Auxiliary Material for
'Influence of Water Ice Clouds on Nighttime Tropical Temperature Structure as Seen by the
Mars Climate Sounder'
R. John Wilson (1), Scott D. Guzewich (2)
(1) NOAA/Geophysical Fluid Dynamics Laboratory, Princeton, NJ, USA
(2) NASA/Goddard Spaceflight Center, Code 693, Greenbelt, MD, USA
Geophysical Research Letters, 2014
Introduction
The files 2014GL060086-fs01.eps to 2014GL060086-fs03.eps contain the supplementary figures
S1, S2 and S3, as referenced in the article.
Figures S1 and S3 include simulation results derived from the the Mars Global Climate Model
developed at the Laboratoire de Meteorologie Dynamique (LMD)[Madeleine et al., 2012;
Navarro et al., 2014]. Model output is organized into a database of climatological meteorological
fields [Millour et al., 2014]. The database is publicly available at http://wwwmars.lmd.jussieu.fr.
Figures
2014GL060086-fs01.eps: The seasonal evolution of nighttime surface temperatures within a
4°×4° box in the Tharsis region centered at 260°E, 0°N. Data points include MCS 32 µm
temperatures for MY29-32 (red, blue, black, and green dots) and 0200 LT TES 20 µm
temperatures for MY24-26 (black stars). Solid curves show simulated surface temperatures with
(red) and without (black) radiatively active water ice clouds. The simulations are from the LMD
Mars Climate Database. The seasonally-varying enhancement of observed brightness
temperatures over those of the baseline simulation is attributed to downward IR flux from water
ice clouds which wax and wane in the aphelion season.
2014GL060086-fs02.eps: Latitude-pressure distribution of MCS nighttime temperature (a) and
water ice cloud opacity (b) along the 250-260°E longitude band at 0300 LT. (b) Simulated
temperature at 250°E. (c) MCS ice cloud field. (d) Contribution to the simulated longwave
heating rate (K/sol) by water ice clouds.
2014GL060086-fs031.eps: (a) Longitude-pressure distribution of nighttime (0300 LT) equatorial
(1.9°S – 1.9°N) temperature from the LMD Mars Climate Database for Ls = 90-120° using RAC.
(b) As above, but using a simulation without RAC. (c) The temperature difference between the
above two simulations. The RAC mass mixing ratio is contoured at intervals of 20 ppm. Format
is the same as for Figure 3.
References:
Madeleine, J.-B., F. Forget, E. Millour, T. Navarro, and A. Spiga (2012), The influence of
radiatively active water ice clouds on the Martian climate, Geophys. Res. Lett., 39, L23202,
doi10.1092/2012GL053564.
Millour, E., F. Forget, A. Spiga, T. Navarro, J.-B. Madeleine, A. Pottier, L. Montabone, L. Kerber,
A. Colaitis, F. Montmessin, J.-Y. Chaufray, M.A. Lopez-Valverde, F. Gonzalez-Galindo, P.L.
Read, S.R. Lewis, M.-C. Desjean, and J.-P. Huot (2014), A new Mars Climate Database, Version
5.1, paper presented at Fifth International workshop on the Mars Atmosphere: Modelling and
observations, CNES, Oxford, UK, 2014.
Navarro, T., J.-B. Madeleine, F. Forget, A. Spiga, E. Millour, F. Montmessin, and A. Maatanen,
Modeling of the martian water cycle with an improved representation of water ice clouds,
paper presented at Fifth International Workshop on the Mars Atmosphere: Modeling and
Observations, CNRS, Oxford, UK, 2014.