Investigating Titan’s Surface-Atmosphere Interactions with a General Circulation Model Claire E. Newman, Mark I. Richardson and Yuan Lian Ashima Research, Pasadena, CA

Why a General Circulation Model (GCM)? Atmospheric processes involve non-linear interactions and feedbacks => related phenomena can be complex, and hard to predict using theory or simple models To fully understand surface phenomena linked to the atmosphere, we must model the full 3D circulation Titan GCMs have uncertainties in physical processes / parameters (e.g., strength of sub-grid scale mixing) and boundary conditions (e.g., surface properties) We can us e comparison between GCM predictions and observations to constrain and refine the GCM, and thus improve our knowledge and understanding of real Titan

Surface Phenomena Examined Here 1.The observed seasonal variation in surface methane, and estimated evaporation/precipitation rates – These depend on atmospheric transport, cloud processes, and the atmosphere-surface exchange of heat and methane – We use a simple methane cycle scheme in our GCM, TitanWRF: Surface evaporation Atmospheric transport (advection and mixing) Atmospheric condensation followed by instant deposition [unless sub-saturated layers exist below, in which case sufficient condensate is re-evaporated to saturate them] Surface precipitation of any condensate that remains Latent heating effects and finite surface methane abundances

Shortwave heating into the surface as a function of latitude and time of year (L s ) Newman et al. Icarus 2013, in review

Titan has a tilt, timing of perihelion, and seasons that are in many ways similar to Earth Newman et al. Icarus 2013, in review Present day perihelion

Infinite surface methane No latent heating effects

Newman et al. Icarus 2013, in review Surface temperature as a function of latitude and time of year

Newman et al. Icarus 2013, in review Northern spring (L s =0-30°) Northern summer (L s =90-120°) Northern autumn (L s = °) Northern winter (L s = °) Tropospheric mass streamfunctions

Newman et al. Icarus 2013, in review Northern spring (L s =0-30°) Northern summer (L s =90-120°) Northern autumn (L s = °) Northern winter (L s = °) Tropospheric mass streamfunctions

Newman et al. Icarus 2013, in review Peak upwelling speed in the troposphere

Newman et al. Icarus 2013, in review Peak upwelling speed in the troposphere Peak low and mid-latitude upwelling follows the approximate path of the Inter- tropical Convergence Zone (ITCZ) where main Hadley cell branches converge and rise

Newman et al. Icarus 2013, in review Peak upwelling speed in the troposphere Even stronger upwelling at high latitudes in late winter through into early summer

Newman et al. Icarus 2013, in review Peak upwelling speed in the troposphere Even stronger upwelling at high latitudes in late winter through into early summer Polar cells producing strong high latitude upwelling are greatly enhanced in TitanWRF with strong stratospheric superrotation

Newman et al. Icarus 2013, in review Meridional divergence in the lowest layer

Newman et al. Icarus 2013, in review Meridional divergence in the lowest layer

Newman et al. Icarus 2013, in review Methane distribution in the troposphere Column abundance (in kg m -2 )Lowest layer mole fraction

Newman et al. Icarus 2013, in review Methane distribution in the troposphere Column abundance (in kg m -2 )Lowest layer mole fraction Strong upwelling in late spring depletes near-surface methane

Newman et al. Icarus 2013, in review 3 Titan years of evaporation and precipitation Evaporation rate (in mm per Earth hour) Precipitation rate (in mm per Earth hour)

Newman et al. Icarus 2013, in review 3 Titan years of evaporation and precipitation Evaporation rate (in mm per Earth hour) Precipitation rate (in mm per Earth hour) Peak evaporation in late spring through early summer

Newman et al. Icarus 2013, in review Resultant change in surface methane over time Change (in mm) from value at start of simulation (~6 Titan years earlier)

Infinite surface methane simulations indicated that low and mid-latitudes tended to dry out, while high latitudes tended to gain methane [as in Mitchell 2008] Re-ran simulation starting with finite, globally- uniform surface methane cover equivalent to ~11m depth

Finite surface methane Still no latent heating effects Results shown for years after simulation reached steady state => no long-term change in surface methane distribution

Newman et al. Icarus 2013, in review 3 Titan years of evaporation and precipitation Evaporation rate (in mm per Earth hour) Precipitation rate (in mm per Earth hour)

Newman et al. Icarus 2013, in review 3 Titan years of evaporation and precipitation Evaporation rate (in mm per Earth hour) Precipitation rate (in mm per Earth hour) Condensation (cloud) still occurs in low and mid-latitudes, but all the condensate re-evaporates before reaching the surface

Newman et al. Icarus 2013, in review 3 Titan years of surface methane (in mm)

Newman et al. Icarus 2013, in review The steady state surface methane distribution Surface methane changes over the entire simulation Titan years from start Green line shows surface methane decrease equatorward of 60° Red line shows surface methane increase north of 60° N Blue line shows surface methane increase south of 60° S In steady state, north pole has ~50% more methane than south

