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@comment{{Command line: bib2bib --quiet -c year=2015 -c $type="ARTICLE" -oc pub2015.txt -ob pub2015.bib}}
  author = {{Lebonnois}, S. and {Eymet}, V. and {Lee}, C. and {Vatant d'Ollone}, J.
  title = {{Analysis of the radiative budget of the Venusian atmosphere based on infrared Net Exchange Rate formalism}},
  journal = {Journal of Geophysical Research (Planets)},
  keywords = {Venus atmosphere, radiative transfer, Net Exchange Rate analysis},
  year = 2015,
  volume = 120,
  pages = {1186-1200},
  abstract = {{A detailed one-dimensional analysis of the energy balance in Venus
atmosphere is proposed in this work, based on the Net Exchange Rate
formalism that allows the identification in each altitude region of the
dominant energy exchanges controlling the temperature. Well-known
parameters that control the temperature profile are the solar flux
deposition and the cloud particle distribution. Balance between solar
heating and infrared energy exchanges is analyzed for each region: upper
atmosphere (from cloud top to 100 km), upper cloud, middle cloud, cloud
base, and deep atmosphere (cloud base to surface). The energy
accumulated below the clouds is transferred to the cloud base through
infrared windows, mostly at 3-4 {$\mu$}m and 5-7 {$\mu$}m. The continuum
opacity in these spectral regions is not well known for the hot
temperatures and large pressures of Venus's deep atmosphere but strongly
affects the temperature profile from cloud base to surface. From cloud
base, upward transport of energy goes through convection and short-range
radiative exchanges up to the middle cloud where the atmosphere is thin
enough in the 20-30 {$\mu$}m window to cool directly to space. Total
opacity in this spectral window between the 15 {$\mu$}m CO$_{2}$ band
and the CO$_{2}$ collision-induced absorption has a strong impact
on the temperature in the cloud convective layer. Improving our
knowledge of the gas opacities in these different windows through new
laboratory measurements or ab initio computations, as well as improving
the constraints on cloud opacities would help to separate gas and cloud
contributions and secure a better understanding of Venus's atmosphere
energy balance.
  doi = {10.1002/2015JE004794},
  adsurl = {},
  localpdf = {REF/2015JGRE..120.1186L.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Charnay}, B. and {Barth}, E. and {Rafkin}, S. and {Narteau}, C. and 
	{Lebonnois}, S. and {Rodriguez}, S. and {Courrech Du Pont}, S. and 
	{Lucas}, A.},
  title = {{Methane storms as a driver of Titan's dune orientation}},
  journal = {Nature Geoscience},
  archiveprefix = {arXiv},
  eprint = {1504.03404},
  primaryclass = {astro-ph.EP},
  year = 2015,
  volume = 8,
  pages = {362-366},
  abstract = {{The equatorial regions of Saturn's moon Titan are covered by linear
dunes that propagate eastwards. Global climate models (GCMs), however,
predict westward mean surface winds at low latitudes on Titan, similar
to the trade winds on Earth. This apparent contradiction has been
attributed to Saturn's gravitational tides, large-scale topography and
wind statistics, but none of these hypotheses fully explains the global
eastward propagation of dunes in Titan's equatorial band. However, above
altitudes of about 5 km, Titan's atmosphere is in eastward
super-rotation, suggesting that this momentum may be delivered to the
surface. Here we assess the influence of equatorial tropical methane
storms--which develop at high altitudes during the equinox--on Titan's
dune orientation, using mesoscale simulations of convective methane
clouds with a GCM wind profile that includes super-rotation. We find
that these storms produce fast eastward gust fronts above the surface
that exceed the normal westward surface winds. These episodic gusts
generated by tropical storms are expected to dominate aeolian transport,
leading to eastward propagation of dunes. We therefore suggest a
coupling between super-rotation, tropical methane storms and dune
formation on Titan. This framework, applied to GCM predictions and
analogies to some terrestrial dune fields, explains the linear shape,
eastward propagation and poleward divergence of Titan's dunes, and
implies an equatorial origin of dune sand.
  doi = {10.1038/ngeo2406},
  adsurl = {},
  localpdf = {REF/2015NatGe...8..362C.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}
  author = {{Vinatier}, S. and {B├ęzard}, B. and {Lebonnois}, S. and 
	{Teanby}, N.~A. and {Achterberg}, R.~K. and {Gorius}, N. and 
	{Mamoutkine}, A. and {Guandique}, E. and {Jolly}, A. and {Jennings}, D.~E. and 
	{Flasar}, F.~M.},
  title = {{Seasonal variations in Titan's middle atmosphere during the northern spring derived from Cassini/CIRS observations}},
  journal = {\icarus},
  keywords = {Titan, atmosphere, Infrared observations, Atmospheres, structure, Atmospheres, composition},
  year = 2015,
  volume = 250,
  pages = {95-115},
  abstract = {{We analyzed spectra acquired at the limb of Titan in the 2006-2013
period by the Cassini/Composite Infrared Spectrometer (CIRS) in order to
monitor the seasonal evolution of the thermal, gas composition and
aerosol spatial distributions. We are primarily interested here in the
seasonal changes after the northern spring equinox and interpret our
results in term of global circulation seasonal changes. Data cover the
600-1500 cm$^{-1}$ spectral range at a resolution of 0.5 or 15.5
cm$^{-1}$ and probe the 150-500 km vertical range with a vertical
resolution of about 30 km. Retrievals of the limb spectra acquired at
15.5 cm$^{-1}$ resolution allowed us to derive eight global maps
of temperature, aerosols and C$_{2}$H$_{2}$,
C$_{2}$H$_{6}$ and HCN molecular mixing ratios between July
2009 and May 2013. In order to have a better understanding of the global
changes taking place after the northern spring equinox, we analyzed 0.5
cm$^{-1}$ resolution limb spectra to infer the mixing ratio
profiles of 10 molecules for some latitudes. These profiles are compared
with CIRS observations performed during the northern winter. Our
observations are compatible with the coexistence of two circulation
cells upwelling at mid-latitudes and downwelling at both poles from at
last January 2010 to at least June 2010. One year later, in June 2011,
there are indications that the global circulation had reversed compared
to the winter situation, with a single pole-to-pole cell upwelling at
the north pole and downwelling at the south pole. Our observations show
that in December 2011, this new pole-to-pole cell has settled with a
downward velocity of 4.4 mm/s at 450 km above the south pole. Therefore,
in about two years after the equinox, the global circulation observed
during the northern winter has totally reversed, which is in agreement
with the predictions of general circulation models. We observe a sudden
unexpected temperature decrease above the south pole in February 2012,
which is probably related to the strong enhancement of molecular gas in
this region, acting as radiative coolers. In July and November 2012, we
observe a detached haze layer located around 320-330 km, which is
comparable to the altitude of the detached haze layer observed by the
Cassini Imaging Science Subsystem (ISS) in the UV.
  doi = {10.1016/j.icarus.2014.11.019},
  adsurl = {},
  localpdf = {REF/2015Icar..250...95V.pdf},
  adsnote = {Provided by the SAO/NASA Astrophysics Data System}