Apr 19, 2023 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

Apr 19, 2023 2

Mars Atmospheric Regions and Processes

Apr 19, 2023 3

Spacecraft Vertical Structures

Viking 1 1

Viking 2 1

Pathfinder 1

MER A and B 2

Mars Global Surveyor Accelerometer 1600

Mars Odyssey Accelerometer 600

Mars Upper Atmosphere Sampling (Limited Spatially & Temporally)

Apr 19, 2023 4

Keating et al., [2002]

Apr 19, 2023 5

Odyssey AM Temperatures (100-110 km)

Apr 19, 2023 6

Global Energy Budgets : Power in Watts

PLANET EUV PARTICLE JOULE TOTAL

Earth

(quiet)

~5x1011 -----

-----

~5x1011

Earth

(storm)

~5x1011 ~1-2x1010 ~7.0x1010 ~5-6x1011

Mars ~2.5x1010 ----- ----- ~2.5x1010

Jupiter ~ 8x1011 1.0x1014 >1.0x1014 >2.0x1014

Apr 19, 2023 7

Jupiter Thermosphere-Ionosphere Processes

ENERGYDEPOSITION

GRODEN T ET AL. [2001]

MAGNETIC FIELD

V1P4 MODEL

J. CONNERNEY [1998]

Case 1Case 2Case 3Future

WAVE PROPAGATION(GW OR TIDES)

ION DRIFT(NON-COROTATING)

(UI - UN)

IONDRAG

JOULEHEATING (U I - UN)

NEUTRALTRANSPORT

AFFECTING(H, H

2, He)

(H2 (v=1, 2, 3, 4)

ADVECTION

PRESSUREGRID

NEUTRAL HEATING

IONCHEMISTRY

PH+ (e, h)

IONOSPHERE W/DIFFUSION

H+, H3+

PH2+ (e,h)

IONOSPHERE INPCE

H2+, CH5

+, C2H5+

JovianAURORA

Symmetric in |||or

Asymmetry in |||

SIIIAURORAL

LTSOLAR

EUV

NEUTRAL GASHEATING

EQUATION(Q vs. ColH2

)

HYDROCARBONCOOLING (7-15 µm)

COOL-TO-SPACEBY C2H2, CH4, C2H6

DROSSART et al. [1993]

HYDROCARBONMINOR SPECIES

C2H2, CH4, C2H6(PRESCRIBED)

WAVE PROPAGATION(GW OR TIDES)

ColH2

MAJOR SPECIESDIFFUSION

MINOR SPECIESDIFFUSION

(H, H2, He) (H2, (v = 1, 2, 3, 4)

PH PH2(e,h)(e,h)

nn

LT DEPENDENTJOVIAN

SOLAR EUV

Jupiter TGCM

ION-NEUTRALCHEMISTRY

ONLYBELOW~1 µbar

GLADSTO NEet al. [1996]

L 25 (PRESCRIBED)

EVIATOR BARBOSA [1984]

ROBLE &RIDLEY [1987]

Apr 19, 2023 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

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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.

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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)

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TES Dust Distributions (Ls = 90):Year #1 (1999-2000)

LAT

LON

Apr 19, 2023 12

TES Dust Distributions (Ls = 270):Year #2 (2001-2002)

LAT

LON

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

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

Apr 19, 2023 15

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

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

Apr 19, 2023 17

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

Apr 19, 2023 18

Summer

Winter

Subsidence

Adiabatic Heating

N

S

Meridional Flow

From Summer H.

To Winter H.

Schematic Of Possible MarsWinter Polar Warming Process

Apr 19, 2023 19

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

Apr 19, 2023 20

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

Apr 19, 2023 21

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

Apr 19, 2023 22

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

Apr 19, 2023 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.

Apr 19, 2023 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.

Apr 19, 2023 25

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

Apr 19, 2023 26

JTGCM Ion Convection Pattern(Ui + Vi Vectors)

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

Apr 19, 2023 28

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

Apr 19, 2023 29

JTGCM ZM: Auroral + Joule (40%)Temperatures

Apr 19, 2023 30

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

Apr 19, 2023 31

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

Apr 19, 2023 32

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

Apr 19, 2023 33

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

Apr 19, 2023 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).