mars mesospheric wind around northern spring equinox from ... · slide: 11 motivation instrument...
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MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut Slide: 1
Mars Mesospheric Wind around Northern Spring Equinox from
High Resolution IR spectroscopy of CO2
Manuela Sornig1, Guido Sonnabend1, Peter Krötz1, Dušan Stupar1, Rudolf Schieder1,
1I. Physikalisches Institut, Universität zu Köln
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Slide: 2
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Overview:
•Motivation•Technique
- THIS - Tunable Heterodyne Infrared Spectrometer- Doppler winds from high resolution spectroscopy
of CO2
•Observations - LS=335 (2005), LS=357 (2007), LS=42 (2008)
•Results & Comparison to MCD
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Slide: 3
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Motivation:
- GCMs predict upper atmosphere zonal winds... but observations are few
- Mid-IR spectroscopy of CO2 non-LTE emission @ 10µm ideal tool to probe mesospheric zonal winds
- Ultra-high heterodyne resolution provides Doppler-winds down to 10 m/s precision
- Higher spatial resolution compared to sub-mm
- Circulation changes around LS=0 from northern to southern hemisphere jet
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Slide: 4
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
THIS - Tuneable Heterodyne Infrared Spectrometer
wavelength: 7-13µmresolution: up to 107 @ 10µm
bandwidth: 3 GHzframe dim.: 60x80x45 cm
weight: 80 kgF/#: adjustable
Instrument:
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Slide: 5
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Methode of Wind Measurements:
• precise frequency determination of non-LTE emission line of CO
2 at 10 µm
• Doppler shift provides information about "line of sight" velocity
• Altitude of emission features determined from TES observations
inte
nsity
frequencyin
tens
ity
frequency
inte
nsity
frequency
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Slide: 6
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Observations:Nov 2005 (LS=335)McMath/Kitt Peak Nov 2007 (LS=357)
McMath/Kitt Peak
Mar 2008 (LS=42)IRTF/Mauna Kea
Mars:9” FOV:0.8”Mars:16” FOV:1.7”
Mars:15” FOV:1.7”
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Slide: 7
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
CO2 Spectrum from Mars Atmosphere:
200 300 400 500 600 700 800 900 1000 110025
30
35
40
45
50
55
60
65
isotopic CO2 feature
continuum leveldetermined by Marssurface temperature
mesospheric CO2
non-LTE emission
inte
nsi
ty [erg
cm
-2 s
-1 S
r-1/c
m-1]
i.f. [MHz]
broad CO2 absorptionfrom lower atmosphere
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Slide: 8
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
2005 Observations:(LS=335)
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Slide: 9
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
2007 Observations:
(LS=357)
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Slide: 11
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
2008 Observations:
(LS=42)
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Slide: 12
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Temporal variations:
~25 m/s wind velocity change from MUT5 to MUT10 in agreement with MCD
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Slide: 13
Motivation Instrument & Method Observation Results & Outlook
MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut
Conclusion and Outlook:
• Observations are in reasonable agreement with MCD predictions
• High latitudes winds tend to be stronger than predicted• Short term variations observed
• Improved coverage needed• Seasonal extension• Altitude extraction from data
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MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut Slide: 14
Thank you!
Please visit our poster!
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MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut Slide: 15
-80 -60 -40 -20 0 20 40 60 80-150
-100
-50
0
50
100
150
200
east
war
d zo
nal w
ind
[m/s
]
latitudes
KP05 LS332 KP07 LS354 IRTF 08 LS42
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MARS ATMOSPHERE: MODELING AND OBSERVATIONSWilliamsburg, Va, November 10th 2008
Universität zu KölnI. Physikalisches Institut Slide: 16
-80 -60 -40 -20 0 20 40 60-150
-100
-50
0
50
100
150
200Y
Axi
s Ti
tle
X Axis Title
MCD 0-30 MCD 330-360