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- W2336818755 abstract "SPICAV VIS-IR spectrometer on-board the Venus Express mission measured the H2O abundance above Venus’ clouds in the 1.38 µm band, and provided an estimation of the cloud top altitude based on CO2 bands in the range of 1.4–1.6 µm. The H2O content and the cloud top altitude have been retrieved for the complete Venus Express dataset from 2006 to 2014 taking into account multiple scattering in the cloudy atmosphere. The cloud top altitude, corresponding to unit nadir aerosol optical depth at 1.48 µm, varies from 68 to 73 km at latitudes from 40ºS to 40ºN with an average of 70.2 ± 0.8 km assuming the aerosol scale height of 4 km. In high northern latitudes, the cloud top decreases to 62–68 km. The altitude of formation of water lines ranges from 59 to 66 km. The H2O mixing ratio at low latitudes (20ºS-20ºN) is equal to 6.1 ± 1.2 ppm with variations from 4 to 11 ppm and the effective altitude of 61.9 ± 0.5 km. Between 30º and 50º of latitude in both hemispheres, a local minimum was observed with a value of 5.4 ± 1 ppm corresponding to the effective altitude of 62.1 ± 0.6 km and variations from 3 to 8 ppm. At high latitudes in both hemispheres, the water content varies from 4 to 12 ppm with an average of 7.2 ± 1.4 ppm which corresponds to 60.6 ± 0.5 km. Observed variations of water vapor within a factor of 2-3 on the short timescale appreciably exceed individual measurement errors and could be explained as a real variation of the mixing ratio or/and possible variations of the cloud opacity within the clouds. The maximum of water at lower latitudes supports a possible convection and injection of water from lower atmospheric layers. The vertical gradient of water vapor inside the clouds explains well the increase of water near the poles correlating with the decrease of the cloud top altitude and the H2O effective altitude. On the contrary, the depletion of water in middle latitudes does not correlate with the H2O effective altitude and cannot be completely explained by the vertical gradient of water vapor within the clouds. Retrieved H2O mixing ratio is higher than those obtained in 2.56 µm from VIRTIS-H data (Cottini et al., [2015] Planet. Space Sci., 113, 219–225 ) at altitudes of 68–70 km which is well consistent with the lower altitudes of water mixing ratio from the 1.38 µm band. Observations for different solar and emission angles allowed to constrain also the average vertical distribution of H2O mixing ratio in the clouds with 2 ppm at 66 km and 7–7.5 ppm at 59–61 km. The water vapor latitudinal-longitudinal distribution does not show any direct correlation with the cloud tops. Yet a strong asymmetry of H2O longitudinal distribution has been observed with a maximum of 7–7.5 ppm from −120º to 30º of longitude and shifted to the southern hemisphere (20ºS-10ºN). To the east, the minimum is observed with values not in excess of 6 ppm and over a wide range of longitudes from 30º to 160º. Bertaux et al. (2015) announced a correlation between the zonal wind pattern in the equatorial region and underlying topography of Aphrodite Terra as the result of stationary gravity waves produced at the ground level near the mountains. The water minimum corresponds to the Aphrodite Terra highlands and can be also associated with the influence of Venus topography. No prominent long-term on the time scale of 8.5 years nor local time variations of water vapor and the cloud top altitude were detected." @default.
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- W2336818755 date "2016-09-01" @default.
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- W2336818755 title "Variations of water vapor and cloud top altitude in the Venus’ mesosphere from SPICAV/VEx observations" @default.
- W2336818755 cites W137696424 @default.
- W2336818755 cites W1538970967 @default.
- W2336818755 cites W1579401992 @default.
- W2336818755 cites W1820669772 @default.
- W2336818755 cites W1973188337 @default.
- W2336818755 cites W1978095175 @default.
- W2336818755 cites W1981085063 @default.
- W2336818755 cites W1986214263 @default.
- W2336818755 cites W1987576960 @default.
- W2336818755 cites W1992020149 @default.
- W2336818755 cites W1992685216 @default.
- W2336818755 cites W2000130216 @default.
- W2336818755 cites W2002514556 @default.
- W2336818755 cites W2003064350 @default.
- W2336818755 cites W2003165523 @default.
- W2336818755 cites W2006606446 @default.
- W2336818755 cites W2007338792 @default.
- W2336818755 cites W2008303998 @default.
- W2336818755 cites W2009341411 @default.
- W2336818755 cites W2012096461 @default.
- W2336818755 cites W2018820951 @default.
- W2336818755 cites W2023357858 @default.
- W2336818755 cites W2023755075 @default.
- W2336818755 cites W2026164300 @default.
- W2336818755 cites W2033213489 @default.
- W2336818755 cites W2034036462 @default.
- W2336818755 cites W2042198989 @default.
- W2336818755 cites W2042369298 @default.
- W2336818755 cites W2045231383 @default.
- W2336818755 cites W2050679459 @default.
- W2336818755 cites W2056435673 @default.
- W2336818755 cites W2061833413 @default.
- W2336818755 cites W2064716271 @default.
- W2336818755 cites W2068090667 @default.
- W2336818755 cites W2072250007 @default.
- W2336818755 cites W2073036983 @default.
- W2336818755 cites W2073694855 @default.
- W2336818755 cites W2074960347 @default.
- W2336818755 cites W2075501990 @default.
- W2336818755 cites W2076414174 @default.
- W2336818755 cites W2078271287 @default.
- W2336818755 cites W2083142113 @default.
- W2336818755 cites W2083438663 @default.
- W2336818755 cites W2084383883 @default.
- W2336818755 cites W2085558968 @default.
- W2336818755 cites W2091765021 @default.
- W2336818755 cites W2092960892 @default.
- W2336818755 cites W2105959125 @default.
- W2336818755 cites W2117810590 @default.
- W2336818755 cites W2121228368 @default.
- W2336818755 cites W2121508043 @default.
- W2336818755 cites W2124600301 @default.
- W2336818755 cites W2126858388 @default.
- W2336818755 cites W2133137731 @default.
- W2336818755 cites W2135472056 @default.
- W2336818755 cites W2165742018 @default.
- W2336818755 cites W2170603779 @default.
- W2336818755 cites W2357822693 @default.
- W2336818755 cites W2410003943 @default.
- W2336818755 cites W2624490378 @default.
- W2336818755 cites W4205182410 @default.
- W2336818755 doi "https://doi.org/10.1016/j.icarus.2016.04.010" @default.
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