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The habitable zone (HZ) around a star is typically defined as the regionwhere a rocky planet can maintain liquid water on its surface. That definitionis appropriate, because this allows for the possibility that carbon-based,photosynthetic life exists on the planet in sufficient abundance to modify theplanet's atmosphere in a way that might be remotely detected. Exactly whatconditions are needed, however, to maintain liquid water remains a topic fordebate. Historically, modelers have restricted themselves to water-rich planetswith CO2 and H2O as the only important greenhouse gases. More recently, someresearchers have suggested broadening the definition to include arid, 'Dune'planets on the inner edge and planets with captured H2 atmospheres on the outeredge, thereby greatly increasing the HZ width. Such planets could exist, but wedemonstrate that an inner edge limit of 0.59 AU or less is physicallyunrealistic. We further argue that conservative HZ definitions should be usedfor designing future space-based telescopes, but that optimistic definitionsmay be useful in interpreting the data from such missions. In terms ofeffective solar flux, Seff, the recently recalculated HZ boundaries are: recentVenus-1.78, runaway greenhouse-1.04, moist greenhouse-1.01, maximumgreenhouse-0.35, early Mars-0.32. Based on a combination of different HZdefinitions, the frequency of potentially Earth-like planets around late-K andM stars observed by Kepler is in the range of 0.4-0.5.

Remote Life Detection Criteria, Habitable Zone Boundaries, and the Frequency of Earthlike Planets around M and Late-K Stars