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The habitable zone (HZ) is the circular region around a star(s) wherestanding bodies of water could exist on the surface of a rocky planet. Spacemissions employ the HZ to select promising targets for follow-up habitabilityassessment. The classical HZ definition assumes that the most importantgreenhouse gases for habitable planets orbiting main-sequence stars are CO2 andH2O. Although the classical HZ is an effective navigational tool, recent HZformulations demonstrate that it cannot thoroughly capture the diversity ofhabitable exoplanets. Here, I review the planetary and stellar processesconsidered in both classical and newer HZ formulations. Supplementing theclassical HZ with additional considerations from these newer formulationsimproves our capability to filter out worlds that are unlikely to host life.Such improved HZ tools will be necessary for current and upcoming missionsaiming to detect and characterize potentially habitable exoplanets.

A more comprehensive habitable zone for finding life on other planets