pub2007.bib
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@article{2007Natur.450..646B,
author = {{Bertaux}, J.-L. and {Vandaele}, A.-C. and {Korablev}, O. and
{Villard}, E. and {Fedorova}, A. and {Fussen}, D. and {Quémerais}, E. and
{Belyaev}, D. and {Mahieux}, A. and {Montmessin}, F. and {Muller}, C. and
{Neefs}, E. and {Nevejans}, D. and {Wilquet}, V. and {Dubois}, J.~P. and
{Hauchecorne}, A. and {Stepanov}, A. and {Vinogradov}, I. and
{Rodin}, A. and {Bertaux}, J.-L. and {Nevejans}, D. and {Korablev}, O. and
{Montmessin}, F. and {Vandaele}, A.-C. and {Fedorova}, A. and
{Cabane}, M. and {Chassefière}, E. and {Chaufray}, J.~Y. and
{Dimarellis}, E. and {Dubois}, J.~P. and {Hauchecorne}, A. and
{Leblanc}, F. and {Lefèvre}, F. and {Rannou}, P. and {Quémerais}, E. and
{Villard}, E. and {Fussen}, D. and {Muller}, C. and {Neefs}, E. and
{van Ransbeeck}, E. and {Wilquet}, V. and {Rodin}, A. and {Stepanov}, A. and
{Vinogradov}, I. and {Zasova}, L. and {Forget}, F. and {Lebonnois}, S. and
{Titov}, D. and {Rafkin}, S. and {Durry}, G. and {Gérard}, J.~C. and
{Sandel}, B.},
title = {{A warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H$_{2}$O and HDO}},
journal = {\nat},
year = 2007,
volume = 450,
pages = {646-649},
abstract = {{Venus has thick clouds of H$_{2}$SO$_{4}$ aerosol particles
extending from altitudes of 40 to 60km. The 60-100km region (the
mesosphere) is a transition region between the 4day retrograde
superrotation at the top of the thick clouds and the solar-antisolar
circulation in the thermosphere (above 100km), which has upwelling over
the subsolar point and transport to the nightside. The mesosphere has a
light haze of variable optical thickness, with CO, SO$_{2}$, HCl,
HF, H$_{2}$O and HDO as the most important minor gaseous
constituents, but the vertical distribution of the haze and molecules is
poorly known because previous descent probes began their measurements at
or below 60km. Here we report the detection of an extensive layer of
warm air at altitudes 90-120km on the night side that we interpret as
the result of adiabatic heating during air subsidence. Such a strong
temperature inversion was not expected, because the night side of Venus
was otherwise so cold that it was named the `cryosphere' above 100km. We
also measured the mesospheric distributions of HF, HCl, H$_{2}$O
and HDO. HCl is less abundant than reported 40years ago.
HDO/H$_{2}$O is enhanced by a factor of \~{}2.5 with respect to the
lower atmosphere, and there is a general depletion of H$_{2}$O
around 80-90km for which we have no explanation.
}},
doi = {10.1038/nature05974},
adsurl = {https://ui.adsabs.harvard.edu/abs/2007Natur.450..646B},
localpdf = {REF/2007Natur.450..646B.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2007Natur.450..641D,
author = {{Drossart}, P. and {Piccioni}, G. and {Gérard}, J.~C. and
{Lopez-Valverde}, M.~A. and {Sanchez-Lavega}, A. and {Zasova}, L. and
{Hueso}, R. and {Taylor}, F.~W. and {Bézard}, B. and {Adriani}, A. and
{Angrilli}, F. and {Arnold}, G. and {Baines}, K.~H. and {Bellucci}, G. and
{Benkhoff}, J. and {Bibring}, J.~P. and {Blanco}, A. and {Blecka}, M.~I. and
