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

<div>Repository: Turbulent Fluxes and Evaporation/Sublimation Rates on Earth, Mars, Titan, and Exoplanets</div> <div>Khuller &amp; Clow (2024)</div> <div>&nbsp;</div> <div>Contents:</div> <div>&nbsp;</div> <div>1. Comparison of Khuller &amp; Clow model, Dundas &amp; Byrne (2010) model vs. turbulent fluxes measured by Fitzpatrick et al. (2017)</div> <div>a) Measured fluxes</div> <div>i) Measured_Abs_LE_Fitzpatrick: Absolute value of measured latent heat fluxes in W/m^2</div> <div>ii) Measured_Abs_SH_Fitzpatrick: Absolute value of measured sensible heat fluxes in W/m^2</div> <div>b) Modeled fluxes</div> <div>i) Modeled_DB_Abs_LE_Fitzpatrick: Absolute value of Dundas &amp; Byrne (2010) modeled latent heat fluxes in W/m^2</div> <div>ii) Modeled_DB_Abs_SH_Fitzpatrick: Absolute value of Dundas &amp; Byrne (2010) modeled sensible heat fluxes in W/m^2</div> <div>iii) Modeled_KC_Abs_LE_Fitzpatrick: Absolute value of Khuller &amp; Clow modeled latent heat fluxes in W/m^2</div> <div>iv) Modeled_KC_Abs_SH_Fitzpatrick: Absolute value of Khuller &amp; Clow modeled sensible heat fluxes in W/m^2</div> <div>&nbsp;</div> <div>2. Comparison of Khuller &amp; Clow model, Dundas &amp; Byrne (2010) model vs. turbulent fluxes measured by Fairall et al. (1996); Fairall et al. (2003)</div> <div>a) Measured fluxes</div> <div>i) Measured_Abs_LE_COARE: Absolute value of measured latent heat fluxes in W/m^2</div> <div>ii) Measured_Abs_SH_COARE: Absolute value of measured sensible heat fluxes in W/m^2</div> <div>b) Modeled luxes</div> <div>i) Modeled_DB_Abs_LE_COARE: Absolute value of Dundas &amp; Byrne (2010) modeled latent heat fluxes in W/m^2</div> <div>ii) Modeled_DB_Abs_SH_COARE: Absolute value of Dundas &amp; Byrne (2010) modeled sensible heat fluxes in W/m^2</div> <div>iii) Modeled_KC_Abs_LE_COARE: Absolute value of Khuller &amp; Clow modeled latent heat fluxes in W/m^2</div> <div>iv) Modeled_KC_Abs_SH_COARE: Absolute value of Khuller &amp; Clow modeled sensible heat fluxes in W/m^2</div> <div>&nbsp;</div> <div>3. Comparison of Khuller &amp; Clow model, Dundas &amp; Byrne (2010) model vs. ice sublimation rates measured by Clow et al. (1988)</div> <div>a) Measured sublimation rates</div> <div>i) Measured_dzdt_Clow: Measured sublimation rates in mm/day</div> <div>&nbsp;</div> <div>b) Modeled sublimation rates</div> <div>i) Modeled_DB_dzdt_Clow: Dundas &amp; Byrne (2010) modeled sublimation rates in mm/day</div> <div>ii) Modeled_KC_dzdt_Clow: Khuller &amp; Clow modeled sublimation rates in mm/day</div> <div>&nbsp;</div> <div>4. Comparison of Khuller &amp; Clow model, Dundas &amp; Byrne (2010) model vs. ice sublimation rate measured by Douglas &amp; Mellon (2019)</div> <div>a) Roughness Lengths used</div> <div>i) z0_DM: Roughness lengths used in cm</div> <div>&nbsp;</div> <div>b) Modeled Sublimation Rates</div> <div>i) Modeled_DB_dzdt_u_001_DM: Dundas &amp; Byrne (2010) modeled sublimation rates for u = 0.01 m/s in mm/day</div> <div>ii) Modeled_DB_dzdt_u_005_DM: Dundas &amp; Byrne (2010) modeled sublimation rates for u = 0.05 m/s in mm/day</div> <div>iii) Modeled_DB_dzdt_u_010_DM: Dundas &amp; Byrne (2010) modeled sublimation rates for u = 0.10 m/s in mm/day</div> <div>iv) Modeled_DB_dzdt_u_015_DM: Dundas &amp; Byrne (2010) modeled sublimation rates for u = 0.15 m/s in mm/day</div> <div>v) Modeled_KC_dzdt_u_001_DM: