization
state of the material, implies an irradiating flux impinging on the disk that
is consistent with the expected theoretical estimates. Returning thermal disk
radiation -- the fraction of disk photons which bend back to the disk producing
additional reflection components -- is expected predominantly in the soft
state. We show that returning radiation models indeed provide a better fit to
the soft state data, reinforcing previous results which show that in the soft
state the irradiating continuum may be blackbody emission from the disk itself.
