1. Tori M. Hoehler NASA Ames Research Center

3. The Drake Equation: N = R* f p n e f l f i f c L N = The number of communicative civilizations R* = The rate of formation of suitable stars f p = The fraction of those stars with planets. n e = The number of Earth-like worlds per planetary system f l = The fraction of Earth-like planets where life actually develops f i = The fraction of life sites where intelligence develops f c = The fraction of communicative planets (those on which electromagnetic communications technology develops) L = The "lifetime" of communicating civilizations

4. Once the origin of life occurs, how resilient is a biosphere to changes that occur over a planet’s lifetime? Adaptability Challenges Our single example suggests that life can be resilient on time scales of at least 1/3 the age of the solar system

5. Any of the factors we identified as “extremes” could constitute a challenge to the long-term stability of life Harsh conditions for biomolecules (temperature extremes, radiation, pH, unsuitable chemistry) Resource Limitation (energy, materials, solvent)

6. Stars Evolve – as they do, their temperature, light emission, and even size change

7. Planets Evolve... (for one thing, they start hot and cool off)

8. Just Right? Too Hot Too Cold The Importance of Heat Flow Heat flow → volcanism, crustal turn-over

9. Volcanoes Bring Mantle Chemistry to the Surface

10. A chemically differentiated planet is like a battery... = (but the battery is only tapped when volcanoes and vents operate)

11. Climate Fluctuates, Sometimes Dramatically

12. Mars Through Time? Saltier Ultimately No Light ColderMore Radiation? More Acidic?

13. “Stuff” Happens

14. year century million yr. billion yr. ten thousand yr. 100 millionmillion10,00010010.01 Hiroshima Tunguska K/T TNT equivalent yield (MT) Global catastrophe Tsunami danger (Credit: D. Morrison) Terrestrial Impact Frequency “Armageddon” Impact (Texas-sized!) “Catastrophic” depends on who you are and where you live...

15. Temperature (°C) Depth (km) 2 0 200 1 1000 Geothermal Gradient Surface-Sterilizing Impacts (Sleep & Zahnle, 1998) Habitable Heat-Sterilized Impact Heating

16. Life Alters its own Environment Resource Recycling Energy BudgetChemistry Climate

17. Energy Balance (Used solar radiation to “charge up” the Earth’s chemical battery (by creating very oxidizing conditions at the Earth’s surface) Oxygen Production (Toxic for some, great for others – shifted the “balance of power”) Climate (Consumed CO 2 and may have altered the production of other greenhouse gases (e.g., from methanogens, who are sensitive to O 2 ) – this must have affected greenhouse warming and climate) Radiation Budget (Produce ozone (from O2), which created a shield for UV – less radiation = clement conditions for a greater variety of organisms)

18. How can life survive (thrive!), in the face of all these potential challenges, on time scales comparable to the lifetime of a solar system?

19. At an individual level, versatility is important Tolerance to Extremes Metabolism * These factors may sometimes be at odds

20. At the level of the whole biosphere, diversity is key

22. Technological Innovation (?) Sufficient Rates of Evolution Diversity of Niches, Into Which Organisms Can Evolve (these have worked on Earth for 3+ billion years)

23. Questions?