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Filtering by: Creator Bougher, S. W. (University of Michigan) Remove constraint Creator: Bougher, S. W. (University of Michigan) Creator Brecht, A. S. (NASA Ames Research Center) Remove constraint Creator: Brecht, A. S. (NASA Ames Research Center) Keyword upper mesophere Remove constraint Keyword: upper mesophere Language ascii and NetCDF for datafiles, ascii for README file Remove constraint Language: ascii and NetCDF for datafiles, ascii for README file Discipline Science Remove constraint Discipline: Science

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  • Planetary-scale Wave Impacts on the Venusian Upper Mesosphere and Lower Thermosphere: Supporting Datasets for VTGCM Numerical Simulations

    work
    Creator:
    Bougher, S. W. (University of Michigan) and Brecht, A. S. (NASA Ames Research Center)
    Description:
    This work examines the planetary wave-induced variability within the upper mesosphere/lower thermosphere of Venus by utilizing the Venus Thermospheric General Circulation Model (VTGCM). Rossby and Kelvin wave perturbations are driven by variations in the geopotential height of the VTGCM lower boundary (~70 km). A suite of simulations was conducted to examine the impact of the individual and combined waves propagating from two different lower boundary conditions (uniform and varying). The Kelvin wave is the more dominant wave which produces the most variability, as was shown in Hoshino et al., 2012. The combination of the Kelvin and Rossby waves provides a maximum temperature amplitude of 13 K at 92 km and maximum zonal wind amplitude of 23 m/s at 102 km. The combined waves overall are able to propagate up to 125 km. Most of the variation within the temperature, winds, and composition occurs between 70 km and 110 km. The varying lower boundary increases the magnitude of the wave deposition but weakly changes the propagation altitude. The thermal variation due to the planetary waves does not reproduce most observed variations. The simulated O2 IR nightglow emission is sensitive to the waves with respect to intensity and local time, but lacks latitudinal variation. The integrated intensity ranges from 1.2 MR to 1.65 MR and the local time ranges from 0.33 local time to 23.6 local time. Overall, planetary waves do affect the atmospheric structure, but there are still observed large variations that planetary waves alone cannot explain (i.e. thermal structure).
    Keyword:
    Venus, planetary waves, upper mesophere, lower thermosphere, and O2 nightglow
    Citation to related publication:
    Brecht, A. S., Bougher, S. W., Shields, D., & Liu, H.-L. (2021). Planetary-scale wave impacts on the Venusian upper mesosphere and lower thermosphere. Journal of Geophysical Research: Planets, 126, e2020JE006587.  https://doi.org/10.1029/2020JE006587
    Discipline:
    Science