Difference between revisions of "Other GCM Configurations worth knowing about"
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== 3D DYNAMICO setup == | == 3D DYNAMICO setup == | ||
| − | Due to the rich dynamical activities in their atmospheres (banded zonal jets, eddies, vortices, storms, equatorial oscillations,...) resulting from multi-scale dynamic interactions, the Global Climate Modelling of the giant planet requires to resolve eddies arising from hydrodynamical instabilities to correctly establish the planetary-scaled jets regime. To this purpose, their Rossby radius deformation $$L_D$$, which is the length scale at which rotational effects become as important as buoyancy or gravity wave effects in the evolution of the flow about some disturbance, is calculated to determine the most suitable horizontal grid resolution. At mid-latitude range, for the giant planets, $$L_D$$ is of the same order of magnitude as that of the Earth. As the giant planets have a size of roughly 10 times the Earth size (i.e., Jupiter and Saturn), the modelling grid must be of a horizontal resolution of 0.5$$^{\circ}$$ over longitude and latitude (vs 5$$^{\circ}$$ for the Earth), considering 3 grid points to resolved $$L_D$$. Moreover, these atmospheres are cold, with long radiative response time which needs radiative transfer computations over decade-long years of Jupiter, Saturn, Uranus or Neptune (depending on the planet | + | Due to the rich dynamical activities in their atmospheres (banded zonal jets, eddies, vortices, storms, equatorial oscillations,...) resulting from multi-scale dynamic interactions, the Global Climate Modelling of the giant planet requires to resolve eddies arising from hydrodynamical instabilities to correctly establish the planetary-scaled jets regime. To this purpose, their Rossby radius deformation $$L_D$$, which is the length scale at which rotational effects become as important as buoyancy or gravity wave effects in the evolution of the flow about some disturbance, is calculated to determine the most suitable horizontal grid resolution. At mid-latitude range, for the giant planets, $$L_D$$ is of the same order of magnitude as that of the Earth. As the giant planets have a size of roughly 10 times the Earth size (i.e., Jupiter and Saturn), the modelling grid must be of a horizontal resolution of 0.5$$^{\circ}$$ over longitude and latitude (vs 5$$^{\circ}$$ for the Earth), considering 3 grid points to resolved $$L_D$$. Moreover, giant planets owns very rich atmospheric dynamics, particularly visible at the top of the tropospheric cloud layer. These planets are characterised by band-structured wind jet streams, with super-rotating equatorial jets, which could reach 400 m/s in the case of Saturn. Monitoring of tropospheric dynamical activity has revealed turbulence and vortices in and around the jets, as well as storms that can extend over several degrees of latitude and longitude, among others. Extending observations of temperature and chemical compounds in giant planet stratospheres allows to predict large-scale dynamics similar to those on Earth, such as the equatorial oscillation and a seasonal inter-hemispheric circulation. Both of these climate phenomena have been studied for decades for the Earth's atmosphere, and result from small- and large-scale interactions between the troposphere and stratosphere. Because of the nature of the climate phenomena, GCM must also resolve the propagation of dynamic instabilities, waves and turbulence along the vertical. Finally, these atmospheres are cold, with long radiative response time which needs radiative transfer computations over decade-long years of Jupiter ($$approx$$ 12 Earth years), Saturn ($$approx$$ 30 Earth years), Uranus ($$approx$$ 84 earth years) or Neptune($$approx$$ 169 Earth years), depending on the planet. |
| − | To this | + | |
| + | To be able to deal with these three -- and non-exhaustive -- requirements to build a giant planet GCM, we need massive computational ressources. For this, we use a dynamical core suitable and numerical stable for massive parallel ressource computations: DYNAMICO [Dubos et al,. 2015]. | ||
Revision as of 23:10, 21 June 2022
3D lon-lat LMDZ setup
early Mars
It is already described in the Quick Install and Run section.
