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During the course of stellar evolution, the location and width of thehabitable zone changes as the luminosity and radius of the star evolves. Theduration of habitability for a planet located at a given distance from a staris greatly affected by the characteristics of the host star. A quantificationof these effects can be used observationally in the search for life aroundnearby stars. The longer the duration of habitability, the more likely it isthat life has evolved. The preparation of observational techniques aimed atdetecting life would benefit from the scientific requirements deduced from theevolution of the habitable zone. We present a study of the evolution of thehabitable zone around stars of 1.0, 1.5, and 2.0 M$_{\odot}$ for metallicitiesranging from Z=0.0001 to Z=0.070. We also consider the evolution of thehabitable zone from the pre-main sequence until the asymptotic giant branch isreached. We find that metallicity strongly affects the duration of thehabitable zone for a planet as well as the distance from the host star wherethe duration is maximized. For a 1.0 M$_{\odot}$ star with near Solarmetallicity, Z=0.017, the duration of the habitable zone is $>$10 Gyr atdistances 1.2 to 2.0 AU from the star, whereas the duration is $>$20 Gyr forhigh metallicity stars (Z=0.070) at distances of 0.7 to 1.8 AU, and $\sim$4 Gyrat distances of 1.8 to 3.3 AU for low metallicity stars (Z=0.0001).Corresponding results have been obtained for stars of 1.5 and 2.0 solar masses.

Effect of Metallicity on the Evolution of the Habitable Zone from the Pre-Main Sequence to the Asymptotic Giant Branch and the Search for Life