Planets - User contributions [en]

Overview of the Venus PCM

2026-03-23T16:08:26Z

Mlefevre: /* POULDP Venus */

Welcome to the overview page of the Venus Planetary Climate Model

== The Venus PCM (Planetary Climate Model) ==

In a nutshell the Venus PCM is a suite of models combining the Venus physics package and a dynamical core which may be LMDZ (the historical lon-lat grid), DYNAMICO (a more recent icosahedral dynamical core) or [[WRF dynamical core for LES/mesoscale simulations|'''WRF''']] (limited area dynamical core).

== Getting started ==
The traditional Venus PCM - LMDZ (formerly know as the IPSL Venus GCM) is the most commonly used version. For a first try at installing running the Venus PCM we recommend you start from the [[Quick Install and Run Venus PCM]] page. You will also most likely be interested in all the pages tagged as "Venus-Model" or "Venus-LMDZ" in the [[Special:Categories|Categories]] section.

== POULDP Venus ==
A POULDP meeting, for Point Organisé et Utile LMDZ Dynamico Planéto (apologies to non-French speakers), is organized between the developers to discuss the development of the model and plan improvements.

To subscribe to the POULDP mailing list (and/or browse through past messages): https://groupes.renater.fr/sympa/info/pouldp_venus

== Bibliography ==

Some recent reference articles:
==== 2026 ====
*Martinez, A., H. Karyu, A. Brecht, G. Gilli, S. Lebonnois, T. Kuroda, A. Stolzenbach, F. González-Galindo, S. Bougher, and H. Fujiwara, '''Comparison of General Circulation Models of the Venus upper atmosphere''', Icarus, 447, 116901 (2026). DOI: https://doi.org/10.1016/j.icarus.2025.116901
*Martinez, A., G. Gilli, A. Stolzenbach, T. Navarro, F. Lefèvre, S. Lebonnois, and N. Streel, '''New Insight on the Global Dynamics in the "Transition Region" of Venus Atmosphere (80─130 km) With a 3D Model''', Journal of Geophysical Research (Planets), 131, e2025JE009313 (2026). DOI: https://doi.org/10.1029/2025JE009313
==== 2025 ====
*Lai, D., T. Li, S. Lebonnois, and M. Lefèvre, '''Stationary wave dynamics in Venus's upper clouds: Morphology and forcing from Akatsuki/LIR and Venus planetary climate model analyses''', Astronomy and Astrophysics, 704, A286 (2025). DOI: https://doi.org/10.1051/0004-6361/202557330
*Lefèvre, M., S. Lebonnois, A. Spiga, and F. Forget, '''The Effect of Near-Surface Winds on Surface Temperature and Dust Transport on Venus''', Journal of Geophysical Research (Planets), 130, e2025JE009133 (2025). DOI: https://doi.org/10.1029/2025JE009133
*Egan, J. V., W. Feng, A. D. Jame, J. Manners, D. R. Marsh, S. Lebonnois, F. Lefèvre, A. Stolzenbach, and J. M. C. Plane, '''Is OSSO a Significant Contributor to the Unknown UV Absorber in Venus' Atmosphere?''', Geophysical Research Letters, 52, e2024GL113090 (2025). DOI: https://doi.org/10.1029/2024GL113090
*Cohen, M., J. Holmes, S. Lewis, M. Patel, and S. Lebonnois, '''Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation''', The Astrophysical Journal, 980, L11 (2025). DOI: https://doi.org/10.3847/2041-8213/adade9