Earth with slab ocean
TBD by Martin
TRAPPIST-1e with photochemistry
A temperate rocky planet in synchronous rotation around a low mass star
TBD by Yassin
TRAPPIST-1c in Venus-like conditions
A warm rocky planet in synchronous rotation around a low mass star
TBD by Gabriella
mini-Neptune GJ1214b
A warm mini-Neptune
TBD by Benjamin
3D DYNAMICO setup
Due to the rich dynamical activities in their atmospheres (banded zonal jets, eddies, vortices, storms, equatorial oscillations,...) resulting from multi-scale dynamic interactions, the Global Climate Modelling of the giant planet requires to resolve eddies arising from hydrodynamical instabilities to correctly establish the planetary-scaled jets regime. To this purpose, their Rossby radius deformation $$L_D$$, which is the length scale at which rotational effects become as important as buoyancy or gravity wave effects in the evolution of the flow about some disturbance, is calculated to determine the most suitable horizontal grid resolution. At mid-latitude range, for the giant planets, $$L_D$$ is of the same order of magnitude as that of the Earth. As the giant planets have a size of roughly 10 times the Earth size (i.e., Jupiter and Saturn), the modelling grid must be of a horizontal resolution of 0.5$$^{\circ}$$ over longitude and latitude (vs 5$$^{\circ}$$ for the Earth), considering 3 grid points to resolved $$L_D$$. Moreover, giant planets owns very rich atmospheric dynamics, particularly visible at the top of the tropospheric cloud layer. These planets are characterised by band-structured wind jet streams, with super-rotating equatorial jets, which could reach 400 m/s in the case of Saturn. Monitoring of tropospheric dynamical activity has revealed turbulence and vortices in and around the jets, as well as storms that can extend over several degrees of latitude and longitude, among others. Extending observations of temperature and chemical compounds in giant planet stratospheres allows to predict large-scale dynamics similar to those on Earth, such as the equatorial oscillation and a seasonal inter-hemispheric circulation. Both of these climate phenomena have been studied for decades for the Earth's atmosphere, and result from small- and large-scale interactions between the troposphere and stratosphere. Because of the nature of the climate phenomena, GCM must also resolve the propagation of dynamic instabilities, waves and turbulence along the vertical. Finally, these atmospheres are cold, with long radiative response time which needs radiative transfer computations over decade-long years of Jupiter ($$approx$$ 12 Earth years), Saturn ($$approx$$ 30 Earth years), Uranus ($$approx$$ 84 earth years) or Neptune($$approx$$ 169 Earth years), depending on the planet.
To be able to deal with these three -- and non-exhaustive -- requirements to build a giant planet GCM, we need massive computational ressources. For this, we use a dynamical core suitable and numerical stable for massive parallel ressource computations: DYNAMICO [Dubos et al,. 2015].
In these two following subsections, we purpose an example of installation for Jupiter and a Hot Jupiter. All the install, compiling, setting and parameters files for each giant planets could be found on:
https://github.com/aymeric-spiga/dynamico-giant
If you have already downloaded LMDZ.COMMON, LMDZ.GENERIC, IOIPSL, ARCH, you only have to download:
ICOSAGCM: the DYNAMICO dynamical core
git clone https://gitlab.in2p3.fr/ipsl/projets/dynamico/dynamico.git ICOSAGCM
cd ICOSAGCM
git checkout 90f7138a60ebd3644fbbc42bc9dfa22923386385
ICOSA_LMDZ: the interface using to link LMDZ.GENERIC physical packages and ICOSAGCM
svn update -r 2655 -q ICOSA_LMDZ
XIOS (XML Input Output Server): the library to interpolate input/output fields between the icosahedral and longitude/latitude regular grids on fly
svn co -r 2319 -q http://forge.ipsl.jussieu.fr/ioserver/svn/XIOS/trunk XIOS
If you haven't already download LMDZ.COMMON, LMDZ.GENERIC, IOIPSL, ARCH, you can use the install.sh script provided by the Github repository.
Jupiter with DYNAMICO
TBD by Deborah
Hot Jupiter with DYNAMICO
TBD by Lucas
3D LES setup
Proxima b with LES
TBD by Maxence
1D setup
rcm1d test case
Our 1-D forward model
TBD by Gwenael ?
kcm1d test case
Our 1-D inverse model
TBD by Guillaume or Martin
