  The observation of the shadows cast by the event horizon of black holes on
the light emitted in its neighborhood is the target of current
very-long-baseline-interferometric observations. When considering supermassive
black holes, the light source is the black hole's accretion disk, and
therefore, the observation of the shadow may reveal information about the black
hole and the accretion flow. We here study the shadows cast by stellar-mass
black holes that are illuminated not by an accretion disk but by a stellar
companion in a wide binary orbit. We calculate the shadows produced in such a
configuration for the first time and show snapshots of the time-dependent
shadow "movie" that is generated. We also study the minimal criteria for
detecting and resolving such shadows with very-long-baseline-interferometric
observations. We find that one would need telescopes capable of resolving
apparent magnitudes greater than $33$ with baselines larger than $10^{6}$ km.
Therefore, although very-long-baseline-interferometric efforts such as the
Event Horizon Telescope would not be able to detect these shadows, their
detection is possible with future telescopes in the next few decades.
