Paleoclimate of Titan with hydrocarbon oceans and continents simulated by a global climate model

Tokano, Tetsuya

doi:10.1016/j.icarus.2022.115253

Cited by 1 publication

(1 citation statement)

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“…Early models (e.g., Tokano et al., 2001) used simplifications for calculating the latent heat fluxes/evaporation rate by ignoring atmospheric stability and assuming that z 0 m = z 0 v = z 0 h (Charnay and Lebonnois (2012) also make the same simplifications). Subsequent modeling efforts made improvements, by either incorporating stability effects (Lora et al., 2015; Tokano, 2009, 2023) or calculating z 0 m , z 0 v and z 0 h separately (Mitri et al., 2007), but neither groups of models included both effects together. Models based on WRF (e.g., Chatain et al., 2022; Newman et al., 2016; Rafkin & Soto, 2020) include both stability and roughness length ( z 0 m ≠ z 0 v ≠ z 0 h ) effects, but were based on older versions of WRF and therefore contain the stability approximations and limits described in Section 3.1.2.…”

Section: Previous Models Of Turbulent Fluxes Evaporation and Sublimat...mentioning

confidence: 99%

Turbulent Fluxes and Evaporation/Sublimation Rates on Earth, Mars, Titan, and Exoplanets

Khuller,

Clow

2024

JGR Planets

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Turbulent fluxes of heat, momentum, and humidity in the atmospheric boundary layer are pivotal to the evolution of geology, weather and climate, and the possibility of life. Here we extend recent advances in calculating these near‐surface turbulent fluxes in the Earth's atmospheric boundary layer to any terrestrial planetary body with an atmosphere. These improvements include: (a) incorporating Monin‐Obukhov similarity functions that encompass the entire range of atmospheric stability expected on terrestrial planetary bodies, (b) accounting for the additional shear associated with buoyant plumes under unstable conditions, (c) using surface renewal theory to calculate transfer rates within the interfacial layer adjacent to the surface, and (d) explicitly accounting for key humidity effects that become especially important when a volatile is more buoyant than the ambient gas (e.g., on Mars where H2O is lighter than CO2). We tested and validated our model using in situ data collected on Earth, Mars, and Titan under a wide range of atmospheric stability, pressure, and surface roughness conditions. The model shows up to 71% better agreement with measurements compared to methods commonly used on Mars for evaporation/sublimation. Compared to previous estimates for H2O ice on Mars, our model predicts up to 1.5–190x lower latent heat fluxes under stable atmospheric conditions (depending on the wind speed) and 1.78x higher latent heat fluxes under unstable conditions. Our results provide improved constraints on the stability of ice on Mars and will help determine whether ice can melt under present‐day conditions.

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Section: Previous Models Of Turbulent Fluxes Evaporation and Sublimat...mentioning

confidence: 99%

Turbulent Fluxes and Evaporation/Sublimation Rates on Earth, Mars, Titan, and Exoplanets

Khuller,

Clow

2024

JGR Planets

View full text Add to dashboard Cite

show abstract

Paleoclimate of Titan with hydrocarbon oceans and continents simulated by a global climate model

Cited by 1 publication

References 56 publications

Turbulent Fluxes and Evaporation/Sublimation Rates on Earth, Mars, Titan, and Exoplanets

Turbulent Fluxes and Evaporation/Sublimation Rates on Earth, Mars, Titan, and Exoplanets

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