==== 2024 ====
*Martinez, A., J.-Y. Chaufray, S. Lebonnois, F. Gonzàlez-Galindo, F. Lefèvre, and G. Gilli, '''Three-dimensional Venusian ionosphere model''', Icarus, 415, 116035 (2024). DOI: https://doi.org/10.1016/j.icarus.2024.116035
*Lai, D., S. Lebonnois, and T. Li, '''Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM''', Journal of Geophysical Research (Planets), 129, e2023JE008253 (2024). DOI: https://doi.org/10.1029/2023JE008253
*Lefèvre, M., F. Lefèvre, E. Marcq, A. Määttänen, A. Stolzenbach, and N. Streel, '''Impact of the Turbulent Vertical Mixing on Chemical and Cloud Species in the Venus Cloud Layer''', Geophysical Research Letters, 51, e2024GL108771 (2024). DOI: https://doi.org/10.1029/2024GL108771
==== 2023 ====
* Stolzenbach, A.; Lefèvre, F.; Lebonnois, S. and Määttänen, A., '''Three-dimensional modeling of Venus photochemistry and clouds''', Icarus, vol.395, pp.115447 (2023). DOI: https://doi.org/10.1016/j.icarus.2023.115447
* Martinez, A.; Lebonnois, S.; Millour, E.; Pierron, T.; Moisan, E.; Gilli, G. and Lefèvre, F., '''Exploring the variability of the venusian thermosphere with the IPSL Venus GCM''', Icarus, vol.389, pp.115272 (2023). DOI: https://doi.org/10.1016/j.icarus.2022.115272
==== 2022 ====
* Lefèvre, M.; Marcq, E. and F. Lefèvre., F. , '''The Impact of Turbulent Vertical Mixing in the Venus Clouds on Chemical Tracers''', Icarus, 86, 115148 (2022). DOI: https://doi.org/10.1016/j.icarus.2022.115148
* Lefèvre, M., '''Venus boundary layer dynamics: eolian transport and convective vortex''', Icarus, 387, 115167 (2022) DOI: https://doi.org/10.1016/j.icarus.2022.115167
==== 2021 ====
* Navarro, T.; Gilli, G.; Schubert, G.; Lebonnois, S.; Lefèvre, F. and Quirino, D., '''Venus' upper atmosphere revealed by a GCM: I. Structure and variability of the circulation''', Icarus, vol.366, pp.114400 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114400
* Gilli, G.; Navarro, T.; Lebonnois, S.; Quirino, D.; Silva, V.; Stolzenbach, A.; Lefèvre, F. and Schubert, G., '''Venus upper atmosphere revealed by a GCM: II. Model validation with temperature and density measurements''', Icarus, vol.366, pp.114432 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114432
==== 2020 ====
* Lefèvre, M.; Spiga, A. and Lebonnois, S., '''Mesoscale modeling of Venus' bow-shape waves''', Icarus, vol.335, pp.113376 (2020). DOI: https://doi.org/10.1016/j.icarus.2019.07.010
==== 2018 ====
* Lebonnois, S.; Schubert, G.; Forget, F. and Spiga, A., '''Planetary boundary layer and slope winds on Venus''', Icarus, vol.314, pp.149 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.06.006
* Garate-Lopez, I. and Lebonnois, S., '''Latitudinal variation of clouds' structure responsible for Venus' cold collar''', Icarus, vol.314, pp.1 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.05.011
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.487 (2018). DOI: https://doi.org/10.1038/s41561-018-0157-x
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.965 (2018). DOI: https://doi.org/10.1038/s41561-018-0257-7
* Lefèvre, M.; Lebonnois, S. and Spiga, A., '''Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear''', Journal of Geophysical Research (Planets), vol.123, pp.2773 (2018). DOI: https://doi.org/10.1029/2018JE005679

[[Category:Venus-Model]]
[[Category:Venus-LMDZ]]

Overview of the Venus PCM

2026-03-23T11:13:30Z

Mlefevre:

Welcome to the overview page of the Venus Planetary Climate Model

== The Venus PCM (Planetary Climate Model) ==

In a nutshell the Venus PCM is a suite of models combining the Venus physics package and a dynamical core which may be LMDZ (the historical lon-lat grid), DYNAMICO (a more recent icosahedral dynamical core) or [[WRF dynamical core for LES/mesoscale simulations|'''WRF''']] (limited area dynamical core).

== Getting started ==
The traditional Venus PCM - LMDZ (formerly know as the IPSL Venus GCM) is the most commonly used version. For a first try at installing running the Venus PCM we recommend you start from the [[Quick Install and Run Venus PCM]] page. You will also most likely be interested in all the pages tagged as "Venus-Model" or "Venus-LMDZ" in the [[Special:Categories|Categories]] section.

