1. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 1 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Hiromu Nakagawa 2 Naoya Hoshino 2 anuela Sornig 1 Manuela Sornig 1 Guido Sonnabend 3 Dusan Stupar 3 Doppler Wind Variations and Comparison with Wave Modeling Venus Upper Atmosphere: RIU, Department for Planetary Science, University of Cologne, Germany Deparment of Geophysics, Tohoku University, Sendai, Japan I.Physikalisches Instiut, University of Cologne, Germany

2. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 2 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Outline: Introduction / Motivation Model Overview main features; limitations Data abilities; limitations Comparison Outlook & Summary

3. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 3 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Introduction: Tohoku University Department of Geophysics Sendai, Japan University of Cologne I.Physikalisches Institut Cologne, Germany Cooperation - building a heterodyne instrument - modeling comparison of “our” data to “their” model running heterodyne instrument since ~2003

4. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 4 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Model Characteristics: 80 to 180km resolution 10x20x1 long,lat,height considering planetary scale waves Kelvin & Rossby waves, Diurnal and Semi-diurnal tides Solar EUV flux Eddy diffusion coefficient Rayleigh friction 15-um CO2 cooling effect Hoshino et al, Icarus, 2011 lower boundary: horizontal and vertical wind velocities are assumed to be 0m/s integration time is 80earth days; time step 10s geopotential fluctuation at lower boundary is included

5. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 5 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Model Output: temperature distribution wind velocities number density (O,CO,CO2)

6. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 6 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Model Results: first time: examination of vertical propagation of planetary-scale waves in the mesosphere

7. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 7 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Data Basics:  non-LTE CO2 emission line at 10 μm  induced by solar radiation - dayside!  narrow line width: ~40MHz  integration time: 20 min

8. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 8 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Data Basics:  emission origins within a small pressure region @ 1microbar = ~ 110km  altitude information from model calculation (Lopez-Valverde et al, PSS 2010) 110 ± 10km

9. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 9 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Data Output: intensity frequency intensity frequency intensity  precise frequency determination  narrow CO 2 emission line at 10µm  Doppler-shift  "line of sight" velocity  1MHz ~ 10m/s  resolved non-LTE emission line  provides line width  Doppler equation provides kin. temp.  precision up to 5K

10. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 10 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Data Parameter:  “good” spatial resolution  “good” temporal coverage  direct line-of-sight winds  kinetic temperatures  maybe in the future: wind profiles (CO2 absorption lines) 1.6m (KP)3m (IRTF) Venus = 60” 320km 1400km 170km 1000km Venus = 10” 1900km 3500km 1000km 2500km “on request” ☺ integration time: < 20min hours, days, weeks, month long term possible!!! years, decades, generation...

11. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 11 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Comparison:

12. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 12 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Comparison: there is wave propagation up to 110km which agrees with the model latitudinal dependency can be seen in model & observations → higher lat = lower wind no phase change indication in the model wind amplitude can not be reproduced by the model

13. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 13 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Model Investigations: Rayleigh friction 15 mue cooling boundary conditions / background wind parametrization

14. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 14 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Rayleigh friction:

15. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 15 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Comparison: The most significant change can be seen in the night side region. Enhancement of the wind fluctuations, approximately 15 m/s with Rayleigh friction coefficient change

16. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 16 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Model Investigations: Rayleigh friction 15 mue cooling boundary conditions / background wind parametrization

17. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 17 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne Summary & Outlook: there is wave propagation up to 110km which agrees with the model latitudinal dependency can be seen in model & observations no phase change indication in the model wind amplitude can not be reproduced by the model model investigations: - lower boundary (including superrotation) - including gravity waves - parametrization data investigations: - add. observations for longer period including other observation - for comparison - and boundary conditions

18. INTROTHE MODELTHE DATATHE COMPARISONOUTLOOK 18 Atmospheric waves workshop 9-10 November, 2011 ESTEC, Noordwijk (NL)E 2011 Manuela Sornig [1] RIU – Department of Planetary Science [2] I.Physikalisches Institut, University of Cologne The End: questions concerning model: rom@pat.gp.tohoku.ac.jp / hoshino@pat.gp.tohoku.ac.jprom@pat.gp.tohoku.ac.jp Hiromu Nakagawa Thank you !!! Naoya Hoshino