Simulating Jupiter's weather layer: Accompanying data for Parts I and II

Name: Simulating Jupiter's weather layer: Accompanying data for Parts I and II
Published: 2018-01-01T00:00:00Z
License: https://opendatacommons.org/licenses/by/1-0/index.html

Young, R

Documentation:: See file readme.pdf. This dataset contains instantaneous model states from two simulations of Jupiter’s atmosphere, over 100 Earth days. The data were generated by a version of the MIT General Circulation Model (MITgcm) modified to simulate Jupiter’s upper troposphere and lower stratosphere. The model simulates Jupiter’s weather layer down to 18 bar at 0.7 degree horizontal resolution, with parametrizations of radiative forcing, vertical diffusion, dry convection, and ammonia and water cycles. Run B has 5.7 W/m2 heating into the bottom of the domain, while Run A does not; both are heated by the Sun from above.

Version:: 1.0

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APA Style

Young, R. (2018). Simulating Jupiter's weather layer: Accompanying data for Parts I and II. University of Oxford.

MLA Style

Young, R. Simulating Jupiter's Weather Layer: Accompanying Data for Parts I and II. University of Oxford, 2018.

Chicago Style

Young, R. 2018. Simulating Jupiter's Weather Layer: Accompanying Data for Parts I and II. University of Oxford.
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Files:: RunA.tgz

(gtar, 1.8GB, Terms of use)

RunB.tgz

(gtar, 1.8GB, Terms of use)

readme.pdf

(Preview, pdf, 152.7KB, Terms of use)

Authors/Creators

+ Young, R More by this author/creator

Institution:: University of Oxford
Division:: MPLS
Department:: Physics
Role:: Researcher, Creator

Contributors

+ Wang, Y

Institution:: University of Oxford
Division:: MPLS
Department:: Physics
Role:: Contributor

+ Read, P

Institution:: University of Oxford
Division:: MPLS
Department:: Physics
Role:: Principal Investigator (PI)

+ US National Science Foundation More from this funder

Funding agency for:: Young, R
Grant:: PHY-1125915

+ Science and Technology Facilities Council More from this funder

Funding agency for:: Young, R; Young, R; Young, R; Read, P
Grant:: ST/K00106X/1; ST/I001948/1; ST/F003145/1; ST/N00082X/1

Publisher:: University of Oxford
Publication date:: 2018
Spatial coverage:: Jupiter
Version number:: 1.0
DOI:: 10.5287/bodleian:PyYbbxpk2

Language:: English
Keywords:: Jupiter

Barotropic instability

Water

Super-rotation

General Circulation Model

Convection

Ammonia

Clouds
Subjects:: Numerical modelling

Physics

Geophysical fluid dynamics

Atmospheric physics

Planetary science
Pubs id:: 1480060
UUID:: uuid:ce0e862f-2cf4-400e-b558-60889e316eda
Local pid:: pubs:1480060
Deposit date:: 2018-12-04
ARK identifier:: ark:/29072/ora_ce0e862f2cf4400eb55860889e316eda

Related item:: Simulating Jupiter's weather layer. Part II: Passive ammonia and water cycles
Description:: We examine the ammonia and water cycles in Jupiter’s upper troposphere and lower stratosphere during spin-up of a multiple zonal jet circulation using the Oxford Jupiter GCM. Jupiter’s atmosphere is simulated at 512 × 256 horizontal resolution with 33 vertical levels between 0.01 and 18 bar, putting the lowest level well below the expected water cloud base. Simulations with and without a 5.7 interior heat source were run for 130000–150000 d to allow the deep atmosphere to come into radiative-convective-dynamical equilibrium, with variants on the interior heating case including varying the initial tracer distribution, particle condensate diameter, and cloud process timescales. The cloud scheme includes simple representations of the ammonia and water cycles. Ammonia vapour changes phase to ice, and reacts with hydrogen sulphide to produce ammonium hydrosulphide. Water changes phases between vapour, liquid, and ice depending on local environmental conditions, and all condensates sediment at their respective Stokes velocities. With interior heating, clouds of ammonia ice, ammonium hydrosulphide ice, and water ice form with cloud bases around 0.4 bar, 1.5 bar, and 3 bar respectively. Without interior heating the ammonia cloud base forms in the same way, but the ammonium hydrosulphide and water clouds sediment to the bottom of the domain. The liquid water cloud is either absent or extremely sparse. Zonal structures form that correlate regions of strong latitudinal shear with regions of constant condensate concentration, implying that jets act as barriers to the mixing. Regions with locally high and low cloud concentrations also correlated with regions of upwelling and downwelling, respectively. Shortly after initialisation, the ammonia vapour distribution up to the cloud base resembles the enhanced concentration seen in Juno observations, due to strong meridional mean circulation at the equator. The resemblance decays rapidly over time, but suggests that at least some of the relevant physics is captured by the model. The comparison should improve with additional microphysics and better representation of the deep ammonia reservoir.
Related item:: Simulating Jupiter's weather layer. Part I: Jet spin-up in a dry atmosphere
Description:: We investigate the dynamics of Jupiter’s upper troposphere and lower stratosphere using a General Circulation Model that includes two-stream radiation and optional heating from below. Based on the MITgcm dynamical core, this is a new generation of the Oxford Jupiter model [Zuchowski, L.C. et al., 2009. Plan. Space Sci., 57, 1525–1537, doi:10.1016/j.pss.2009.05.008]. We simulate Jupiter’s atmosphere at up to 0.7° horizontal resolution with 33 vertical levels down to a pressure of 18 bar, in configurations with and without a 5.7W m interior heat flux. Simulations ran for 130000–150000days to allow the deep atmosphere to come into radiative equilibrium. Baroclinic instability generates alternating, eddy-driven, midlatitude jets in both cases. With interior heating the zonal jets migrate towards the equator and become barotropically unstable. This generates Rossby waves that radiate away from the equator, depositing westerly momentum there via eddy angular momentum flux convergence and spinning up a super-rotating 20 equatorial jet throughout the troposphere. There are 30–35 zonal jets with latitudinal separation comparable with the real planet, and there is strong eddy activity throughout. Without interior heating the jets do not migrate and a divergent eddy angular momentum flux at the equator spins up a broad, 50 sub-rotating equatorial jet with weak eddy activity at low latitudes.

Terms of use

Notes:: This data deposit accompanies two papers which have just been accepted (which are linked above in Section 4, and which I deposited in ORA earlier today). Please can this dataset (and the record, if possible) be embargoed until those two papers are published online. I'll let you know when they appear.

In these two papers I cite this dataset directly. Please can you send me the DOI as soon as it is available, so that when they send me the proofs to check I can add it to the citation. Thanks.

The readme lists a number of other grants that funded the facilities used to generate the data (specific acknowledgment wording, as required by the facilities themselves). I'm not sure whether these should be included under Section 6, and at present I have not included them. Please let me know if they should, and I will add them.

Licence:: Open Data Commons Attribution License (ODC-By)

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