Khuller &amp; Clow modeled sublimation rates for u = 0.01 m/s in mm/day</div> <div>vi) Modeled_KC_dzdt_u_005_DM: Khuller &amp; Clow modeled sublimation rates for u = 0.05 m/s in mm/day</div> <div>vii) Modeled_KC_dzdt_u_010_DM: Khuller &amp; Clow modeled sublimation rates for u = 0.10 m/s in mm/day</div> <div>viii) Modeled_KC_dzdt_u_015_DM: Khuller &amp; Clow modeled sublimation rates for u = 0.15 m/s in mm/day</div> <div>&nbsp;</div> <div>5. Comparison of Khuller &amp; Clow model, Dundas &amp; Byrne (2010) model vs. net ice sublimation inferred at Mars Phoenix landing site, by Smith et al. (2009)</div> <div>a) Parameters used</div> <div>i) z0_PHX: Roughness lengths used in cm</div> <div>ii) u_PHX: Wind speeds used in m/s</div> <div>iii) deltatheta1_PHX: Delta-surface temperatures used in K</div> <div>&nbsp;</div> <div>b) Modeled net sublimation</div> <div>i) Modeled_DB_deltatheta1_sensitivity_PHX: Dundas &amp; Byrne (2010) modeled sublimation rates for varied delta-surface temperatures in cm</div> <div>ii) Modeled_DB_u_sensitivity_PHX: Dundas &amp; Byrne (2010) modeled sublimation rates for varied wind speeds in cm</div> <div>iii) Modeled_DB_z0_sensitivity_PHX: Dundas &amp; Byrne (2010) modeled sublimation rates for varied roughness lengths in cm</div> <div>&nbsp;</div> <div>6. Modeled vertical profiles of temperature and wind speed compared to Huygens probe measurements (Fulchignoni et al., 2005)</div> <div>i) Modeled_theta_Huygens_u_0_02: Temperature profile using 10-m wind speed of 0.02 m/s, in K</div> <div>ii) Modeled_theta_Huygens_u_1: Temperature profile using 10-m wind speed of 1 m/s, in K</div> <div>iii) Modeled_Z_Huygens: Altitude profile in m</div> <div>&nbsp;</div> <div>7. Modeled effect of various parameters on Mars ice sublimation rates</div> <div>a) Input data ranges</div> <div>i) Modeled_Mars_Theta2_warm: 3-m air temperatures for warm cases in K</div> <div>ii) Modeled_Mars_Theta2_cold: 3-m air temperatures for cold cases in K</div> <div>iii) Modeled_Mars_z0_range: Roughness lengths in cm</div> <div>iv) Modeled_Mars_P_range: Surface air pressure values in mbar</div> <div>v) Modeled_Mars_beta_range: Dimensionless gustiness parameters</div> <div>&nbsp;</div> <div>b) Modeled sublimation rates from Dundas &amp; Byrne (2010) model</div> <div>i) Modeled_DB_dzdt_Mars_warm_low_wind: Sublimation rate in cm/Mars yr using 0.5 m/s wind speed at 3-m</div> <div>ii) Modeled_DB_dzdt_Mars_warm_high_wind: Sublimation rate in cm/Mars yr using 15 m/s wind speed at 3-m</div> <div>iii) Modeled_DB_dzdt_Mars_cold_low_wind: Sublimation rate in cm/Mars yr using 0.5 m/s wind speed at 3-m</div> <div>iv) Modeled_DB_dzdt_Mars_cold_high_wind: Sublimation rate in cm/Mars yr using 15 m/s wind speed at 3-m</div> <div>v) Modeled_DB_dzdt_Mars_warm_z0_var: Sublimation rate in cm/Mars yr using range of z0 values</div> <div>vi) Modeled_DB_dzdt_Mars_cold_z0_var: Sublimation rate in cm/Mars yr using range of z0 values</div> <div>vii) Modeled_DB_dzdt_Mars_warm_P_var: Sublimation rate in cm/Mars yr using range of P values</div> <div>viii) Modeled_DB_dzdt_Mars_cold_P_var: Sublimation rate in cm/Mars yr using range of P values</div> <div>xi) Modeled_DB_dzdt_Mars_warm_beta_var: Sublimation rate in cm/Mars yr using range of beta values</div> <div>x) Modeled_DB_dzdt_Mars_cold_beta_var: Sublimation rate in cm/Mars yr using range of beta