pub2022.bib
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@article{2022PSJ.....3..117G,
author = {{Garvin}, J. B. and {Getty}, S. A. and {Arney}, G. N. and {Johnson}, N. M. and {Kohler}, E. and {Schwer}, K. O. and {Sekerak}, M. and {Bartels}, A. and {Saylor}, R. S. and {Elliott}, V. E. and {Goodloe}, C. S. and {Garrison}, M. B. and {Cottini}, V. and {Izenberg}, N. and {Lorenz}, R. and {Malespin}, C. A. and {Ravine}, M. and {Webster}, C. R. and {Atkinson}, D. H. and {Aslam}, S. and {Atreya}, S. and {Bos}, B. J. and {Brinckerhoff}, W. B. and {Campbell}, B. and {Crisp}, D. and {Filiberto}, J. R. and {Forget}, F. and {Gilmore}, M. and {Gorius}, N. and {Grinspoon}, D. and {Hofmann}, A. E. and {Kane}, S. R. and {Kiefer}, W. and {Lebonnois}, S. and {Mahaffy}, P. R. and {Pavlov}, A. and {Trainer}, M. and {Zahnle}, K. J. and {Zolotov}, M.},
title = {{Revealing the Mysteries of Venus: The DAVINCI Mission}},
journal = {\psj},
keywords = {Venus, Planetary science, Planetary probes, Flyby missions, Planetary atmospheres, Planetary surfaces, 1763, 1255, 1252, 545, 1244, 2113, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2022,
month = may,
volume = {3},
number = {5},
eid = {117},
pages = {117},
abstract = {{The Deep Atmosphere Venus Investigation of Noble gases, Chemistry, and
Imaging (DAVINCI) mission described herein has been selected for
flight to Venus as part of the NASA Discovery Program. DAVINCI
will be the first mission to Venus to incorporate science-driven
flybys and an instrumented descent sphere into a unified
architecture. The anticipated scientific outcome will be a new
understanding of the atmosphere, surface, and evolutionary path
of Venus as a possibly once-habitable planet and analog to hot
terrestrial exoplanets. The primary mission design for DAVINCI
as selected features a preferred launch in summer/fall 2029, two
flybys in 2030, and descent-sphere atmospheric entry by the end
of 2031. The in situ atmospheric descent phase subsequently
delivers definitive chemical and isotopic composition of the
Venus atmosphere during an atmospheric transect above Alpha
Regio. These in situ investigations of the atmosphere and near-
infrared (NIR) descent imaging of the surface will complement
remote flyby observations of the dynamic atmosphere, cloud deck,
and surface NIR emissivity. The overall mission yield will be at
least 60 Gbits (compressed) new data about the atmosphere and
near surface, as well as the first unique characterization of
the deep atmosphere environment and chemistry, including trace
gases, key stable isotopes, oxygen fugacity, constraints on
local rock compositions, and topography of a tessera.}},
doi = {10.3847/PSJ/ac63c2},
archiveprefix = {arXiv},
eprint = {2206.07211},
primaryclass = {astro-ph.EP},
localpdf = {REF/2022PSJ.....3..117G.pdf},
adsurl = {https://ui.adsabs.harvard.edu/abs/2022PSJ.....3..117G},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2022A&A...658A.108C,
author = {{Charnay}, B. and {Tobie}, G. and {Lebonnois}, S. and {Lorenz}, R.~D.},
title = {{Gravitational atmospheric tides as a probe of Titan's interior: Application to Dragonfly}},
journal = {\aap},
keywords = {planets and satellites: individual: Titan, planets and satellites: atmospheres, planets and satellites: interiors, Astrophysics - Earth and Planetary Astrophysics},
year = 2022,
month = feb,
volume = {658},
eid = {A108},
pages = {A108},
abstract = {{Context. Saturn's massive gravity is expected to causes a tide in
Titan's atmosphere, producing a surface pressure variation
through the orbit of Titan and tidal winds in the troposphere.
The future Dragonfly mission could analyse this exotic
meteorological phenomenon. \textbackslash Aims: We aim to
analyse the effect of Saturn's tides on Titan's atmosphere and
interior to determine how pressure measurements by Dragonfly
could constrain Titan's interior. \textbackslash Methods: We
model atmospheric tides with analytical calculations and with a
3D global climate model (the IPSL-Titan GCM), including the
tidal response of the interior. \textbackslash Results: We
predict that the Love numbers of Titan's interior should verify
1 + ℜ(k$_{2}$ {\ensuremath{-}} h$_{2}$)
\raisebox{-0.5ex}\textasciitilde 0.02-0.1 and ℑ(k$_{2}$
{\ensuremath{-}} h$_{2}$) < 0.04. The deformation of Titan's
interior should therefore strongly weaken gravitational
atmospheric tides, yielding a residual surface pressure
amplitude of only \raisebox{-0.5ex}\textasciitilde5 Pa, with a
phase shift of 5-20 h. Tidal winds are very weak, of the order
of 3 {\texttimes} 10$^{{\ensuremath{-}}4}$ m
s$^{{\ensuremath{-}}1}$ in the lower troposphere. Finally,
constraints from Dragonfly data may permit the real and the
imaginary parts of k$_{2}$ {\ensuremath{-}} h$_{2}$ to be
estimated with a precision of {\ensuremath{\pm}}0.01-0.03.
