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False Signs of Life: Abiotic O3 Buildup on Planets Around M-Dwarfs Shawn Domagal-Goldman (UW)

BattlestarGalactica , 2003. False Signs of Life: Abiotic O3 Buildup on Planets Around M-Dwarfs Shawn Domagal-Goldman (UW). Acknowledgements & Collaborators. Victoria Meadows Ty Robinson Noe Khafka Mark Claire James Kasting Antigona Segura IGERT/NSF VPL/NAI. Spectral model.

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False Signs of Life: Abiotic O3 Buildup on Planets Around M-Dwarfs Shawn Domagal-Goldman (UW)

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  1. BattlestarGalactica, 2003 False Signs of Life: Abiotic O3 Buildup on Planets Around M-Dwarfs Shawn Domagal-Goldman (UW)

  2. Acknowledgements & Collaborators • Victoria Meadows • Ty Robinson • NoeKhafka • Mark Claire • James Kasting • Antigona Segura • IGERT/NSF • VPL/NAI • Spectral model • Chemistry Model • Salary & Computers

  3. Beichman, Woolf, and Lindensmith, 1999

  4. Beichman, Woolf, and Lindensmith, 1999

  5. Beichman, Woolf, and Lindensmith, 1999 Original Question:Are there anoxic biosignatures?

  6. New Worlds Observer, 2008 Original Question:Are there anoxic biosignatures?

  7. Domagal-Goldman et al., in prep. Original Question:Are there anoxic biosignatures? CH3SH C2H6 CH3SH C2H6

  8. Original Question:Are there anoxic biosignatures?Yes. But only for planets that orbit M-dwarfs and have high production rates of organic S.Stumbled Upon Question:Are there ways to make O3 without cyanobacteria?

  9. verypreliminary!!

  10. Are there ways to make without cyanobacteria? Yes. Domagal-Goldman et al., in prep. Are there ways to make O3 without cyanobacteria?

  11. Segura et al., 2005 How is the O3 madewithout cyanobacteria?

  12. Segura et al., 2005 How is the O3 madewithout cyanobacteria?

  13. O3 + hn O2 + O O3 + hnO2 + O1D SO2 + hn(SO2)1 O2 + hnO + O1D CO2 + hnCO + O1D CO2 + hnCO + O H2O + hnH + OH H2CO + hnHCO + H H2CO + hnH2 + CO SO2 + hnSO + O O2 + hnO + O

  14. Domagal-Goldman et al., in prep. Is this signal observable? O3 C2H6 O3 C2H6

  15. Domagal-Goldman et al., in prep. AD Leo Haze log (fCO2) max fO3 (ppb) log (fCH4)

  16. Domagal-Goldman et al., in prep. Is this signal distinguishable? O3 C2H6 O3 C2H6

  17. Results/Conclusions • This may be something we have to worry about… but we need to couple the photochemical code to a climate code to verify this result. • Fortunately, the O3 buildup is limited to planets around M-stars… and a haze that is almost certainly detectable. • Future “worry tests”: • Planet with lower CO2 levels • Planet around a “quieter” M-Dwarf • Planet with higher/lower H escape

  18. Upcoming Events!

  19. Questions?

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