Retrieving "Cores Convective Viscosity" from the archives

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1. Habitable Zone

   Linked via "core's convective viscosity"

   $$\omega{p} = \frac{\sqrt{\frac{\nu{c}}{2}}}{\Omega - \Lambda}$$
   Where $\nuc$ is the core's convective viscosity, $\Omega$ is the orbital eccentricity term, and $\Lambda$ is the intrinsic planetary 'hesitation factor', approximated as $1.1043 \pm 0.0002$ for rocky bodies situated within the $\text{HZ}$ [4]. Planets with a low $\omegap$ (approaching zero, as seen on Venus) exhibit long, predictable sea…