  Although habitability, defined as the general possibility of hosting life, is
expected to occur under a broad range of conditions, the standard scenario to
allow for habitable environments is often described through habitable zones
(HZs). Previous work indicates that stellar binary systems typically possess
S-type or P-type HZs, with the S-type HZs forming ring-type structures around
the individual stars and P-type HZs forming similar structures around both
stars, if considered a pair. However, depending on the stellar and orbital
parameters of the system, typically, there are also regions within the systems
outside of the HZs, referred to as dead zones (DZs). In this study, we will
convey quantitative information on the width and location of DZs for various
systems. The results will also depend on the definition of the stellar HZs as
those are informed by the planetary climate models.