{Carlson}, R.~W. and {Coradini}, A. and {di Lellis}, A. and
{Encrenaz}, T. and {Erard}, S. and {Fonti}, S. and {Formisano}, V. and
{Fouchet}, T. and {Garcia}, R. and {Haus}, R. and {Helbert}, J. and
{Ignatiev}, N.~I. and {Irwin}, P. and {Langevin}, Y. and {Lebonnois}, S. and
{Luz}, D. and {Marinangeli}, L. and {Orofino}, V. and {Rodin}, A.~V. and
{Roos-Serote}, M.~C. and {Saggin}, B. and {Stam}, D.~M. and
{Titov}, D. and {Visconti}, G. and {Zambelli}, M. and {Tsang}, C. and
{Ammannito}, E. and {Barbis}, A. and {Berlin}, R. and {Bettanini}, C. and
{Boccaccini}, A. and {Bonnello}, G. and {Bouyé}, M. and
{Capaccioni}, F. and {Cardesin}, A. and {Carraro}, F. and {Cherubini}, G. and
{Cosi}, M. and {Dami}, M. and {de Nino}, M. and {Del Vento}, D. and
{di Giampietro}, M. and {Donati}, A. and {Dupuis}, O. and {Espinasse}, S. and
{Fabbri}, A. and {Fave}, A. and {Ficai Veltroni}, I. and {Filacchione}, G. and
{Garceran}, K. and {Ghomchi}, Y. and {Giustizi}, M. and {Gondet}, B. and
{Hello}, Y. and {Henry}, F. and {Hofer}, S. and {Huntzinger}, G. and
{Kachlicki}, J. and {Knoll}, R. and {Kouach}, D. and {Mazzoni}, A. and
{Melchiorri}, R. and {Mondello}, G. and {Monti}, F. and {Neumann}, C. and
{Nuccilli}, F. and {Parisot}, J. and {Pasqui}, C. and {Perferi}, S. and
{Peter}, G. and {Piacentino}, A. and {Pompei}, C. and {Réess}, J.-M. and
{Rivet}, J.-P. and {Romano}, A. and {Russ}, N. and {Santoni}, M. and
{Scarpelli}, A. and {Sémery}, A. and {Soufflot}, A. and
{Stefanovitch}, D. and {Suetta}, E. and {Tarchi}, F. and {Tonetti}, N. and
{Tosi}, F. and {Ulmer}, B.},
title = {{A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express}},
journal = {\nat},
year = 2007,
volume = 450,
pages = {641-645},
abstract = {{The upper atmosphere of a planet is a transition region in which energy
is transferred between the deeper atmosphere and outer space. Molecular
emissions from the upper atmosphere (90-120km altitude) of Venus can be
used to investigate the energetics and to trace the circulation of this
hitherto little-studied region. Previous spacecraft and ground-based
observations of infrared emission from CO$_{2}$, O$_{2}$ and
NO have established that photochemical and dynamic activity controls the
structure of the upper atmosphere of Venus. These data, however, have
left unresolved the precise altitude of the emission owing to a lack of
data and of an adequate observing geometry. Here we report measurements
of day-side CO$_{2}$ non-local thermodynamic equilibrium emission
at 4.3{\micro}m, extending from 90 to 120km altitude, and of night-side
O$_{2}$ emission extending from 95 to 100km. The CO$_{2}$
emission peak occurs at \~{}115km and varies with solar zenith angle over a
range of \~{}10km. This confirms previous modelling, and permits the
beginning of a systematic study of the variability of the emission. The
O$_{2}$ peak emission happens at 96km+/-1km, which is consistent
with three-body recombination of oxygen atoms transported from the day
side by a global thermospheric sub-solar to anti-solar circulation, as
previously predicted.
