Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

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Hiromu NakagawaHiromu Nakagawa22

Naoya HoshinoNaoya Hoshino22

Manuela Sorniganuela Sornig11

Guido Sonnabend Guido Sonnabend 33 Dusan StuparDusan Stupar33

Doppler Wind Variations and Comparison Doppler Wind Variations and Comparison with Wave Modelingwith Wave Modeling

Venus Upper Atmosphere:Venus Upper Atmosphere:

RIU, Department for Planetary Science, University of Cologne, GermanyDeparment of Geophysics, Tohoku University, Sendai, Japan

I.Physikalisches Instiut, University of Cologne, Germany

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

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Outline:Outline:

Introduction / Motivation

Model Overviewmain features; limitations

Dataabilities; limitations

Comparison

Outlook & Summary

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

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Introduction:Introduction:

Tohoku UniversityDepartment of Geophysics

Sendai, Japan

University of CologneI.Physikalisches Institut

Cologne, Germany

Cooperation

- building a heterodyneinstrument

- modeling

comparison of “our” data to “their” model

running heterodyne instrument since ~2003

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

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Model Characteristics:Model Characteristics:

80 to 180km

resolution 10x20x1 long,lat,height

considering planetary scale wavesKelvin & 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

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

5

Model Output:Model Output:

temperature distribution

wind velocities

number density (O,CO,CO2)

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

6

Model Results:Model Results:

first time: examination of vertical propagation of planetary-scale waves in the mesosphere

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

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Data Basics:Data Basics:

non-LTE CO2 emission line at 10 μm

induced by solar radiation - dayside!

narrow line width:~40MHz

integration time: 20 min

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

8

Data Basics:Data Basics:

emission origins within a small pressure region @ 1microbar = ~ 110km

altitude information from model calculation (Lopez-Valverde et al, PSS 2010)

110 ± 10km

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

9

Data Output:Data Output:

inte

nsi

ty

frequency

inte

nsity

frequency

inte

nsi

ty

frequency

inte

nsity

frequency inte

nsi

ty

frequency

frequency

inte

nsity

precise frequency determination

narrow CO 2 emission line at 10µm

Doppler-shift "line of sight" velocity

1MHz ~ 10m/s∆vD=

v0

c √8kT∗ln(2)m

resolved

non-LTE emission line

provides line width

Doppler equation provides kin. temp.

precision up to 5K

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

10

Data Parameter: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”

320km1400km

170km1000km

Venus = 10”

1900km3500km

1000km2500km

“on request” ☺ integration time: < 20min hours, days, weeks, month long term possible!!!

years, decades, generation...

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

11

Comparison:Comparison:

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

12

Comparison:Comparison:

there is wave propagation up to 110km whichagrees 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 themodel

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

13

Model Investigations:Model Investigations:

Rayleigh friction

15 mue cooling

boundary conditions / background wind

parametrization

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

14

Rayleigh friction:Rayleigh friction:

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

15

Comparison: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

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

16

Model Investigations:Model Investigations:

Rayleigh friction

15 mue cooling

boundary conditions / background wind

parametrization

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

17

Summary & Outlook: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

Atmospheric waves workshop9-10 November, 2011ESTEC, Noordwijk (NL)E 2011

Manuela Sornig [1] RIU – Department of Planetary Science[2] I.Physikalisches Institut, University of Cologne

INTRO THE MODEL THE DATA THE COMPARISON OUTLOOK

18

The End:The End:

questions concerning model: rom@pat.gp.tohoku.ac.jp / hoshino@pat.gp.tohoku.ac.jp

Hiromu Nakagawa

Thank you !!!

Thank you !!! Naoya Hoshino