C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST19:18:39

2017A&A...606A..53P - Astronomy and Astrophysics, volume 606A, 53-53 (2017/10-1)

Mapping the thermal structure and minor species of Venus mesosphere with ALMA submillimeter observations.


Abstract (from CDS):

Context. Water vapor and sulfur compounds are key species in the photochemistry of Venus mesosphere. These species, together with mesospheric temperatures, exhibit drastic temporal variations, both on short timescales (diurnal and day-to-day) as well on long timescales, far from being understood.
Aims. We targeted CO, SO, HDO and SO2 transitions in the submillimeter range using the Atacama Large Millimeter Array (ALMA) to study their spatial and temporal variations.
Methods. Four sets of observations were acquired on different dates in November 2011 during the first ALMA Early Science observation Cycle 0. Venus angular diameter was about 11'' with an illumination factor of 92%, so that mostly the day side of the planet was mapped. Assuming a nominal CO abundance profile, we retrieved vertical temperature profiles over the entire disk as a function of latitude and local time. Temperature profiles were later used to retrieve SO, SO2, and H2O. We used HDO as a tracer for water assuming a D/H enrichment of 200 times the terrestrial value.
Results. We derived 3D maps of mesospheric temperatures in the altitude range 70-105km. SO, SO2, and H2O are characterized by a negligible abundance below ∼ 85km followed by an increase with altitude in the upper mesosphere. Disk-averaged SO abundances present a maximum mixing ratio of 15.0±3.1ppb on November 26 followed the next day by a minimum value of 9.9±1.2ppb. Due to a very low S/N, SO2 could only be derived from the disk-averaged spectrum on the first day of observation revealing an abundance of 16.5±4.6ppb. We found a SO2/SO ratio of 1.5±0.4. Global maps of SO reveal strong variations both with latitude and local time and from day to day with abundance ranging from <1 to 15ppb. H2O disk-averages retrievals reveal a steady decrease from November 14 to 27, with the abundance varying from 3.6±0.6ppm on the first day to 2.9±0.7ppm on the last day. H2O maps reveal a slightly higher abundance on the evening side compared to the morning side and a strong depletion between the first and the second day of observation.

Abstract Copyright: © ESO, 2017

Journal keyword(s): planets and satellites: atmospheres - planets and satellites: individual: Venus - submillimeter: planetary systems - radiative transfer - instrumentation: interferometers - methods: data analysis - methods: data analysis

VizieR on-line data: <Available at CDS (J/A+A/606/A53): list.dat so*.dat hdo*.dat tem*.dat>

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 QSO B1730-130 QSO 17 33 02.70578476 -13 04 49.5481484   18 18.5 18.78 17.39 ~ 983 1
2 QSO B1921-293 BLL 19 24 51.05595514 -29 14 30.1210524   18.71 18.21 15.07   ~ 689 0

    Equat.    Gal    SGal    Ecl

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