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Reply to comment "On the hydrogen escape: Comment to variability of the hydrogen in the Martian upper atmosphere as simulated by a 3D atmosphere-exosphere coupling by J.-Y. Chaufray et al." by V. Krasnopolsky, Icarus, 281, 262
Forget, F.; Chaufray, J. -Y.; Leblanc, F. +4 more
Krasnopolsky (2017) makes a careful review of our recent results about the Martian hydrogen content of the Martian upper atmosphere (Chaufray et al., 2015). We comment here on his two major points. First, he suggests that the non-thermal escape of H2, and particularly collisions with hot oxygen, not taken into account in our general cir…
The distribution of putative periglacial landforms on the martian northern plains
Balme, Matthew R.; Patel, Manish R.; Hagermann, Axel +1 more
In this investigation, HiRISE images were surveyed across three regions of the Northern Plains of Mars; Acidalia, Arcadia and Utopia Planitiae. A sample of HiRISE images within each of these areas was examined. The aim of the investigation was to determine the distribution of three varieties of landform; clastic patterned ground, lobate hill-slope…
Long term evolution of temperature in the venus upper atmosphere at the evening and morning terminators
Pätzold, M.; Vandaele, A. C.; Montmessin, F. +11 more
This paper contains a comprehensive dataset of long-term observations between 2009 and 2015 at the upper mesosphere/lower thermosphere providing temperature values at different locations of the morning and evening side of the terminator of Venus. Temperature information is obtained by line-resolved spectroscopy of Doppler broadened CO2 …
Evidence for impact melt sheets in lunar highland smooth plains and implications for polar landing sites
Weitz, Catherine M.; Whitten, Jennifer L.; Campbell, Bruce A. +1 more
Smooth plains units attributed to fluidized basin ejecta occur over much of the lunar highlands. We examined 4-20 km diameter Imbrian- and Eratosthenian-period craters in the southern highlands that have high 12.6-cm wavelength radar backscatter and circular polarization ratios associated with their interior walls but not with their proximal eject…
The opposition effect in Saturn's main rings as seen by Cassini ISS: 4. Correlations of the surge morphology with surface albedos and VIMS spectral properties
Déau, Estelle; Dones, Luke; West, Robert A. +4 more
In this paper, we continue our analysis of the saturnian ring opposition effect seen by Cassini ISS. The ring opposition effect is a peak in the rings' reflectivity caused as the directions from a spot on the rings to the observer and to the light source, respectively, converge toward zero degrees. So far, the exact origin of the ring's opposition…
Enceladus plume density from Cassini spacecraft attitude control data
Lorenz, Ralph D.; Burk, Thomas A.
The plumes of Enceladus are of interest both as a geophysical phenomenon, and as an astrobiological opportunity for sampling internal material. Here we report measurements of the total mass density (gas plus dust, a combination not reported before except in the engineering literature) deduced from telemetry of Cassini's Attitude and Articulation C…
Sesquinary reimpacts dominate surface characteristics on Phobos
Nayak, Michael
We use topographic data to show that impact craters with pitted floor deposits are among the deepest on Mars. This is consistent with the interpretation of pitted materials as primary crater-fill impactite deposits emplaced during crater formation. Our database consists of 224 pitted material craters ranging in size from ∼1 to 150 km in diameter. …
Temperature estimation from hydroxyl airglow emission in the Venus night side mesosphere
Drossart, P.; Piccioni, G.; Gérard, J. -C. +3 more
The temperature of the night side of Venus at about 95 km has been determined by using spectral features of the hydroxyl airglow emission around 3 µm, recorded from July 2006 to July 2008 by VIRTIS onboard Venus Express. The retrieved temperatures vary from 145.5 to about 198.1 K with an average value of 176.3 ± 14.3 K and are in good agreem…
Corrigendum to "The opposition effect in Saturn's main rings as seen by Cassini ISS: 2. Constraints on the ring particles and their regolith with analytical radiative transfer models" Icarus; Vol 253 (2015); Pages 311-345
Estelle, Déau
The authors report a correction to their paper relative to the Hapke (2002, 2008) parameters: