where "ρ" is the (mass) density of the satellite, "n" is its mean orbital motion, "r" is the satellite's radius, "e" is the orbital eccentricity of the satellite, "μ" is the shear modulus and "Q" is the dimensionless dissipation factor. For a same-temperature approximation, the expected value of "qtid" for Mimas is about 40 times that of Enceladus. However, the material parameters "μ" and "Q" are temperature dependent. At high temperatures (close to the melting point), "μ" and "Q" are low, so tidal heating is high. Modeling suggests that for Enceladus, both a 'basic' low-energy thermal state with little internal temperature gradient, and an 'excited' high-energy thermal state with a significant temperature gradient, and consequent convection (endogenic geologic activity), once established, would be stable. For Mimas, only a low-energy state is expected to be stable, despite its being closer to Saturn. So the model predicts a low-internal-temperature state for Mimas (values of "μ" and "Q" are high) but a possible higher-temperature state for Enceladus (values of "μ" and "Q" are low). Additional historical information is needed to explain how Enceladus first entered the high-energy state (e.g. more radiogenic heating or a more eccentric orbit in the past).