Coupled photochemical and condensation model for the Venus atmosphere
Coupled photochemical and condensation model for the Venus atmosphere
Ground based and Venus Express observations have provided a wealth of information on the vertical and latitudinal distribution of many chemical species in the Venus atmosphere [1,2]. Previous 1D models have focused on the chemistry of either the lower [3] or middle atmosphere [4,5]. Photochemical models focusing on the sulfur gas chemistry have also been independent from models of the sulfuric acid haze and cloud formation [6,7]. In recent years sulfur-bearing particles have become important candidates for the observed SO2 inversion above 80 km [5]. To test this hypothesis it is import to create a self-consistent model that includes photochemistry, transport, and cloud condensation.In this work we extend the domain of the 1D chemistry model of Zhang et al. (2012) [5] to encompass the region between the surface to 110 km. This model includes a simple sulfuric acid condensation scheme with gravitational settling. It simultaneously solves for the chemistry and condensation allowing for self-consistent cloud formation. We compare the resulting chemical distributions to observations at all altitudes. We have also validated our model cloud mass against pioneer Venus observations [8]. This updated full atmosphere chemistry model is also being applied in our 2D solver (altitude and altitude). With this 2D model we can model how the latitudinal distribution of chemical species depends on the meridional circulation. This allows us to use the existing chemical observations to place constraints on Venus GCMs [9-11].References: [1] Arney et al., JGR:Planets, 2014 [2] Vandaele et al., Icarus 2017 (pt. 1 & 2) [3] Krasnopolsky, Icarus, 2007 [4] Krasnopolsky, Icarus, 2012 [5] Zhang et al., Icarus 2012 [6] Gao et al., Icarus, 2014 [7] Krasnopolsky, Icarus, 2015 [8] Knollenberg and Hunten, JGR:Space Physics, 1980 [9] Lee et al., JGR:Planets, 2007 [10] Lebonnois et al., Towards Understanding the Climate of Venus, 2013 [11] Mendoncca and Read, Planetary and Space Science, 2016
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Bierson, Carver
a1590f12-ad52-4984-b1e1-645cbb028363
Zhang, Xi
cf867d1b-ba43-4c31-9c21-7730573f8ff6
Mendonca, Joao
cb29fe08-eb94-4fad-8eba-eac1c5de491b
Liang, Mao-Chang
0bea7aee-0503-4acf-8edb-105363133bb6
October 2017
Bierson, Carver
a1590f12-ad52-4984-b1e1-645cbb028363
Zhang, Xi
cf867d1b-ba43-4c31-9c21-7730573f8ff6
Mendonca, Joao
cb29fe08-eb94-4fad-8eba-eac1c5de491b
Liang, Mao-Chang
0bea7aee-0503-4acf-8edb-105363133bb6
Bierson, Carver, Zhang, Xi, Mendonca, Joao and Liang, Mao-Chang
(2017)
Coupled photochemical and condensation model for the Venus atmosphere.
<br/> American Astronomical Society, DPS meeting #49.
01 Oct 2017.
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Conference or Workshop Item
(Other)
Abstract
Ground based and Venus Express observations have provided a wealth of information on the vertical and latitudinal distribution of many chemical species in the Venus atmosphere [1,2]. Previous 1D models have focused on the chemistry of either the lower [3] or middle atmosphere [4,5]. Photochemical models focusing on the sulfur gas chemistry have also been independent from models of the sulfuric acid haze and cloud formation [6,7]. In recent years sulfur-bearing particles have become important candidates for the observed SO2 inversion above 80 km [5]. To test this hypothesis it is import to create a self-consistent model that includes photochemistry, transport, and cloud condensation.In this work we extend the domain of the 1D chemistry model of Zhang et al. (2012) [5] to encompass the region between the surface to 110 km. This model includes a simple sulfuric acid condensation scheme with gravitational settling. It simultaneously solves for the chemistry and condensation allowing for self-consistent cloud formation. We compare the resulting chemical distributions to observations at all altitudes. We have also validated our model cloud mass against pioneer Venus observations [8]. This updated full atmosphere chemistry model is also being applied in our 2D solver (altitude and altitude). With this 2D model we can model how the latitudinal distribution of chemical species depends on the meridional circulation. This allows us to use the existing chemical observations to place constraints on Venus GCMs [9-11].References: [1] Arney et al., JGR:Planets, 2014 [2] Vandaele et al., Icarus 2017 (pt. 1 & 2) [3] Krasnopolsky, Icarus, 2007 [4] Krasnopolsky, Icarus, 2012 [5] Zhang et al., Icarus 2012 [6] Gao et al., Icarus, 2014 [7] Krasnopolsky, Icarus, 2015 [8] Knollenberg and Hunten, JGR:Space Physics, 1980 [9] Lee et al., JGR:Planets, 2007 [10] Lebonnois et al., Towards Understanding the Climate of Venus, 2013 [11] Mendoncca and Read, Planetary and Space Science, 2016
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Published date: October 2017
Venue - Dates:
<br/> American Astronomical Society, DPS meeting #49, 2017-10-01 - 2017-10-01
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Local EPrints ID: 496947
URI: http://eprints.soton.ac.uk/id/eprint/496947
PURE UUID: d00f6de0-0fa3-4b36-8f3f-28b22263e6b2
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Date deposited: 08 Jan 2025 15:10
Last modified: 10 Jan 2025 03:21
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Contributors
Author:
Carver Bierson
Author:
Xi Zhang
Author:
Joao Mendonca
Author:
Mao-Chang Liang
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