213
Planetary
Atmospheres
CO
2
bands detected in the Venus atmosphere by SOIR/Venus Express is conduct‑
ed [Robert et al., 2013].
The modeling of high‑resolution spectra of methane isotopologues
12
CH
3
D
(at 900–5000 cm
‑1
)
and measurements of
12
CH
4
(at 4800–5300 cm
‑1
) is performed
[Nikitin et al., 2014]. Line broadening of ro-vibrational lines of CH
3
CN by N
2
,
and with self-broadening and their temperature dependence is investigated
[Dudaryonok et al., 2015 ab].
The kinetics of electron-exited oxygen and CO molecules in the atmospheres
of Venus and Mars is studied [Kirillov, 2013, 2014 ab].
The upate of the principal spectroscopic databases, HITRAN and GEISA has
been conducted with participation of Russian scientists [Rothman et al., 2014;
Jacquinet-Husson et al., 2011].
A method to study the internal gravity waves using the vertical profiles of
temperature, density or the square of buoyancy in the atmosphere of a planed is
suggested. The method is validated using roadiozonde measurements in the ter‑
restrial stratosphere. The method allows to identify “discrete” (narrow-spectrum)
wave events in the atmospheres of the Earth, Venus and Mars and to determine
the characteristics of the internal gravity waves [Gubenko et al., 2011, 2015].
The so-called shadow method used to estimate the optical depth of the Mar‑
tian atmosphere and the albedo of the surface from the differences in
brightness
between shadowed and sunlit regions observed from an orbiter is described and
evaluated. The method is validated using high-resolution HiRISE/MRO images,
and optical depth measured by the Opportunity rover [Hoekzema et al., 2011;
Petrova et al., 2012].
The atmospheric chemistry suite (ACS) package for sensitive measurements
of minor atmospheric gases, and the monitoring of the atmospheric thermal state
is a part of the Russian contribution to the ExoMars ESA-Roscosmos mission.
ACS consists of three separate infrared spectrometers. The near-infrared (NIR)
channel is a versatile spectrometer for the spectral range of 0.7–1.6 μm with a
resolving power of ~20,000. The instrument employs the principle of an echelle
spectrometer with an AOTF as a preselector. NIR will be operated in nadir, in
solar occultations, and possibly on the limb. Scientific targets of NIR on Mars
are the measurements of water vapor, aerosols, and dayside or nightside airglows.
The mid‑infrared (MIR) channel is a cross‑dispersion echelle instrument dedi‑
cated to solar occultation measurements in the range of 2.2–4.4 μm targeting the
resolving power of 50,000. MIR is dedicated to sensitive measurements of trace
gases, in particular methane. The thermal infrared channel (TIRVIM) is a 2-inch
double pendulum Fourier-transform spectrometer for the spectral range of 1.7–17
μm with apodized resolution varying from 0.2 to 1.6 cm
‑1
. TIRVIM is primarily
dedicated to the monitoring of atmospheric temperatures and
aerosol states in
nadir [Korablev et al., 2014]. The instrument inherits design solution of
214
O. I. Korablev
previously developed instruments for Phobos-Grunt mission [Korablev et al.,
2012, 2013].
7. Conclusion
As previously, many of the research on planetary atmospheres completed in
2011–2014 are related to Venus Express and Mars Express missions. Mars Ex‑
press will continue its operations, as planned at present, until 2018. In the mean‑
while, the launch of the national planetary project Phobos Grunt in 2011 turned
a complete disaster. A new mission with planned serious atmosphere, climate and
meteorology studies, and with a key Russian involvement is ExoMars. ExoMars
consists of two launches, the 2016 with Trace Gas Orbiter, and the entry and
descent demonstrator, and the 2018 with a Rover, and a stationary long-living
science platform. All proposals for a Venus mission, national, or with Russian
involvement [Vorontsov et al., 2011; Wilson et al, 2012] are not being imple‑
mented so far. The lack of national space programs have not prevented from
consolidation of efforts in the field of planetary atmospheres in Russia. The
number of publications is growing, and the studies become more synergetic. The
planetary
astronomy, almost forgotten is coming back.
Many studies included in the current Report were supported by the Pro‑
gramme No22 of the Presidium of Russian Academy of Sciences and the Grant
of the Russian Government No11.G34.31.0074. The author is grateful to Svetla‑
na Gulyakova for the help in preparation of the Report.
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