}},
doi = {10.1038/nature06140},
adsurl = {https://ui.adsabs.harvard.edu/abs/2007Natur.450..641D},
localpdf = {REF/2007Natur.450..641D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2007Natur.450..637P,
author = {{Piccioni}, G. and {Drossart}, P. and {Sanchez-Lavega}, A. and
{Hueso}, R. and {Taylor}, F.~W. and {Wilson}, C.~F. and {Grassi}, D. and
{Zasova}, L. and {Moriconi}, M. and {Adriani}, A. and {Lebonnois}, S. and
{Coradini}, A. and {Bézard}, B. and {Angrilli}, F. and {Arnold}, G. and
{Baines}, K.~H. and {Bellucci}, G. and {Benkhoff}, J. and {Bibring}, J.~P. and
{Blanco}, A. and {Blecka}, M.~I. and {Carlson}, R.~W. and {di Lellis}, A. and
{Encrenaz}, T. and {Erard}, S. and {Fonti}, S. and {Formisano}, V. and
{Fouchet}, T. and {Garcia}, R. and {Haus}, R. and {Helbert}, J. and
{Ignatiev}, N.~I. and {Irwin}, P.~G.~J. and {Langevin}, Y. and
{Lopez-Valverde}, M.~A. and {Luz}, D. and {Marinangeli}, L. and
{Orofino}, V. and {Rodin}, A.~V. and {Roos-Serote}, M.~C. and
{Saggin}, B. and {Stam}, D.~M. and {Titov}, D. and {Visconti}, G. and
{Zambelli}, M. and {Ammannito}, E. and {Barbis}, A. and {Berlin}, R. and
{Bettanini}, C. and {Boccaccini}, A. and {Bonnello}, G. and
{Bouye}, M. and {Capaccioni}, F. and {Cardesin Moinelo}, A. and
{Carraro}, F. and {Cherubini}, G. and {Cosi}, M. and {Dami}, M. and
{de Nino}, M. and {Del Vento}, D. and {di Giampietro}, M. and
{Donati}, A. and {Dupuis}, O. and {Espinasse}, S. and {Fabbri}, A. and
{Fave}, A. and {Veltroni}, I.~F. and {Filacchione}, G. and {Garceran}, K. and
{Ghomchi}, Y. and {Giustini}, M. and {Gondet}, B. and {Hello}, Y. and
{Henry}, F. and {Hofer}, S. and {Huntzinger}, G. and {Kachlicki}, J. and
{Knoll}, R. and {Driss}, K. and {Mazzoni}, A. and {Melchiorri}, R. and
{Mondello}, G. and {Monti}, F. and {Neumann}, C. and {Nuccilli}, F. and
{Parisot}, J. and {Pasqui}, C. and {Perferi}, S. and {Peter}, G. and
{Piacentino}, A. and {Pompei}, C. and {Reess}, J.-M. and {Rivet}, J.-P. and
{Romano}, A. and {Russ}, N. and {Santoni}, M. and {Scarpelli}, A. and
{Semery}, A. and {Soufflot}, A. and {Stefanovitch}, D. and {Suetta}, E. and
{Tarchi}, F. and {Tonetti}, N. and {Tosi}, F. and {Ulmer}, B.
},
title = {{South-polar features on Venus similar to those near the north pole}},
journal = {\nat},
year = 2007,
volume = 450,
pages = {637-640},
abstract = {{Venus has no seasons, slow rotation and a very massive atmosphere, which
is mainly carbon dioxide with clouds primarily of sulphuric acid
droplets. Infrared observations by previous missions to Venus revealed a
bright `dipole' feature surrounded by a cold `collar' at its north pole.
The polar dipole is a `double-eye' feature at the centre of a vast
vortex that rotates around the pole, and is possibly associated with
rapid downwelling. The polar cold collar is a wide, shallow river of
cold air that circulates around the polar vortex. One outstanding
question has been whether the global circulation was symmetric, such
that a dipole feature existed at the south pole. Here we report
observations of Venus' south-polar region, where we have seen clouds
with morphology much like those around the north pole, but rotating
somewhat faster than the northern dipole. The vortex may extend down to
the lower cloud layers that lie at about 50km height and perhaps deeper.
The spectroscopic properties of the clouds around the south pole are
compatible with a sulphuric acid composition.
}},
doi = {10.1038/nature06209},
adsurl = {https://ui.adsabs.harvard.edu/abs/2007Natur.450..637P},
localpdf = {REF/2007Natur.450..637P.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2007Icar..191..236D,
author = {{De La Haye}, V. and {Waite}, J.~H. and {Cravens}, T.~E. and
{Nagy}, A.~F. and {Johnson}, R.~E. and {Lebonnois}, S. and {Robertson}, I.~P.
},
title = {{Titan's corona: The contribution of exothermic chemistry}},
journal = {\icarus},
year = 2007,
volume = 191,
pages = {236-250},
abstract = {{The contribution of exothermic ion and neutral chemistry to Titan's
corona is studied. The production rates for fast neutrals N
$_{2}$, CH $_{4}$, H, H $_{2}$, $^{3}$CH
$_{2}$, CH $_{3}$, C $_{2}$H $_{4}$, C
$_{2}$H $_{5}$, C $_{2}$H $_{6}$, N(
$^{4}$S), NH, and HCN are determined using a coupled ion and
neutral model of Titan's upper atmosphere. After production, the
formation of the suprathermal particles is modeled using a two-stream
simulation, as they travel simultaneously through a thermal mixture of N
$_{2}$, CH $_{4}$, and H $_{2}$. The resulting
suprathermal fluxes, hot density profiles, and energy distributions are
compared to the N $_{2}$ and CH $_{4}$ INMS exospheric data
presented in [De La Haye, V., Waite Jr., J.H., Johnson, R.E., Yelle,
R.V., Cravens, T.E., Luhmann, J.G., Kasprzak, W.T., Gell, D.A., Magee,
B., Leblanc, F., Michael, M., Jurac, S., Robertson, I.P., 2007. J.
