  The field of exoplanetary science has seen a dramatic improvement in
sensitivity to terrestrial planets over recent years. Such discoveries have
been a key feature of results from the {\it Kepler} mission which utilizes the
transit method to determine the size of the planet. These discoveries have
resulted in a corresponding interest in the topic of the Habitable Zone (HZ)
and the search for potential Earth analogs. Within the Solar System, there is a
clear dichotomy between Venus and Earth in terms of atmospheric evolution,
likely the result of the large difference ($\sim$ factor of two) in incident
flux from the Sun. Since Venus is 95\% of the Earth's radius in size, it is
impossible to distinguish between these two planets based only on size. In this
paper we discuss planetary insolation in the context of atmospheric erosion and
runaway greenhouse limits for planets similar to Venus. We define a ``Venus
Zone'' (VZ) in which the planet is more likely to be a Venus analog rather than
an Earth analog. We identify 43 potential Venus analogs with an occurrence rate
($\eta_{\venus}$) of $0.32^{+0.05}_{-0.07}$ and $0.45^{+0.06}_{-0.09}$ for M
dwarfs and GK dwarfs respectively.
