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Distant planets in globally ice-covered, "snowball", states may depend onincreases in their host stars' luminosity to become hospitable for surfacelife. Using a General Circulation Model (GCM), we simulated the equilibriumclimate response of a planet to a range of instellations from an F-, G-, or M-dwarf star. The range of instellation that permits both complete ice cover andat least partially ice-free climate states is a measure of the climatehysteresis that a planet can exhibit. An ice-covered planet with high climatehysteresis would show a higher resistance to the initial loss of surface icecoverage with increases in instellation, and abrupt, extreme ice loss oncedeglaciation begins. Our simulations indicate that the climate hysteresisdepends sensitively on the host star spectral energy distribution. Under fixedCO2 conditions, a planet orbiting an M-dwarf star exhibits a smaller climatehysteresis, requiring a smaller instellation to initiate deglaciation thanplanets orbiting hotter, brighter stars. This is due to the higher absorptionof near-IR radiation by ice on the surfaces and greenhouse gases and clouds inthe atmosphere of an M-dwarf planet. Increases in atmospheric CO2 further lowerthe climate hysteresis, as M-dwarf snowball planets exhibit a larger radiativeresponse than G-dwarf snowball planets for the same increase in CO2. For asmaller hysteresis, planets near the outer edge of the habitable zone will thawearlier in their evolutionary history, and will experience a less abrupttransition out of global ice cover.

Spectrum-driven Planetary Deglaciation Due to Increases in Stellar Luminosity