pub2023.bib

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@comment{{Command line: bib2bib --quiet -c year=2023 -c $type="ARTICLE" -oc pub2023.txt -ob pub2023.bib lebonnois.link.bib}}

@article{2023Icar..38915272M,
  author = {{Martinez}, A. and {Lebonnois}, S. and {Millour}, E. and {Pierron}, T. and {Moisan}, E. and {Gilli}, G. and {Lef{\`e}vre}, F.},
  title = {{Exploring the variability of the Venusian thermosphere with the IPSL Venus GCM}},
  journal = {\icarus},
  keywords = {Venus, Thermosphere, Modeling, Composition, Solar cycle},
  year = 2023,
  month = jan,
  volume = {389},
  eid = {115272},
  pages = {115272},
  abstract = {{Recent simulations of the Institut Pierre-Simon Laplace (IPSL) Venus
        Global Climate Model (VGCM) developed at the Laboratoire de
        M{\'e}t{\'e}orologie Dynamique (LMD) were performed with a model
        top raised from {\ensuremath{\sim}}10$^{-5}$
        ({\ensuremath{\sim}}150 km) to {\ensuremath{\sim}}10$^{-8}$ Pa
        (180-250 km; upper boundary). The parameterizations of non-LTE
        CO$_{2}$ near infrared heating rates and of non-orographic
        gravity waves were improved. In addition, a tuning of atomic
        oxygen production was introduced to improve related effects
        (heating and cooling) and resulting thermospheric number
        densities. This work focusses on validating the modelled
        thermospheric structure using data from the Pioneer Venus,
        Magellan and Venus Express missions which cover similar and
        complementary (equator and pole) regions at different periods of
        solar activity, typically above altitudes of 130 km. This
        version of the IPSL VGCM shows good agreement with the diurnal
        evolution of the exospheric temperature at the equator
        reconstructed from the atomic oxygen scale height of the Pioneer
        Venus Orbiter Neutral Mass Spectrometer data. The model is also
        able to reproduce the sensitivity of the exospheric temperature
        and species density to the EUV flux of the solar high activity
        period (from 180 to 230 solar flux unit; s.f.u). However, to fit
        with the PV-ONMS density observations, it was necessary to
        increase the photodissociation of CO$_{2}$ into CO and O above
        135 km by a factor of 10. Indeed, our study points to the
        importance of an additional source of oxygen and carbon monoxide
        production above 130 km other than CO$_{2}$ photolysis to
        explain the vertical profiles of CO and O number density in the
        thermosphere. Moreover, the presence of a GW drag at altitudes
        above 140 km has a significant impact on the nightside
        temperature value and its distribution.}},
  doi = {10.1016/j.icarus.2022.115272},
  localpdf = {REF/2023Icar..38915272M.pdf},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2023Icar..38915272M},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}