Stephen W. Bougher University of Michigan (bougher@umich)

1. RESPONSE BY THE MARS AND JUPITER UPPER ATMOSPHERES TO EXTERNAL FORCINGS: CONTRASTS FROM TGCM SIMULATIONS Stephen W. Bougher University of Michigan (bougher@umich.edu) Hunter Waite and Tariq Majeed University of Michigan James R. Murphy New Mexico State University

2. Mars Atmospheric Regions and Processes

3. Mars Upper Atmosphere Sampling (Limited Spatially & Temporally) SpacecraftVertical Structures Viking 1 1 Viking 2 1 Pathfinder 1 MER A and B 2 Mars Global Surveyor Accelerometer 1600 Mars Odyssey Accelerometer 600

4. Keating et al., [2002]

5. Odyssey AM Temperatures (100-110 km)

6. Global Energy Budgets : Power in Watts

7. Jupiter Thermosphere-Ionosphere Processes

8. Auroral and Equatorial ThermosphericTemperature Profile Constraints for Jupiter(Waite and Lummerzheim, 2002) Galileo ASI : Seiff et al. 1998 Auroral discrete and diffuse profiles: Grodent et al 2001

9. MTGCM Input Parameters, Fields, and Domain • Domain : ~70-300 km; 33-levels; 5x5 ° resolution • Major Fields and Species : T, U, V, W, CO2, CO, O, N2 • Minor Species : O2, He, Ar, NO, N(4S) • Ions (PCE) : CO2+, O2+, O+, NO+, CO+, N2+ (<180 km) • Time step : 150 sec • Homopause Kzz = 1-2x 107 cm2/sec (at ~125 km) • Prescribed Heating efficiencies : EUV and FUV (22%) • Fast NLTE 15-µm cooling and IR heating formulations from M. Valverde 1-D NLTE code (Spain) • Simplified ion-neutral chemistry (Fox et al., 1995) • Empirical Ti and Te from Viking.

10. MGCM-MTGCM Simulations: Formulation, Parameters and Inputs: • Separate but coupled NASA Ames MGCM (0-90 km) and • NCAR/Michigan MTGCM (70-300 km) codes, linked across an interface at 1.32-microbars on 5x5º grid. • Fields passed upward at interface (T, U, V, Z) on 2-min time-step intervals. No downward coupling enabled. • MGCM-MTGCM captures upward propagating migrating and non-migrating tidal oscillations, as well as in-situ driven solar EUV-UV migrating tides in the thermosphere. • Odyssey: Ls = 270; F10.7 = 175; τ ~ 1.0 (TES-YR2) • MGS2 : Ls = 90 ; F10.7 = 130; τ ~ 0.4 (TES-YR1) • (Specified dust distributions. See next plots)

11. TES Dust Distributions (Ls = 90):Year #1 (1999-2000) LAT LON

12. TES Dust Distributions (Ls = 270):Year #2 (2001-2002) LAT LON

13. MTGCM Odyssey Case (Ls = 270):Temperatures at 200 km

14. MTGCM Odyssey Case (Ls = 270):Temperatures at 110 km

15. MTGCM Odyssey Case (Ls = 270):Densities at 110 km

16. MTGCM Odyssey Case (Ls = 270):SLT=17 Temperatures versus Latitude

17. MTGCM Odyssey Case (Ls = 270):SLT=3 Temperatures versus Latitude

18. Schematic Of Possible MarsWinter Polar Warming Process Subsidence Adiabatic Heating N Meridional Flow From Summer H. To Winter H. Winter Summer S

19. MTGCM Odyssey Case (Ls = 270):SLT = 3 Vertical Velocities versus Latitude

20. MTGCM Odyssey Case (Ls = 270):SLT = 3 Dynamical Heating versus Latitude

21. MTGCM MGS2 Case (Ls = 90):SLT = 15 Temperatures versus Latitude

22. MTGCM MGS2 Case (Ls = 90):SLT = 3 Temperatures versus Latitude

23. MTGCM Modeling Summary and Conclusions: • Coupled MGCM (0-90 km) and MTGCM (70-300 km) simulations capture the upward propagating migrating and non-migrating tides for Ls = 90 and 270 conditions appropriate to MGS2 and Odyssey period observations. Mars seasonal atmospheric expansion and contraction is also properly accommodated. • MTGCM winter polar temperatures near 100-130 km are markedly different between these seasons. Strong Northern polar warming features are reproduced, in accord with Odyssey observations. Weak Southern polar warming features are simulated, similar to MGS2 data. • A stronger inter-hemispheric circulation pattern during Northern winter (Ls = 270) yields larger dynamical heating in the Northern polar region. Seasonally varying TES dust distributions (and local vertical mixing) are likely responsible for these changing winds and the resulting polar heat balances at thermospheric altitudes.

24. JTGCM Input Parameters, Fields, and Domain • Domain : ~250-3000+ km; 39-levels; 5x5 ° resolution • Major Fields and Species : T, U, V, W, plus H2, He, H • Minor Species : CH4 , C2H2 and C2H6 (Gladstone) • Ions : H2+, H3+ (PCE), H+ (dynamical) • Homopause Kzz = 5 x 106 cm2/sec (at ~4.5-microbars) • Heating : 3-component auroral particle (~110 ergs/cm2.s) and Joule heating (~30-40%) [c.f. Grodent et al., 2001] • NLTE 3-4-µm cooling from H3+ (Miller) and hydrocarbon IR cooling (Drossart formulation) from CH4 and C2H2 • Simplified ion-neutral chemistry (Waite, Cravens) • Voyager-1 ion convection pattern (Evitar & Barbosa 1984) • VIP4 magnetic field model to map Ui and Vi to high lats.

25. Profile of JTGCM Auroral Oval Heating(Grodent et al.,2001)

26. JTGCM Ion Convection Pattern(Ui + Vi Vectors)

27. JTGCM ~0.1 µbar: Auroral + Joule (40%)Temperatures and Winds

28. JTGCM ~0.1 µbar: Auroral + Joule (40%)Atomic Hydrogen

29. JTGCM ZM: Auroral + Joule (40%)Temperatures

30. JTGCM ZM: Auroral + Joule (40%)Zonal Winds

31. JTGCM ZM: Auroral + Joule (40%)Meridional Winds

32. JTGCM ZM: Auroral + Joule (40%)Adiabatic Heating (eV/cm3.sec)

33. JTGCM ZM: Auroral + Joule (40%)Atomic Hydrogen

34. JTGCM Modeling Summary and Conclusions: • Reasonable auroral temperatures and strong winds simulated with combined particle plus Joule heating (30-40%); JTGCM temperatures at the equator approaching Galileo ASI values. • H3+ cooling & dynamics dampen impact of Joule heating • Strong winds (~1.0 km/sec) have a significant role in re- distributing high latitude heat & H-atoms toward equator. • JTGCM dynamical terms dominate equatorial heating. • Scaling required (30-40%) to reduce Joule heating to bring calculated temperatures in line with avail. observations. Uncertainty in magnetospheric forcing (Ui & Vi) is likely. • 40+ JTGCM rotations required to achieve steady solutions. • Much different thermal and wind patterns than Mars (solar EUV/UV versus particle/Joule forcing).