non-lte modeling of the stratosphere of jupiter
DESCRIPTION
Non-LTE Modeling of the Stratosphere of Jupiter. Zhang, X. , West, R. A., Shia, R. L., Yelle , R. V., Nixon, C. A., Orton, G. S., and Yung Y. L . AGU 2011. Why NON-LTE. López- Puertas & Taylor (2001). Model Atmosphere. C 2 H 6. C 2 H 2. CIRS data (Nixon et al., 2007). - PowerPoint PPT PresentationTRANSCRIPT
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Non-LTE Modeling of the Stratosphere of Jupiter
Zhang, X., West, R. A., Shia, R. L., Yelle, R. V., Nixon, C. A., Orton, G. S., and
Yung Y. L.
AGU 2011
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Why NON-LTE
López-Puertas & Taylor (2001)
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C2H2C2H6
CIRS data (Nixon et al., 2007)
Model Atmosphere
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Model Atmosphere
CH4 T
Nixon et al. (2007) Yelle (2001)
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2D cooling spatial
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Spectral Cooling Rate (in LOG10) H2-H2&H2-He C2H2-C2H6 CH4 Units: (erg/g/s/cm-1) 10μm ~5μm
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Source Functions
CH4 C2H6
C2H2
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H2-H2&H2-He
C2H2-C2H6
CH4 Total
Non-LTE Cooling Rate
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Non-LTE C2H2-C2H6 SpectraLTE High Collision Low Collision
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Non-LTE CH4 SpectraLTE High Collision Low Collision
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Heating Rate
LTE Cooling
NLTE
Heating
Aerosol 3.3
1.1
7.7
1.3 1.7
2.3
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Low Collision Case: T sensitivity
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Low Collision Case: T sensitivityCIRS Test Seiff (1998)
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Low Collision Case: T sensitivityCIRS Test Seiff (1998)
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Other Heating Mechanisms?
Aerosol Heating at 3.4 micron NIR band?
Bellucci et al. (2009)
Gravity Wave Dissipation?
Young et al. (2005)
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Ave Heat/cool compare
• Slope• Thermosphere compare