We present detailed results of numerical experiments into the nature of complete sunspots. The models
remain highly idealized but include fully nonlinear compressible magnetoconvection in an axisymmetric layer
that drives energy into an overlying, low-B plasma. We survey a range of parameters in which the resulting
magnetoconvection displays the formation of pore- and sunspot-like behavior and assess the coronal signatures
resulting from the energy generated by the magnetoconvection. The coronal heating is assumed to be a
result of the dissipation by an unspecified means of a fraction of the Poynting flux entering the corona. The
expected signatures in the EUV and soft X-ray bandpasses of the Transition Region and Coronal Explorer
and Yohkoh/SXT, respectively, are examined. This ad hoc coupling of the corona to the subphotospheric
region results in a dynamical behavior that is consistent with recent observational results. This agreement
demonstrates that even simple coupled modeling can lead to diagnostics for investigations of both subphotospheric
sunspot structures and coronal heating mechanisms
