Revisiting the radiative impact of dust on Mars using the LMD Global Climate Model

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The influence of radiatively active water ice clouds on the Martian climate (2012, methodology): “The “radiative” effective radius, rrad = rc (1 + nrad), where nrad is the effective variance of the lognormal distribution used by the radiative transfer scheme [Madeleine et al., 2011, equation 6].”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, methodology): “late Mars meteorology (e.g. Forget et al., 1998; Montmessin et al., 2004; Madeleine et al., 2011) and photochemistry (Lefèvre et al.”
Global climate modeling of the Martian water cycle with improved microphysics and radiatively active water ice clouds (2013, methodology): “The model used in this paper is the Mars general circulation model (GCM) developed at Laboratoire de Météorologie Dynamique (LMD) [ Forget et al. , 1999, 2011].”
The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity (2017, background): “…Martian atmosphere transports large amounts of dust, which interacts with solar and infrared radiation, regulating atmospheric and surface heating rates and thus influencing the Martian climate (Gierasch and Goody 1972; Kahn et al. 1992; Forget et al. 1999; Basu et al. 2004; Madeleine et al. 2011).”