values</div> <div>&nbsp;</div> <div>c) Modeled sublimation rates from Khuller &amp; Clow model</div> <div>i) Modeled_KC_dzdt_Mars_warm_low_wind: Sublimation rate in cm/Mars yr using 0.5 m/s wind speed at 3-m</div> <div>ii) Modeled_KC_dzdt_Mars_warm_high_wind: Sublimation rate in cm/Mars yr using 15 m/s wind speed at 3-m</div> <div>iii) Modeled_KC_dzdt_Mars_cold_low_wind: Sublimation rate in cm/Mars yr using 0.5 m/s wind speed at 3-m</div> <div>iv) Modeled_KC_dzdt_Mars_cold_high_wind: Sublimation rate in cm/Mars yr using 15 m/s wind speed at 3-m</div> <div>v) Modeled_KC_dzdt_Mars_warm_z0_var: Sublimation rate in cm/Mars yr using range of z0 values</div> <div>vi) Modeled_KC_dzdt_Mars_cold_z0_var: Sublimation rate in cm/Mars yr using range of z0 values</div> <div>vii) Modeled_KC_dzdt_Mars_warm_P_var: Sublimation rate in cm/Mars yr using range of P values</div> <div>viii) Modeled_KC_dzdt_Mars_cold_P_var: Sublimation rate in cm/Mars yr using range of P values</div> <div>xi) Modeled_KC_dzdt_Mars_warm_beta_var: Sublimation rate in cm/Mars yr using range of beta values</div> <div>x) Modeled_KC_dzdt_Mars_cold_beta_var: Sublimation rate in cm/Mars yr using range of beta values</div> <div>&nbsp;</div> <div>d) Modeled latent heat fluxes from Dundas &amp; Byrne (2010) model</div> <div>i) Modeled_DB_LE_Mars_warm_low_wind: Latent heat flux in W/m^2 using 0.5 m/s wind speed at 3-m</div> <div>ii) Modeled_DB_LE_Mars_warm_high_wind: Latent heat flux in W/m^2 using 15 m/s wind speed at 3-m</div> <div>iii) Modeled_DB_LE_Mars_cold_low_wind: Latent heat flux in W/m^2 using 0.5 m/s wind speed at 3-m</div> <div>iv) Modeled_DB_LE_Mars_cold_high_wind: Latent heat flux in W/m^2 using 15 m/s wind speed at 3-m</div> <div>v) Modeled_DB_LE_Mars_warm_z0_var: Latent heat flux in W/m^2 using range of z0 values</div> <div>vi) Modeled_DB_LE_Mars_cold_z0_var: Latent heat flux in W/m^2 using range of z0 values</div> <div>vii) Modeled_DB_LE_Mars_warm_P_var: Latent heat flux in W/m^2 using range of P values</div> <div>viii) Modeled_DB_LE_Mars_cold_P_var: Latent heat flux in W/m^2 using range of P values</div> <div>xi) Modeled_DB_LE_Mars_warm_beta_var: Latent heat flux in W/m^2 using range of beta values</div> <div>x) Modeled_DB_LE_Mars_cold_beta_var: Latent heat flux in W/m^2 using range of beta values</div> <div>&nbsp;</div> <div>e) Modeled latent heat fluxes from Khuller &amp; Clow model</div> <div>i) Modeled_KC_LE_Mars_warm_low_wind: Latent heat flux in W/m^2 using 0.5 m/s wind speed at 3-m</div> <div>ii) Modeled_KC_LE_Mars_warm_high_wind: Latent heat flux in W/m^2 using 15 m/s wind speed at 3-m</div> <div>iii) Modeled_KC_LE_Mars_cold_low_wind: Latent heat flux in W/m^2 using 0.5 m/s wind speed at 3-m</div> <div>iv) Modeled_KC_LE_Mars_cold_high_wind: Latent heat flux in W/m^2 using 15 m/s wind speed at 3-m</div> <div>v) Modeled_KC_LE_Mars_warm_z0_var: Latent heat flux in W/m^2 using range of z0 values</div> <div>vi) Modeled_KC_LE_Mars_cold_z0_var: Latent heat flux in W/m^2 using range of z0 values</div> <div>vii) Modeled_KC_LE_Mars_warm_P_var: Latent heat flux in W/m^2 using range of P values</div> <div>viii) Modeled_KC_LE_Mars_cold_P_var: Latent heat flux in W/m^2 using range of P values</div> <div>xi) Modeled_KC_LE_Mars_warm_beta_var: Latent heat flux in W/m^2 using range of beta values</div> <div>x) Modeled_KC_LE_Mars_cold_beta_var: Latent heat flux in W/m^2 using range of beta values</div>