Statistics – Computation
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011icar..211..429e&link_type=abstract
Icarus, Volume 211, Issue 1, p. 429-442.
Statistics
Computation
3
Scientific paper
Using a Curtis-matrix model of 15 μ¼m CO2 radiative cooling rates for the martian atmosphere, we have computed vertical scale-dependent IR radiative damping rates from 0 to 200 km altitude over a broad band of vertical wavenumbers |m| = 2π(1-500 km)-1 for representative meteorological conditions at 40°N and average levels of solar activity and dust loading. In the middle atmosphere, infrared (IR) radiative damping rates increase with decreasing vertical scale and peak in excess of 30 days-1 at ˜50-80 km altitude, before gradually transitioning to scale-independent rates above ˜100 km due to breakdown of local thermodynamic equilibrium. We incorporate these computed IR radiative damping rates into a linear anelastic gravity-wave model to assess the impact of IR radiative damping, relative to wave breaking and molecular viscosity, in the dissipation of gravity-wave momentum flux. The model results indicate that IR radiative damping is the dominant process in dissipating gravity-wave momentum fluxes at ˜0-50 km altitude, and is the dominant process at all altitudes for gravity waves with vertical wavelengths ≲10-15 km. Wave breaking becomes dominant at higher altitudes only for "fast" waves of short horizontal and long vertical wavelengths. Molecular viscosity plays a negligible role in overall momentum flux deposition. Our results provide compelling evidence that IR radiative damping is a major, and often dominant physical process controlling the dissipation of gravity-wave momentum fluxes on Mars, and therefore should be incorporated into future parameterizations of gravity-wave drag within Mars GCMs. Lookup tables for doing so, based on the current computations, are provided.
Eckermann Stephen D.
Ma Jun
Zhu Xun
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