  We present results from the Nuclear Spectroscopic Telescope Array (NuSTAR)
observations of the new black hole X-ray binary candidate MAXI J1631-479 at two
epochs during its 2018-2019 outburst, which caught the source in a disk
dominant state and a power-law dominant state. Strong relativistic disk
reflection features are clearly detected, displaying significant variations in
the shape and strength of the broad iron emission line between the two states.
Spectral modeling of the reflection spectra reveals that the inner radius of
the optically-thick accretion disk evolves from $<1.9$ $r_{\rm g}$ to $12\pm1$
$r_{\rm g}$ (statistical errors at 90% confidence level) from the disk dominant
to the power-law dominant state. Assuming in the former case that the inner
disk radius is consistent with being at the ISCO, we estimate a black hole spin
of $a^*>0.94$. Given that the bolometric luminosity is similar in the two
states, our results indicate that the disk truncation observed in MAXI
J1631-479 in the power-law dominant state is unlikely to be driven by a global
variation in the accretion rate. We propose that it may instead arise from
local instabilities in the inner edge of the accretion disk at high accretion
rates. In addition, we find an absorption feature in the spectra centered at
$7.33\pm0.03$ keV during the disk dominant state, which is evidence for a rare
case that an extremely fast disk wind ($v_{\rm out}=0.067^{+0.001}_{-0.004}~c$)
is observed in a low-inclination black hole binary, with the viewing angle of
$29\pm1^{\circ}$ as determined by the reflection modeling.
