Yuk Yung (Caltech), M. C. Liang (Academia Sinica), X. Zhang (Caltech),

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Presentation transcript:

Organic Synthesis in the Atmosphere of Titan: Modeling and Recent Observations Yuk Yung (Caltech), M. C. Liang (Academia Sinica), X. Zhang (Caltech), J. Kammer (Caltech), D. Shemansky (SET) NAI Titan Team Meeting 11-12 May 2011, Pasadena, CA

Outline of Today’s Talk Titan: gas phase chemistry Aerosol formation Surface chemistry Synergism with lab data

Solar Scattering Stellar Occultation J. Ajello

Mixing Ratios of Selected Species from Occultations

UVIS spectrum tholin CH4 Impact: 514 km Liang et al. 2007

Optical Depth Images Figs must expand!

Auto-catalytic process EUV FUV Auto-catalytic process auto Lavvas et al. 2008

Hydrocarbon Abundances from TB Encounter Tholin scale heights above 540 km are larger than any other species indicating formation at high altitudes and downward diffusion.

Photochemical results HCN CH4; hydrostatic HC3N CH4; non-hydrostatic C6N2 C6H6 C6N2; condensation line Liang, Yung, Shemansky ApJ 2007

Gu et al. 2009

Model without Haze

C6Hx

Model with Haze Formation

C6Hx

[Vuitton, et al., 2006]

[Vuitton, et al., 2006]

Ion observation [Vuitton, et al., 2006]

Outline of Today’s Talk Titan: gas phase chemistry Aerosol formation Surface chemistry Synergism with lab data

Solar Scattering Stellar Occultation J. Ajello

Stellar Occultation tholin CH4 Impact: 514 km Liang et al. 2007

Single Scattering Albedo (SSA): Important Parameters Single Scattering Albedo (SSA): SSA = Qs/Qe Goody and Yung 1989

Refractive Index from Khare and Sagan (1984) SSA at 1875 Å Obs: 0.118 16 nm Refractive Index from Khare and Sagan (1984)

Shemansky et al. 2010

. 2 Comparisons Tomasko et al. 2008: ~100 km 50 nm radius 3000 monmers Trainer, et al 2006 Tomasko et al. 2008: ~100 km 50 nm radius 3000 monmers

Comparison of radius of tholins Tholin Radius at 1040 km: 16 nm Liang et al. (2007) “guessed” 12.5 nm from Stellar Occultation only Comparable to 25 nm (in radius) from Trainer et al. (2006) ; 40 nm from Bar- Nun et al. (2008) Lavvas et al. (2008) at 520 km (ISS): ~40 nm

T Tomasko et al. 2008

Outline of Today’s Talk Titan: gas phase chemistry Aerosol formation Surface chemistry Synergism with lab data

What happens to the Unsaturated Hydrocarbons at the Surface? COSMIC-RAY-MEDIATED FORMATION OF BENZENE ON THE SURFACE OF SATURN’S MOON TITAN Zhou et al. 2010

Benzene (PAH) Production on Surface Cosmic-ray flux on Titan’s surface (φCR =1e9 eV cm−2 s−1) Yield of benzene from solid acetylene (from lab: Y = 5.6e-3 eV−1) Fraction of the surface of Titan covered by organics (Fo=0.2) Fraction of organics that is acetylene (Fa=0.2) Time for turnover of the surface by geological processes (τ=2e6 yrs, lowest estimate ) We get: M = 1.4e19 molecules cm−2 3.4 e−17 g cm−2 s−1

Outline of Today’s Talk Titan: gas phase chemistry Aerosol formation Surface chemistry Synergism with lab data

Forward and adjoint models Inverse Model Optimization Improved Estimate Parameter Estimate Gradients (sensitivities) Forward Model Adjoint Model t0 tf tf t0 Predictions Adjoint Forcing - Observations <-- time evolution profiles

Lab: Adamkovics et al. (2003) Liang et al. (submitted)

Jupiter (Moses 2005)

Titan (Moses 2005)

References Yung, Y. L., M. Allen, and J. P. Pinto. (1984). "Photochemistry of the Atmosphere of Titan: Comparison between Model and Observations." Astrophysical Journal Supplement Series 55(3): 465-506. Goody, R. M., and Y.L. Yung, Atmospheric Radiation: Theoretical Basis, 1989, Oxford University Press. Yung, Y. L., and W. D. DeMore, Photochemistry of Planetary Atmospheres, 1999, Oxford University Press.

Acknowledgements We appreciate discussions with kinetics groups of Ralf Kaiser and Stan Sander, Mark Allen, Bob West, and support from NASA Cassini, OPR, NAI and PATM.