1. Radiative Modeling of the Atmosphere of Neptune Y. Yung 1, X. Zhang 1, R. Shia 1, M. Liang 2, G. Orton 3, A. Mainzer 3 and M. Burgdorf 4 1 Caltech, USA 2 Academia Sinica, Taiwan 3 JPL, USA 4 John Moores University, UK

2. Motivation 29 AU Sptizer

3. -Classic P Q R branches from acetylene emission centered at 729 cm -1 -Strong methane absorption into continuum along with some strong emission lines at 1534 cm -1 and 1306 cm -1 -Reflected sunlight dominates frequencies higher than ~1400 cm -1 -All emission lines sitting on top of H 2 collision induced continuum Acetylene (C 2 H 2 ) Ethane (C 2 H 6 ) Ethylene (C 2 H 4 ) Methane (CH 4 ) IRS Cycle 2 Spectrum

4. Chemical Transport Modeling

6. Atmospheric Structure

7. Radiance

8. Heating/Cooling Rate

9. Heating Rate Sensitivity

10. Cooling Rate Sensitivity

12. Aerosol (tholin)? Cross Section: Coefficients n &k from Khare et.al.[1984]

13. Aerosol Profile –Above 1 mbar –Constant number density Cross Section r = 125 A

14. Heating Rate with Aerosol 3

15. Cooling Rate with Aerosol

16. Conclusion Spitzer observations provide new constraints for chemical and radiative processes in the atmosphere of Neptune Imbalance in heating and cooling suggest, most likely, the existence of aerosols in the middle-upper atmosphere

17. Not Used

18. Eddy Sensitivity (… 5x eddy --- 0.1x eddy)

19. Cooling Rate with Aerosol(2) the blue line bottom is heating! So cannot plot out, maybe we shall not show this line this time

20. Radiace Sensitivity

21. Radiative Transfer Model Shortwave Heating: Solar energy absorption by CH4 Radiance and Longwave Cooling : Thermal radiation of atmosphere and absorption by species Heating 1000-50000 cm -1 Cooling 100-2000cm -1