TY - JOUR
T1 - Simulating Jupiter's weather layer. Part I
T2 - Jet spin-up in a dry atmosphere
AU - Young, Roland M.B.
AU - Read, Peter L.
AU - Wang, Yixiong
N1 - Funding Information:
Support for RMBY and PLR provided by UK STFC Grants ST/F003145/1, ST/I001948/1, and ST/K00106X/1. Support for PLR provided by UK STFC Grant ST/N00082X/1. Part of this work was completed during a visit to the Kavli Institute for Theoretical Physics at UC Santa Barbara. This work was supported in part by the US National Science Foundation under Grant No. NSF PHY-1125915. The authors would like to thank Terry Davies, Nathan Mayne, William Ingram, Hiro Yamazaki, and Lena Zuchowski for assistance with an earlier version of the model, Pat Irwin and João Mendonça for help with the new radiation scheme, Liam Brannigan, Yuan Lian, David Munday and Inna Polichtchouk for assistance running the MITgcm, Jeremy Yates for his patience while we ran the simulations, Michael McIntyre, Aymeric Spiga, and Stephen Thomson for useful discussions, and two anonymous reviewers whose extensive comments improved the paper significantly. Many figures used David Fanning's Coyote IDL Program Library. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology, and the Darwin Data Analytic system at the University of Cambridge, operated by the University of Cambridge HPC Service, both on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grants ST/K00042X/1 and ST/K001590/1, STFC capital grants ST/K00087X/1, ST/H008861/1, and ST/H00887X/1, DiRAC Operations grants ST/K003267/1 and ST/K00333X/1, and Durham University. DiRAC is part of the UK National E-Infrastructure. The authors acknowledge the use of the IRIDIS High Performance Computing Facility, and associated support services at the University of Southampton, in the completion of this work. The authors acknowledge the use of the University of Oxford Advanced Research Computing (ARC) facility in carrying out this work. http://dx.doi.org/10.5281/zenodo.22558.
Funding Information:
This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology, and the Darwin Data Analytic system at the University of Cambridge, operated by the University of Cambridge HPC Service, both on behalf of the STFC DiRAC HPC Facility ( www.dirac.ac.uk ). This equipment was funded by BIS National E-infrastructure capital grants ST/K00042X/1 and ST/K001590/1, STFC capital grants ST/K00087X/1, ST/H008861/1, and ST/H00887X/1, DiRAC Operations grants ST/K003267/1 and ST/K00333X/1, and Durham University. DiRAC is part of the UK National E-Infrastructure. The authors acknowledge the use of the IRIDIS High Performance Computing Facility, and associated support services at the University of Southampton, in the completion of this work. The authors acknowledge the use of the University of Oxford Advanced Research Computing (ARC) facility in carrying out this work. http://dx.doi.org/10.5281/zenodo.22558 .
Funding Information:
Support for RMBY and PLR provided by UK STFC Grants ST/F003145/1, ST/I001948/1, and ST/K00106X/1. Support for PLR provided by UK STFC Grant ST/N00082X/1. Part of this work was completed during a visit to the Kavli Institute for Theoretical Physics at UC Santa Barbara. This work was supported in part by the US National Science Foundation under Grant No. NSF PHY-1125915. The authors would like to thank Terry Davies, Nathan Mayne, William Ingram, Hiro Yamazaki, and Lena Zuchowski for assistance with an earlier version of the model, Pat Irwin and João Mendonça for help with the new radiation scheme, Liam Brannigan, Yuan Lian, David Munday and Inna Polichtchouk for assistance running the MITgcm, Jeremy Yates for his patience while we ran the simulations, Michael McIntyre, Aymeric Spiga, and Stephen Thomson for useful discussions, and two anonymous reviewers whose extensive comments improved the paper significantly. Many figures used David Fanning’s Coyote IDL Program Library.
Publisher Copyright:
© 2018 The Authors
PY - 2019/7/1
Y1 - 2019/7/1
N2 - 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 Oxford's Jupiter General Circulation 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 5.7Wm −2 interior heat flux. Simulations ran for 130000–150000 d 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 20ms −1 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, 50ms −1 sub-rotating equatorial jet with weak eddy activity at low latitudes.
AB - 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 Oxford's Jupiter General Circulation 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 5.7Wm −2 interior heat flux. Simulations ran for 130000–150000 d 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 20ms −1 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, 50ms −1 sub-rotating equatorial jet with weak eddy activity at low latitudes.
KW - Barotropic instability
KW - Convection
KW - General circulation model
KW - Jupiter
KW - Super-rotation
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U2 - 10.1016/j.icarus.2018.12.005
DO - 10.1016/j.icarus.2018.12.005
M3 - Article
AN - SCOPUS:85062210204
SN - 0019-1035
VL - 326
SP - 225
EP - 252
JO - Icarus
JF - Icarus
ER -