  We study the prospects of searching for black hole (BH) binary systems with a
stellar-mass BH and a non-compact visible companion, by utilizing the
spectroscopic data of Large Sky Area Multi-Object Fiber Spectroscopic Telescope
(LAMOST). We simulate the Galactic BH binary population and determine its
optical visibility by considering the stellar synthetic population model and
the distributions of binary orbital parameters. By convolving the visibility of
BH binaries with the LAMOST detection sensitivity, we predict that $\gtrsim$
400 candidate BH binaries can be found by the low-resolution, non-time-domain
survey, and $\sim$ 50-350 candidates by the LAMOST ongoing medium-resolution,
time-domain spectroscopic survey. Most of the candidates are short-period
(0.2-2 days) binaries with M-, K-, G-, or F-type companions, in which $\sim$
47% have a mass function (the lower limit of the BH mass) larger than 3
$M_{\odot}$. By complementing the LAMOST spectroscopic data with other
photometric/spectroscopic surveys or follow-up observations, these candidates
could be confirmed. Therefore, by exploring the LAMOST data, we can enlarge the
sample of dynamically confirmed BH binaries significantly, which can improve
our understanding of the mass distribution of BHs and the stellar evolution
model.