\textbackslash Conclusions: Measurements of pressure variations
by Dragonfly over the whole mission could give valuable
constraints on the thickness of Titan's ice shell, and, via
geophysical models, its heat flux and the density of its
internal ocean.}},
doi = {10.1051/0004-6361/202141898},
archiveprefix = {arXiv},
eprint = {2111.02199},
primaryclass = {astro-ph.EP},
localpdf = {REF/2022A&A...658A.108C.pdf},
adsurl = {https://ui.adsabs.harvard.edu/abs/2022A&A...658A.108C},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}
@article{2022ExA...tmp....2R,
author = {{Rodriguez}, S. and {Vinatier}, S. and {Cordier}, D. and {Tobie}, G. and {Achterberg}, R. K. and {Anderson}, C. M. and {Badman}, S. V. and {Barnes}, J. W. and {Barth}, E. L. and {B{\'e}zard}, B. and {Carrasco}, N. and {Charnay}, B. and {Clark}, R. N. and {Coll}, P. and {Cornet}, T. and {Coustenis}, A. and {Couturier-Tamburelli}, I. and {Dobrijevic}, M. and {Flasar}, F. M. and {de Kok}, R. and {Freissinet}, C. and {Galand}, M. and {Gautier}, T. and {Geppert}, W. D. and {Griffith}, C. A. and {Gudipati}, M. S. and {Hadid}, L. Z. and {Hayes}, A. G. and {Hendrix}, A. R. and {Jaumann}, R. and {Jennings}, D. E. and {Jolly}, A. and {Kalousova}, K. and {Koskinen}, T. T. and {Lavvas}, P. and {Lebonnois}, S. and {Lebreton}, J.-P. and {Le Gall}, A. and {Lellouch}, E. and {Le Mou{\'e}lic}, S. and {Lopes}, R. M.~C. and {Lora}, J. M. and {Lorenz}, R. D. and {Lucas}, A. and {MacKenzie}, S. and {Malaska}, M. J. and {Mandt}, K. and {Mastrogiuseppe}, M. and {Newman}, C. E. and {Nixon}, C. A. and {Radebaugh}, J. and {Rafkin}, S. C. and {Rannou}, P. and {Sciamma-O'Brien}, E. M. and {Soderblom}, J. M. and {Solomonidou}, A. and {Sotin}, C. and {Stephan}, K. and {Strobel}, D. and {Szopa}, C. and {Teanby}, N. A. and {Turtle}, E. P. and {Vuitton}, V. and {West}, R. A.},
title = {{Science goals and new mission concepts for future exploration of Titan's atmosphere, geology and habitability: titan POlar scout/orbitEr and in situ lake lander and DrONe explorer (POSEIDON)}},
journal = {Experimental Astronomy},
keywords = {Titan, Atmosphere, Geology, Habitability, Orbiter, Lake lander, Drones, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
year = 2022,
month = jan,
abstract = {{In response to ESA's ``Voyage 2050'' announcement of opportunity, we
propose an ambitious L-class mission to explore one of the most
exciting bodies in the Solar System, Saturn's largest moon
Titan. Titan, a ``world with two oceans'', is an organic-rich
body with interior-surface-atmosphere interactions that are
comparable in complexity to the Earth. Titan is also one of the
few places in the Solar System with habitability potential.
Titan's remarkable nature was only partly revealed by the
Cassini-Huygens mission and still holds mysteries requiring a
complete exploration using a variety of vehicles and
instruments. The proposed mission concept POSEIDON (Titan POlar
Scout/orbitEr and In situ lake lander DrONe explorer) would
perform joint orbital and in situ investigations of Titan. It is
designed to build on and exceed the scope and
scientific/technological accomplishments of Cassini-Huygens,
exploring Titan in ways that were not previously possible, in
particular through full close-up and in situ coverage over long
periods of time. In the proposed mission architecture, POSEIDON
consists of two major elements: a spacecraft with a large set of
instruments that would orbit Titan, preferably in a low-
eccentricity polar orbit, and a suite of in situ investigation
components, i.e. a lake lander, a ``heavy'' drone (possibly
amphibious) and/or a fleet of mini-drones, dedicated to the
exploration of the polar regions. The ideal arrival time at
Titan would be slightly before the next northern Spring equinox
(2039), as equinoxes are the most active periods to monitor
still largely unknown atmospheric and surface seasonal changes.
The exploration of Titan's northern latitudes with an orbiter
and in situ element(s) would be highly complementary in terms of
timing (with possible mission timing overlap), locations, and
science goals with the upcoming NASA New Frontiers Dragonfly
mission that will provide in situ exploration of Titan's
equatorial regions, in the mid-2030s.}},
doi = {10.1007/s10686-021-09815-8},
archiveprefix = {arXiv},
eprint = {2110.10466},
primaryclass = {astro-ph.EP},
localpdf = {REF/2022ExA...tmp....2R.pdf},
adsurl = {https://ui.adsabs.harvard.edu/abs/2022ExA...tmp....2R},
adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}