== POULDP Venus ==
A POULDP meeting, for Point Organisé et Utile LMDZ Dynamico Planéto (apologies to non-French speakers), is organized between the developers to discuss the development of the model and plan improvements.
To subscribe to the POULDP mailing list (and/or browse through past messages): https://groupes.renater.fr/sympa/info/pouldp_venus

== Bibliography ==

Some recent reference articles:
==== 2026 ====
*Martinez, A., H. Karyu, A. Brecht, G. Gilli, S. Lebonnois, T. Kuroda, A. Stolzenbach, F. González-Galindo, S. Bougher, and H. Fujiwara, '''Comparison of General Circulation Models of the Venus upper atmosphere''', Icarus, 447, 116901 (2026). DOI: https://doi.org/10.1016/j.icarus.2025.116901
*Martinez, A., G. Gilli, A. Stolzenbach, T. Navarro, F. Lefèvre, S. Lebonnois, and N. Streel, '''New Insight on the Global Dynamics in the "Transition Region" of Venus Atmosphere (80─130 km) With a 3D Model''', Journal of Geophysical Research (Planets), 131, e2025JE009313 (2026). DOI: https://doi.org/10.1029/2025JE009313
==== 2025 ====
*Lai, D., T. Li, S. Lebonnois, and M. Lefèvre, '''Stationary wave dynamics in Venus's upper clouds: Morphology and forcing from Akatsuki/LIR and Venus planetary climate model analyses''', Astronomy and Astrophysics, 704, A286 (2025). DOI: https://doi.org/10.1051/0004-6361/202557330
*Lefèvre, M., S. Lebonnois, A. Spiga, and F. Forget, '''The Effect of Near-Surface Winds on Surface Temperature and Dust Transport on Venus''', Journal of Geophysical Research (Planets), 130, e2025JE009133 (2025). DOI: https://doi.org/10.1029/2025JE009133
*Egan, J. V., W. Feng, A. D. Jame, J. Manners, D. R. Marsh, S. Lebonnois, F. Lefèvre, A. Stolzenbach, and J. M. C. Plane, '''Is OSSO a Significant Contributor to the Unknown UV Absorber in Venus' Atmosphere?''', Geophysical Research Letters, 52, e2024GL113090 (2025). DOI: https://doi.org/10.1029/2024GL113090
*Cohen, M., J. Holmes, S. Lewis, M. Patel, and S. Lebonnois, '''Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation''', The Astrophysical Journal, 980, L11 (2025). DOI: https://doi.org/10.3847/2041-8213/adade9

