1. Oxygen: Stratosphere, Mesosphere and Thermosphere Part-3 Chemical Rate Equations Ozone Density vs. Altitude Stratospheric Heating Thermal Conductivity Thermospheric Structure Temperature Structure on other planets

2. n1n1 Rate Equations for Oxygen Chemistry

3. Introduce Ozone

4. Ozone continued

5. Dependence on z Remember: J 2 (z) = J 2 o exp[ -  2 (z)/  ] where  = cos   2 (z) =  abs  o  n 2 dz n 2 (z)  0.21 n M n M (z) = n M (0) exp(-z/H) in mixed region J 3 (z) = J 3 o exp[ -  3 (z)/  ] For  3 (z) need n 3 (z) which we are solving for.

6. 10 -9 /s 10 -2 /s 20 80 40 80 mesopause … stratopause Tropopaus n 3, T J2J2 J3J3 n3n3 T High z J 2 /J 3 =constant ~10 -7 Low z J 2 /J 3 --> 0

7. Densities of O 2,O 3 and O C+H To get right: need some diffusive separation in the upper regions At night: J 2 (z) and J 3 (z) --> 0 ‘slow’ reactions become important High z n 1  1/n 2 1/2 n 3  n 2 3/2 Log 10 n(mol/cc)

8. Temperature vs. Altitude Earth’s Atmosphere Stratospheric Heating peak and Ozone Peak related J 3 (z) = J 3 o exp[ -  3 (z)/  ] dT/dt  h 3 J 3 (z) n 3 (z)

9. Summary

10. EUV Thermal conduction mesopause I R Thermosphere + Ionosphere Z 130km 80km

11. F s (z) zz  T +  TT zz

12. Thermosphere Continued

13. Thermosphere T Structure T m is where the heat conducted downward is radiated to space Relation to our old T e ?

14. Thermosphere Structure (Cont)

15. y(x) =  o x { [1-exp(-x’)]/x’} dx’ x   (z); y   T 7/4 Integral for thermosphere model

16. Temperature vs. Altitude Earth’s Atmosphere Rise in T in Thermosphere due to EUV Absorption and Thermal Conduction to Mesopause These are averages Tropopause is higher and hotter Near equator ~16-18km and ~ 10km near poles Drives high altitude horizontal flow Jets ~10km to be close to stratosphere and avoid turbulence

17. A result of Horizontal Transport Ozone column density in ppm Tropopause higher near equator and lower in T Drives upper atmospheric flows Will treat horizontal transport soon

18. Noctilucent Clouds (night shining clouds, ~85km, ice grains) (polar mesospheric clouds) over a lake in northern Sweden Possibly produced by climate change and space shuttle exhaust Polar Stratospheric (nacreous)Clouds ~15-25km: ice, nitric and sulfuric acids Implicated in ozone holes

19. Polar Stratospheric (nacreous)Clouds ~15-25km: ice, nitric and sulfuric acids Implicated in ozone holes Polar Stratospheric (nacreous)Clouds

20. Earth’s Thermal Structure dePL Thermosphere T depends on Solar Activity

21. Venus Atmosphere dePL Cloud Tops --> T e CO2 even at high altitudes --> cooling Slow Rotation 1 year = 2 days (retrograde due to thickatmosphere and tidal forces?)

22. Mars Atmosphere dePL T e at Surface Dust absorbs h and changes the lapse rate Thermosphere strongly dependent on solar activity

23. Photo-chemistry Venus + Mars CO 2 + h  CO + O (1) CO+O+M  CO 2 + M (2) (2) is very slow at Mars (density of M Is very small): Expect considerable CO, especially so as free O oxidize surface (iron oxide) But there is a small amount of H2O H 2 O + h  OH + H (3) CO + OH  CO 2 + H (4) On Venus CO --> CO 2 may be aided by sulfur + chlorine species

24. Titan’s Atmosphere dePL Stratosphere/ mesosphere due to absorption in hydrocarbon haze CH 4 + h -> CH 3 +H(CH f +H 2 ) React to form C n H m and H 2 escapes. Thermosphere subject to particles from Saturn’s magnetosphere

25. Giant Planets dePL Internal heat sources Adiabatic lapse rate down to liquid metal hydrogen Jupiter has evidence of a stratosphere and a mesosphere

26. Typically troposphere (Lower, Convective) Mesosphere [ Stratosphere ] (Middle, Radiative) Thermosphere (Upper, Conductive) Exosphere (Escape) Venus Temperature Lapse,   d Tropopause at cloud layer (~ 70 km) T e ~ Top of cloud layer Thermosphere (Cryosphere) T d ~ 300 km (CO 2 at high altitudes) T n ~ 100 km (Slow rotation 1yr  2 days) Mars Temperature Lapse    d (Strong Day / Night Variations: Dust    d Mesosphere T < Te (CO 2 cooling) Thermosphere like Mesosphere (Strongly affect by solar activity) Titan Temperature Lapse    d Stratosphere (Haze Layer) Mesosphere (Cooler to space) Thermosphere (Solar UV + Energetic Particles from Magnetosphere Cooled by HCN, Slow Rotations) Grant Planets Internal heat source comparable to solar Tropopause ~ 0.1 bar,  ~  d, Temperature + pressure increase to about 2M bar so phase change to a liquid (metallic) state (4x10 4 km) and a metallic core (3x10 4 K) (1x10 4 km) (Jupiter) Mesosphere (stratosphere)  0.001 bar Hydrocarbon coolants Thermosphere (Solar EUV) Atmosphere Thermal Structure: Summary

27. #3 Summary Things you should know Earth’s thermal structure Rate equations Oxygen reactions Ozone layer Stratosphere Mesosphere Thermosphere Thermal conductivity Heat flux