pubvenus0.bib

@comment{{This file has been generated by bib2bib 1.98}}

@comment{{Command line: /usr/bin/bib2bib --quiet -c 'not journal:"Discussions"' -c 'not title:"Correction to"' -c 'title:"Venus" or title:"Venusian"' -c $type="ARTICLE" -oc pubvenus0.txt -ob pubvenus0.bib spiga.link.bib}}

@article{2020Icar..33513376L,
  author = {{Lefèvre}, M. and {Spiga}, A. and {Lebonnois}, S.},
  title = {{Mesoscale modeling of Venus' bow-shape waves}},
  journal = {\icarus},
  archiveprefix = {arXiv},
  eprint = {1902.07010},
  primaryclass = {astro-ph.EP},
  year = 2020,
  volume = 335,
  eid = {113376},
  pages = {113376},
  abstract = {{The Akatsuki instrument LIR measured an unprecedented wave feature at
the top of Venusian cloud layer. Stationary bow-shape waves of thousands
of kilometers large lasting several Earth days have been observed over
the main equatorial mountains. Here we use for the first time a
mesoscale model of the Venus's atmosphere with high-resolution
topography and fully coupled interactive radiative transfer
computations. Mountain waves resolved by the model form large-scale bow
shape waves with an amplitude of about 1.5 K and a size up to several
decades of latitude similar to the ones measured by the Akatsuki
spacecraft. The maximum amplitude of the waves appears in the afternoon
due to an increase of the near-surface stability. Propagating vertically
the waves encounter two regions of low static stability, the mixed layer
between approximately 18 and 30 km and the convective layer between 50
and 55 km. Some part of the wave energy can pass through these regions
via wave tunneling. These two layers act as wave filter, especially the
deep atmosphere layer. The encounter with these layers generates trapped
lee waves propagating horizontally. No stationary waves is resolved at
cloud top over the polar regions because of strong circumpolar transient
waves, and a thicker deep atmosphere mixed layer that filters most of
the mountain waves.
}},
  doi = {10.1016/j.icarus.2019.07.010},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2020Icar..33513376L},
  localpdf = {REF/2020Icar..33513376L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2018Icar..314..149L,
  author = {{Lebonnois}, S. and {Schubert}, G. and {Forget}, F. and {Spiga}, A.
	},
  title = {{Planetary boundary layer and slope winds on Venus}},
  journal = {\icarus},
  keywords = {Venus, Atmosphere, Planetary boundary layer, Slope winds},
  year = 2018,
  volume = 314,
  pages = {149-158},
  abstract = {{Few constraints are available to characterize the deep atmosphere of
Venus, though this region is crucial to understand the interactions
between surface and atmosphere on Venus. Based on simulations performed
with the IPSL Venus Global Climate Model, the possible structure and
characteristics of Venus' planetary boundary layer (PBL) are
investigated. The vertical profile of the potential temperature in the
deepest 10 km above the surface and its diurnal variations are
controlled by radiative and dynamical processes. The model predicts a
diurnal cycle for the PBL activity, with a stable nocturnal PBL while
convective activity develops during daytime. The diurnal convective PBL
is strongly correlated with surface solar flux and is maximum around
noon and in low latitude regions. It typically reaches less than 2 km
above the surface, but its vertical extension is much higher over high
elevations, and more precisely over the western flanks of elevated
terrains. This correlation is explained by the impact of surface winds,
which undergo a diurnal cycle with downward katabatic winds at night and
upward anabatic winds during the day along the slopes of high-elevation
terrains. The convergence of these daytime anabatic winds induces upward
vertical winds, that are responsible for the correlation between height
of the convective boundary layer and topography.
}},
  doi = {10.1016/j.icarus.2018.06.006},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2018Icar..314..149L},
  localpdf = {REF/2018Icar..314..149L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2018JGRE..123.2773L,
  author = {{Lefèvre}, M. and {Lebonnois}, S. and {Spiga}, A.},
  title = {{Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Venus, modeling, convection, gravity waves},
  year = 2018,
  volume = 123,
  pages = {2773-2789},
  abstract = {{Venus' convective cloud layers and associated gravity waves strongly
impact the local and global budget of heat, momentum, and chemical
species. Here we use for the first time three-dimensional
turbulence-resolving dynamical integrations of Venus' atmosphere from
the surface to 100-km altitude, coupled with fully interactive radiative
transfer computations. We show that this enables to correctly reproduce
the vertical position (46- to 55-km altitude) and thickness (9 km) of
the main convective cloud layer measured by Venus Express and Akatsuki
radio occultations, as well as the intensity of convective plumes (3
m/s) measured by VEGA balloons. Both the radiative forcing in the
visible and the large-scale dynamical impact play a role in the
variability of the cloud convective activity with local time and
latitude. Our model reproduces the diurnal cycle in cloud convection
observed by Akatsuki at the low latitudes and the lack thereof observed
by Venus Express at the equator. The observed enhancement of cloud
convection at high latitudes is simulated by our model, although
underestimated compared to observations. We show that the influence of
the vertical shear of horizontal superrotating winds must be accounted
for in our model to allow for gravity waves of the observed intensity
($\gt$1 K) and horizontal wavelength (up to 20 km) to be generated
through the obstacle effect mechanism. The vertical extent of our model
also allows us to predict for the first time a 7-km-thick convective
layer at the cloud top (70-km altitude) caused by the solar absorption
of the unknown ultraviolet absorber.
}},
  doi = {10.1029/2018JE005679},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2018JGRE..123.2773L},
  localpdf = {REF/2018JGRE..123.2773L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2017JGRE..122..134L,
  author = {{Lefèvre}, M. and {Spiga}, A. and {Lebonnois}, S.},
  title = {{Three-dimensional turbulence-resolving modeling of the Venusian cloud layer and induced gravity waves}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {3-D mesoscale modeling, Venus, convective cloud layer, gravity waves},
  year = 2017,
  volume = 122,
  pages = {134-149},
  abstract = {{The impact of the cloud convective layer of the atmosphere of Venus on
the global circulation remains unclear. The recent observations of
gravity waves at the top of the cloud by the Venus Express mission
provided some answers. These waves are not resolved at the scale of
global circulation models (GCM); therefore, we developed an
unprecedented 3-D turbulence-resolving large-eddy simulations (LES)
Venusian model using the Weather Research and Forecast terrestrial
model. The forcing consists of three different heating rates: two
radiative ones for solar and infrared and one associated with the
adiabatic cooling/warming of the global circulation. The rates are
extracted from the Laboratoire de Météorlogie Dynamique
Venus GCM using two different cloud models. Thus, we are able to
characterize the convection and associated gravity waves in function of
latitude and local time. To assess the impact of the global circulation
on the convective layer, we used rates from a 1-D radiative-convective
model. The resolved layer, taking place between 1.0 {\times}
10$^{5}$ and 3.8 {\times} 10$^{4}$ Pa (48-53 km), is
organized as polygonal closed cells of about 10 km wide with vertical
wind of several meters per second. The convection emits gravity waves
both above and below the convective layer leading to temperature
perturbations of several tenths of kelvin with vertical wavelength
between 1 and 3 km and horizontal wavelength from 1 to 10 km. The
thickness of the convective layer and the amplitudes of waves are
consistent with observations, though slightly underestimated. The global
dynamics heating greatly modify the convective layer.
}},
  doi = {10.1002/2016JE005146},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2017JGRE..122..134L},
  localpdf = {REF/2017JGRE..122..134L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}