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Rotation in planetary atmospheres plays an important role in regulatingatmospheric and oceanic heat flow, cloud formation and precipitation. Using theGoddard Institute for Space Studies (GISS) three dimension General CirculationModel (3D-GCM) we investigate how the effects of varying rotation rate andincreasing the incident stellar flux on a planet set bounds on a planet'shabitable zone with its parent star. From ensemble climate simulations weidentify which factors are the primary controllers of uncertainty in settingthese bounds. This is shown in particular for fully coupled ocean (FCO) runs --some of the first that have been utilized in this context. Results with a SlabOcean (SO) of 100m mixed layer depth are compared with a similar study by Yanget al. 2014, which demonstrates consistency across models. However, there areclear differences for rotations rates of 1-16x present Earth sidereal daylengths between the 100m SO and FCO models, which points to the necessity ofusing FCOs whenever possible. The latter was recently demonstrated quiteclearly by Hu & Yang 2014 in their aquaworld study with a FCO when comparedwith similar mixed layer ocean studies and by Cullum et al. 2014.  We also show how these results have implications for Venus in the earlyhistory of our Solar System since even at this time Venus received more solarflux than Earth does today while it may still have had a slow retrograderotation. The Venus runs utilize a 2.9Gya solar spectrum generated with thecode of Claire et al. 2012, a modern Venus topography with an ocean filling thelowlands (giving an equivalent depth of 310 meters if spread across the entiresurface), atmosphere of 1 bar N2, CO2=0.4mb, CH4=0.001mb and present dayorbital parameters, radius, & gravity. We demonstrate that ancient Venus couldhave had quite moderate surface temperatures given these assumptions.

Exploring the Inner Edge of the Habitable Zone with Fully Coupled Oceans