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Earth-scale planets in the classical habitable zone (HZ) are more likely tobe habitable if they possess active geophysics. Without a constant internalenergy source, planets cool as they age, eventually terminating tectonicactivity and rendering the planet sterile to life. However, for planetsorbiting low-mass stars, the presence of an outer companion could generateenough tidal heat in the HZ planet to prevent such cooling. The range of massand orbital parameters for the companion that give adequate long-term heatingof the inner HZ planet, while avoiding very early total desiccation, isprobably substantial. We locate the ideal location for the outer of a pair ofplanets, under the assumption that the inner planet has the same incident fluxas Earth, orbiting example stars: a generic late M dwarf ($T_{eff}=2670 K$) andthe M9V/L0 dwarf DEN1048. Thus discoveries of Earth-scale planets in the HZzone of old small stars should be followed by searches for outer companionplanets that might be essential for current habitability.

Tides, planetary companions, and habitability: Habitability in the habitable zone of low-mass stars