==== 2024 ====
*Martinez, A., J.-Y. Chaufray, S. Lebonnois, F. Gonzàlez-Galindo, F. Lefèvre, and G. Gilli, '''Three-dimensional Venusian ionosphere model''', Icarus, 415, 116035 (2024). DOI: https://doi.org/10.1016/j.icarus.2024.116035
*Lai, D., S. Lebonnois, and T. Li, '''Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM''', Journal of Geophysical Research (Planets), 129, e2023JE008253 (2024). DOI: https://doi.org/10.1029/2023JE008253
*Lefèvre, M., F. Lefèvre, E. Marcq, A. Määttänen, A. Stolzenbach, and N. Streel, '''Impact of the Turbulent Vertical Mixing on Chemical and Cloud Species in the Venus Cloud Layer''', Geophysical Research Letters, 51, e2024GL108771 (2024). DOI: https://doi.org/10.1029/2024GL108771
==== 2023 ====
* Stolzenbach, A.; Lefèvre, F.; Lebonnois, S. and Määttänen, A., '''Three-dimensional modeling of Venus photochemistry and clouds''', Icarus, vol.395, pp.115447 (2023). DOI: https://doi.org/10.1016/j.icarus.2023.115447
* Martinez, A.; Lebonnois, S.; Millour, E.; Pierron, T.; Moisan, E.; Gilli, G. and Lefèvre, F., '''Exploring the variability of the venusian thermosphere with the IPSL Venus GCM''', Icarus, vol.389, pp.115272 (2023). DOI: https://doi.org/10.1016/j.icarus.2022.115272
==== 2022 ====
* Lefèvre, M.; Marcq, E. and F. Lefèvre., F. , '''The Impact of Turbulent Vertical Mixing in the Venus Clouds on Chemical Tracers''', Icarus, 86, 115148 (2022). DOI: https://doi.org/10.1016/j.icarus.2022.115148
* Lefèvre, M., '''Venus boundary layer dynamics: eolian transport and convective vortex''', Icarus, 387, 115167 (2022) DOI: https://doi.org/10.1016/j.icarus.2022.115167
==== 2021 ====
* Navarro, T.; Gilli, G.; Schubert, G.; Lebonnois, S.; Lefèvre, F. and Quirino, D., '''Venus' upper atmosphere revealed by a GCM: I. Structure and variability of the circulation''', Icarus, vol.366, pp.114400 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114400
* Gilli, G.; Navarro, T.; Lebonnois, S.; Quirino, D.; Silva, V.; Stolzenbach, A.; Lefèvre, F. and Schubert, G., '''Venus upper atmosphere revealed by a GCM: II. Model validation with temperature and density measurements''', Icarus, vol.366, pp.114432 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114432
==== 2020 ====
* Lefèvre, M.; Spiga, A. and Lebonnois, S., '''Mesoscale modeling of Venus' bow-shape waves''', Icarus, vol.335, pp.113376 (2020). DOI: https://doi.org/10.1016/j.icarus.2019.07.010
==== 2018 ====
* Lebonnois, S.; Schubert, G.; Forget, F. and Spiga, A., '''Planetary boundary layer and slope winds on Venus''', Icarus, vol.314, pp.149 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.06.006
* Garate-Lopez, I. and Lebonnois, S., '''Latitudinal variation of clouds' structure responsible for Venus' cold collar''', Icarus, vol.314, pp.1 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.05.011
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.487 (2018). DOI: https://doi.org/10.1038/s41561-018-0157-x
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.965 (2018). DOI: https://doi.org/10.1038/s41561-018-0257-7
* Lefèvre, M.; Lebonnois, S. and Spiga, A., '''Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear''', Journal of Geophysical Research (Planets), vol.123, pp.2773 (2018). DOI: https://doi.org/10.1029/2018JE005679

[[Category:Venus-Model]]
[[Category:Venus-LMDZ]]

Overview of the Venus PCM

2026-03-23T11:03:51Z

Mlefevre: /* Bibliography */

Welcome to the overview page of the Venus Planetary Climate Model

== The Venus PCM (Planetary Climate Model) ==

In a nutshell the Venus PCM is a suite of models combining the Venus physics package and a dynamical core which may be LMDZ (the historical lon-lat grid), DYNAMICO (a more recent icosahedral dynamical core) or [[WRF dynamical core for LES/mesoscale simulations|'''WRF''']] (limited area dynamical core).

== Getting started ==
The traditional Venus PCM - LMDZ (formerly know as the IPSL Venus GCM) is the most commonly used version. For a first try at installing running the Venus PCM we recommend you start from the [[Quick Install and Run Venus PCM]] page. You will also most likely be interested in all the pages tagged as "Venus-Model" or "Venus-LMDZ" in the [[Special:Categories|Categories]] section.

== Bibliography ==

Some recent reference articles:
==== 2026 ====
*Martinez, A., H. Karyu, A. Brecht, G. Gilli, S. Lebonnois, T. Kuroda, A. Stolzenbach, F. González-Galindo, S. Bougher, and H. Fujiwara, '''Comparison of General Circulation Models of the Venus upper atmosphere''', Icarus, 447, 116901 (2026). DOI: https://doi.org/10.1016/j.icarus.2025.116901
*Martinez, A., G. Gilli, A. Stolzenbach, T. Navarro, F. Lefèvre, S. Lebonnois, and N. Streel, '''New Insight on the Global Dynamics in the "Transition Region" of Venus Atmosphere (80─130 km) With a 3D Model''', Journal of Geophysical Research (Planets), 131, e2025JE009313 (2026). DOI: https://doi.org/10.1029/2025JE009313
==== 2025 ====
*Lai, D., T. Li, S. Lebonnois, and M. Lefèvre, '''Stationary wave dynamics in Venus's upper clouds: Morphology and forcing from Akatsuki/LIR and Venus planetary climate model analyses''', Astronomy and Astrophysics, 704, A286 (2025). DOI: https://doi.org/10.1051/0004-6361/202557330
*Lefèvre, M., S. Lebonnois, A. Spiga, and F. Forget, '''The Effect of Near-Surface Winds on Surface Temperature and Dust Transport on Venus''', Journal of Geophysical Research (Planets), 130, e2025JE009133 (2025). DOI: https://doi.org/10.1029/2025JE009133
*Egan, J. V., W. Feng, A. D. Jame, J. Manners, D. R. Marsh, S. Lebonnois, F. Lefèvre, A. Stolzenbach, and J. M. C. Plane, '''Is OSSO a Significant Contributor to the Unknown UV Absorber in Venus' Atmosphere?''', Geophysical Research Letters, 52, e2024GL113090 (2025). DOI: https://doi.org/10.1029/2024GL113090
*Cohen, M., J. Holmes, S. Lewis, M. Patel, and S. Lebonnois, '''Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation''', The Astrophysical Journal, 980, L11 (2025). DOI: https://doi.org/10.3847/2041-8213/adade9

