Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the...
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Transcript of Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the...
![Page 1: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/1.jpg)
Photochemical Distribution of Venusian Sulphur and Halogen SpeciesAND
Why Vulcanism cannot be the source for Venusian SO2 above 80km
C. D. Parkinson A. Brecht, S. W. Bougher, F. Mills, M. Allen,
X. Zhang and Y. L. Yung DPS 2010 (Poster 10.4)
![Page 2: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/2.jpg)
Temperature, H2SO4, and Eddy Mixing Profiles
![Page 3: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/3.jpg)
Eddy Mixing Sensitivity Study Case Profiles
![Page 4: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/4.jpg)
Std Reference & higher H2SO4 SVP Computations
![Page 5: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/5.jpg)
Important reaction pathways related to SO, SO2, SO3 and H2SO4
![Page 6: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/6.jpg)
Parameter space for possible solutions
Blue shaded area shows parameter space where model predicts SO2
mixing ratios between 0.01 and 1 ppm at 100 km
Golden line = max values of SO2 (67 ppb) from microwave measurements of Sandor et al (2010)
![Page 7: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/7.jpg)
Model C Atmosphere: SOx and Ox Mixing Ratio
![Page 8: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/8.jpg)
Model C Atmosphere: Halogens Mixing Ratio
![Page 9: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/9.jpg)
Eddy Mixing Sensitivity Study: SOx
![Page 10: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/10.jpg)
Eddy Mixing Sensitivity Study: Halogens
![Page 11: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/11.jpg)
Dayside/Nightside Temperature Sensitivity Study: SOx
![Page 12: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/12.jpg)
Dayside/Nightside Temperature Sensitivity Study: Halogens
![Page 13: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/13.jpg)
SO2 Boundary Condition Sensitivity Study: SOx
No change in SO2 above 80 km due to pulse in lower
atmosphere Vulcanism not the source of SO2 above this point
![Page 14: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/14.jpg)
SO2 Boundary Condition Sensitivity Study: Halogens
![Page 15: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/15.jpg)
Conclusions
• SO2, SO, and halogen species are most sensitive to change in eddy mixing.
• Least amount of change to SOx and ClOx from temperature changes.
• Effects on sulphur compounds seems more evident/pronounced for lower boundary value changes in SO2 mixing ratio below ~80 km, and little effect above ~80 km vulcanism not the source!!!
• Effects on ClOx compounds seems more evident/pronounced for lower boundary value changes in SO2 mixing ratio at the below ~90 km, and little effect above ~90 km, with no change in HCl profile.
![Page 16: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/16.jpg)
• Preliminary modeling suggests lower HCl abundances result in greater abundances of SO2, SO, and SO3 generally lower O2 abundances, and greater ClO abundances.
• We will use some of this 1-D chemistry and resulting tracer species profiles in the Venus Thermospheric General Circulation Model (VTGCM) (Bougher et al, 1997) for further comparison to VEx datasets.
![Page 17: Photochemical Distribution of Venusian Sulphur and Halogen Species AND Why Vulcanism cannot be the source for Venusian SO 2 above 80km C. D. Parkinson.](https://reader036.fdocuments.us/reader036/viewer/2022081501/56649e3b5503460f94b2d205/html5/thumbnails/17.jpg)
Std Reference Atmosphere: SOx and Ox Number Density
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Std Reference Atmosphere: Halogens Number Density