Geophys. Res., doi:10.1029/2006JA012222, in press], and are found
insufficient for producing the suprathermal populations measured. Global
losses of nitrogen atoms and carbon atoms in all forms due to exothermic
chemistry are estimated to be 8.3{\times}10 Ns and 7.2{\times}10 Cs.
}},
doi = {10.1016/j.icarus.2007.04.031},
adsurl = {https://ui.adsabs.harvard.edu/abs/2007Icar..191..236D},
localpdf = {REF/2007Icar..191..236D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2007P&SS...55.1653D,
author = {{Drossart}, P. and {Piccioni}, G. and {Adriani}, A. and {Angrilli}, F. and
{Arnold}, G. and {Baines}, K.~H. and {Bellucci}, G. and {Benkhoff}, J. and
{Bézard}, B. and {Bibring}, J.-P. and {Blanco}, A. and {Blecka}, M.~I. and
{Carlson}, R.~W. and {Coradini}, A. and {Di Lellis}, A. and
{Encrenaz}, T. and {Erard}, S. and {Fonti}, S. and {Formisano}, V. and
{Fouchet}, T. and {Garcia}, R. and {Haus}, R. and {Helbert}, J. and
{Ignatiev}, N.~I. and {Irwin}, P.~G.~J. and {Langevin}, Y. and
{Lebonnois}, S. and {Lopez-Valverde}, M.~A. and {Luz}, D. and
{Marinangeli}, L. and {Orofino}, V. and {Rodin}, A.~V. and {Roos-Serote}, M.~C. and
{Saggin}, B. and {Sanchez-Lavega}, A. and {Stam}, D.~M. and
{Taylor}, F.~W. and {Titov}, D. and {Visconti}, G. and {Zambelli}, M. and
{Hueso}, R. and {Tsang}, C.~C.~C. and {Wilson}, C.~F. and {Afanasenko}, T.~Z.
},
title = {{Scientific goals for the observation of Venus by VIRTIS on ESA/Venus express mission}},
journal = {\planss},
year = 2007,
volume = 55,
pages = {1653-1672},
abstract = {{The Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on board
the ESA/Venus Express mission has technical specifications well suited
for many science objectives of Venus exploration. VIRTIS will both
comprehensively explore a plethora of atmospheric properties and
processes and map optical properties of the surface through its three
channels, VIRTIS-M-vis (imaging spectrometer in the 0.3-1 {$\mu$}m range),
VIRTIS-M-IR (imaging spectrometer in the 1-5 {$\mu$}m range) and VIRTIS-H
(aperture high-resolution spectrometer in the 2-5 {$\mu$}m range). The
atmospheric composition below the clouds will be repeatedly measured in
the night side infrared windows over a wide range of latitudes and
longitudes, thereby providing information on Venus's chemical cycles. In
particular, CO, H $_{2}$O, OCS and SO $_{2}$ can be studied.
The cloud structure will be repeatedly mapped from the brightness
contrasts in the near-infrared night side windows, providing new
insights into Venusian meteorology. The global circulation and local
dynamics of Venus will be extensively studied from infrared and visible
spectral images. The thermal structure above the clouds will be
retrieved in the night side using the 4.3 {$\mu$}m fundamental band of CO
$_{2}$. The surface of Venus is detectable in the short-wave
infrared windows on the night side at 1.01, 1.10 and 1.18 {$\mu$}m,
providing constraints on surface properties and the extent of active
volcanism. Many more tentative studies are also possible, such as
lightning detection, the composition of volcanic emissions, and
mesospheric wave propagation.
}},
doi = {10.1016/j.pss.2007.01.003},
adsurl = {https://ui.adsabs.harvard.edu/abs/2007P%26SS...55.1653D},
localpdf = {REF/2007P_26SS...55.1653D.pdf},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}