Newman et al. Icarus 2013, in review The steady state surface methane distribution Evaporation, precipitation and net change over the last 3 Titan years Planetocentric solar longitude, L s (deg) Evaporation N of 60° N Precipitation N of 60° N Net N of 60° N Evaporation S of 60° S Precipitation S of 60° S Net S of 60° S

Results did not include evaporative cooling at the surface, or evaporative cooling / condensational heating in the atmosphere – i.e., there were no latent heat effects

Finite surface methane And latent heating effects

Newman et al. Icarus 2013, in review 3 Titan years of evaporation and precipitation Evaporation rate (in mm per Earth hour) Precipitation rate (in mm per Earth hour)

Newman et al. Icarus 2013, in review 3 Titan years of condensation and precipitation Column-integrated methane condensate (in kg m -2 over 8 Titan days) Precipitation rate (in mm per Earth hour)

Newman et al. Icarus 2013, in review 3 Titan years of condensation and precipitation Column-integrated methane condensate (in kg m -2 over 8 Titan days) Precipitation rate (in mm per Earth hour) * * * * ** Times and locations of rainfall inferred from ISS observations * * * * **

Newman et al. Icarus 2013, in review Peak upwelling speed in the troposphere

Newman et al. Icarus 2013, in review 3 Titan years of condensation and precipitation Column-integrated methane condensate (in kg m -2 over 8 Titan days) Precipitation rate (in mm per Earth hour) Only the strongest upwelling and condensation events result in surface precipitation

Newman et al. Icarus 2013, in review 3 Titan years of surface methane (in mm)

Newman et al. Icarus 2013, in review Surface temperatures and evaporative cooling No evaporative coolingWith evaporative cooling Evaporative cooling + higher surface thermal inertia Including latent heating modifies the surface heat balance and produces much larger T surf gradients (and lower mean T surf ) than observed The (currently uniform) surface thermal inertia is one of many parameters that impact this => may perhaps be constrained by comparison between modeled and observed T surf

Newman et al. Icarus 2013, in review Impact of reversing timing of perihelion Cumulative mass change (kg) Present day timing (just after southern summer solstice) ‘Reversed’ timing (just after northern summer solstice) Green line shows surface methane decrease equatorward of 60° Red line shows surface methane increase north of 60° N Blue line shows surface methane increase south of 60° S North gains relative to south South gains relative to north

Methane cycle conclusions TitanWRF shows partial match to several aspects, including evaporation rates and cloud and rainfall observations We predict more surface methane in northern than in southern high latitudes, with this reversed when perihelion is switched from southern to northern summer In TitanWRF, this is basically due to more high latitude evaporation during the warmer (perihelion) summer Ongoing work involves the improved treatment of cloud physics and methane’s behavior at/below the surface, before using observations to constrain the model further

Surface Phenomena Examined Here 1.The observed seasonal variation in surface methane and estimated evaporation/precipitation rates 2.Observed dune characteristics – Dunes are the time-integrated result of a non- linear, threshold- dependent, wind-driven process (saltation) – We predict dune orientations using the Gross Bedform-Normal Transport (GBNT) approach – We predict the direction of dune migration / motion using the net (resultant) sand transport direction over a Titan year

Predicting Titan dune characteristics Expect overall direction of motion / migration to be roughly the resultant transport direction R R at any given time depends on – the choice of threshold wind stress for saltation to occur, and – the sand flux formulation R is then summed over a full Titan year to give the long-term resultant transport direction Predicting direction of dune motion in a given wind field:

See Rubin & Hunter, Science, 1987 for a full description of the GBNT approach Basic concept: dunes form due to sand transport in both directions across bedform => Dunes will be oriented such that the total transport across the dune crest is maximized Total transport = |B|+|C| summed over entire year = Gross Bedform-Normal Transport Also depends on threshold and sand flux formulation B C Predicting dune orientations in a given wind field: Predicting Titan dune characteristics

Dune crest orientation & resultant transport direction predicted for a threshold of 0.014Pa and no topography Very little eastward resultant transport (very few eastward- pointing black arrows) equatorward of 25° => Almost all dune motion expected to be toward the west

But if we include topography into TitanWRF… An extrapolated ‘plausible’ global topography map based on Cassini Radar data (pre Lorenz et al.’s 2013 map, which we will use next) [data provided by Karl Mitchell and Jeff Andrews-Hanna]

30°N 30°S 0° from Lorenz and Radebaugh

Dune conclusions Interaction between dunes and topographic obstacles hypothesized to imply largely eastward dune movement Topography + higher thresholds can produce more predicted eastward resultant transport However, predicted dune crest orientations are less consistent with observations for these conditions Predicted dune morphology (based on relationship between predicted orientation and resultant transport direction) is also less consistent with dunes observed