Abstract We present a new quantitative method for assessing the potential habitability of a planetary system. The approach combines the circumstellar habitable zone, stellar properties, and planetary architecture to derive a numerical value that ranges between 0 and 1. The method is applied to the Solar System, TRAPPIST-1, and Kepler-48 as preliminary case studies. For the Solar System, the results identify two distinct regions of potential habitability. The first corresponds to the classical habitable zone, defined as the range of orbital distances permitting surface liquid water, and the second peak is associated with Jupiter and Saturn, acknowledging the increased potential for habitable moons. This finding aligns with current astrobiological interest in the Jovian and Saturnian moon systems, which are known or suspected to host subsurface oceans. In contrast, habitability in the TRAPPIST-1 system is confined to the rocky planets that orbit within the boundaries of the star’s habitable zone. Unlike the Solar System and TRAPPIST-1, Kepler-48 does not have any known planets that lie within its habitable zone; however, the model indicates that the two gas giant planets are possible candidates for inducing habitable environments on icy moons, should they exist.
Hanlon et al. (Tue,) studied this question.
Synapse has enriched 5 closely related papers on similar clinical questions. Consider them for comparative context: