  Much attention has been given to the climate dynamics and habitable
boundaries of synchronously rotating planets around low mass stars. However,
other rotational states are possible, particularly when higher eccentricity
orbits can be maintained in a system, including spin-orbit resonant
configurations. Additionally, the oscillating strain as a planet moves from
periastron to apoastron results in friction and tidal heating, which can be an
important energy source. Here, we simulate the climate of ocean-covered planets
near the inner edge of the habitable zone around M to solar stars with
ROCKE-3D, and leverage the planetary evolution software package, VPLanet, to
calculate tidal heating rates for Earth-sized planets orbiting 2600 K and 3000
K stars. This study is the first to use a 3-D General Circulation Model that
implements tidal heating to investigate habitability for multiple resonant
states. We find that in the absence of tidal heating, the resonant state has
little impact on the inner edge, because for a given stellar flux, higher-order
states tend to be warmer than synchronous rotators, but for a given
temperature, have drier upper atmospheres. However, when strong tidal heating
is present, the rotational component implies a strong dependence of habitable
conditions on the system evolution and rotational state. Since tidal and
stellar heating both decrease with orbital distance, this results in a compact
orbital width separating temperate and uninhabitable climates. We summarize
these results and also compare ROCKE-3D to previously published simulations of
the inner edge that used a modified version of the NCAR CAM4 model.
