pub2016.bib

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@comment{{Command line: bib2bib --quiet -c year=2016 -c $type="ARTICLE" -oc pub2016.txt -ob pub2016.bib lebonnois.link.bib}}

@article{2016Icar..278...38L,
  author = {{Lebonnois}, S. and {Sugimoto}, N. and {Gilli}, G.},
  title = {{Wave analysis in the atmosphere of Venus below 100-km altitude, simulated by the LMD Venus GCM}},
  journal = {\icarus},
  keywords = {Venus, atmosphere, Atmospheres, dynamics, Numerical modeling},
  year = 2016,
  volume = 278,
  pages = {38-51},
  abstract = {{A new simulation of Venus atmospheric circulation obtained with the LMD
Venus GCM is described and the simulated wave activity is analyzed.
Agreement with observed features of the temperature structure, static
stability and zonal wind field is good, such as the presence of a cold
polar collar, diurnal and semi-diurnal tides. At the resolution used (96
longitudes {\times} 96 latitudes), a fully developed superrotation is
obtained both when the simulation is initialized from rest and from an
atmosphere already in superrotation, though winds are still weak below
the clouds (roughly half the observed values). The atmospheric waves
play a crucial role in the angular momentum budget of the Venus's
atmospheric circulation. In the upper cloud, the vertical angular
momentum is transported by the diurnal and semi-diurnal tides. Above the
cloud base (approximately 1 bar), equatorward transport of angular
momentum is done by polar barotropic and mid- to high-latitude
baroclinic waves present in the cloud region, with frequencies between 5
and 20 cycles per Venus day (periods between 6 and 23 Earth days). In
the middle cloud, just above the convective layer, a Kelvin type wave
(period around 7.3 Ed) is present at the equator, as well as a
low-latitude Rossby-gravity type wave (period around 16 Ed). Below the
clouds, large-scale mid- to high-latitude gravity waves develop and play
a significant role in the angular momentum balance.
}},
  doi = {10.1016/j.icarus.2016.06.004},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016Icar..278...38L},
  localpdf = {REF/2016Icar..278...38L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2016JGRE..121.1087B,
  author = {{Bertaux}, J.-L. and {Khatuntsev}, I.~V. and {Hauchecorne}, A. and 
	{Markiewicz}, W.~J. and {Marcq}, E. and {Lebonnois}, S. and 
	{Patsaeva}, M. and {Turin}, A. and {Fedorova}, A.},
  title = {{Influence of Venus topography on the zonal wind and UV albedo at cloud top level: The role of stationary gravity waves}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Venus, zonal wind, gravity waves, Venus Express, VMC, superrotation},
  year = 2016,
  volume = 121,
  pages = {1087-1101},
  abstract = {{Based on the analysis of UV images (at 365 nm) of Venus cloud top
(altitude 67 {\plusmn} 2 km) collected with Venus Monitoring Camera on
board Venus Express (VEX), it is found that the zonal wind speed south
of the equator (from 5{\deg}S to 15{\deg}S) shows a conspicuous variation
(from -101 to -83 m/s) with geographic longitude of Venus, correlated
with the underlying relief of Aphrodite Terra. We interpret this pattern
as the result of stationary gravity waves produced at ground level by
the uplift of air when the horizontal wind encounters a mountain slope.
These waves can propagate up to the cloud top level, break there, and
transfer their momentum to the zonal flow. Such upward propagation of
gravity waves and influence on the wind speed vertical profile was shown
to play an important role in the middle atmosphere of the Earth by
Lindzen (1981) but is not reproduced in the current GCM of Venus
atmosphere from LMD. (Laboratoire de Météorologie
Dynamique) In the equatorial regions, the UV albedo at 365 nm varies
also with longitude. We argue that this variation may be simply
explained by the divergence of the horizontal wind field. In the
longitude region (from 60{\deg} to -10{\deg}) where the horizontal wind
speed is increasing in magnitude (stretch), it triggers air upwelling
which brings the UV absorber at cloud top level and decreases the albedo
and vice versa when the wind is decreasing in magnitude (compression).
This picture is fully consistent with the classical view of Venus
meridional circulation, with upwelling at equator revealed by horizontal
air motions away from equator: the longitude effect is only an
additional but important modulation of this effect. This interpretation
is comforted by a recent map of cloud top H$_{2}$O, showing that
near the equator the lower UV albedo longitude region is correlated with
increased H$_{2}$O. We argue that H$_{2}$O enhancement is
the sign of upwelling, suggesting that the UV absorber is also brought
to cloud top by upwelling.
}},
  doi = {10.1002/2015JE004958},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016JGRE..121.1087B},
  localpdf = {REF/2016JGRE..121.1087B.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{2016QJRMS.142..703R,
  author = {{Read}, P.~L. and {Barstow}, J. and {Charnay}, B. and {Chelvaniththilan}, S. and 
	{Irwin}, P.~G.~J. and {Knight}, S. and {Lebonnois}, S. and {Lewis}, S.~R. and 
	{Mendon{\c c}a}, J. and {Montabone}, L.},
  title = {{Global energy budgets and `Trenberth diagrams' for the climates of terrestrial and gas giant planets}},
  journal = {Quarterly Journal of the Royal Meteorological Society},
  year = 2016,
  volume = 142,
  pages = {703-720},
  doi = {10.1002/qj.2704},
  adsurl = {https://ui.adsabs.harvard.edu/abs/2016QJRMS.142..703R},
  localpdf = {REF/2016QJRMS.142..703R.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}