==== 2024 ====
*Martinez, A., J.-Y. Chaufray, S. Lebonnois, F. Gonzàlez-Galindo, F. Lefèvre, and G. Gilli, '''Three-dimensional Venusian ionosphere model''', Icarus, 415, 116035 (2024). DOI: https://doi.org/10.1016/j.icarus.2024.116035
*Lai, D., S. Lebonnois, and T. Li, '''Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM''', Journal of Geophysical Research (Planets), 129, e2023JE008253 (2024). DOI: https://doi.org/10.1029/2023JE008253
*Lefèvre, M., F. Lefèvre, E. Marcq, A. Määttänen, A. Stolzenbach, and N. Streel, '''Impact of the Turbulent Vertical Mixing on Chemical and Cloud Species in the Venus Cloud Layer''', Geophysical Research Letters, 51, e2024GL108771 (2024). DOI: https://doi.org/10.1029/2024GL108771
==== 2023 ====
* Stolzenbach, A.; Lefèvre, F.; Lebonnois, S. and Määttänen, A., '''Three-dimensional modeling of Venus photochemistry and clouds''', Icarus, vol.395, pp.115447 (2023). DOI: https://doi.org/10.1016/j.icarus.2023.115447
* Martinez, A.; Lebonnois, S.; Millour, E.; Pierron, T.; Moisan, E.; Gilli, G. and Lefèvre, F., '''Exploring the variability of the venusian thermosphere with the IPSL Venus GCM''', Icarus, vol.389, pp.115272 (2023). DOI: https://doi.org/10.1016/j.icarus.2022.115272
==== 2022 ====
* Lefèvre, M.; Marcq, E. and F. Lefèvre., F. , '''The Impact of Turbulent Vertical Mixing in the Venus Clouds on Chemical Tracers''', Icarus, 86, 115148 (2022). DOI: https://doi.org/10.1016/j.icarus.2022.115148
* Lefèvre, M., '''Venus boundary layer dynamics: eolian transport and convective vortex''', Icarus, 387, 115167 (2022) DOI: https://doi.org/10.1016/j.icarus.2022.115167
==== 2021 ====
* Navarro, T.; Gilli, G.; Schubert, G.; Lebonnois, S.; Lefèvre, F. and Quirino, D., '''Venus' upper atmosphere revealed by a GCM: I. Structure and variability of the circulation''', Icarus, vol.366, pp.114400 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114400
* Gilli, G.; Navarro, T.; Lebonnois, S.; Quirino, D.; Silva, V.; Stolzenbach, A.; Lefèvre, F. and Schubert, G., '''Venus upper atmosphere revealed by a GCM: II. Model validation with temperature and density measurements''', Icarus, vol.366, pp.114432 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114432
==== 2020 ====
* Lefèvre, M.; Spiga, A. and Lebonnois, S., '''Mesoscale modeling of Venus' bow-shape waves''', Icarus, vol.335, pp.113376 (2020). DOI: https://doi.org/10.1016/j.icarus.2019.07.010
==== 2018 ====
* Lebonnois, S.; Schubert, G.; Forget, F. and Spiga, A., '''Planetary boundary layer and slope winds on Venus''', Icarus, vol.314, pp.149 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.06.006
* Garate-Lopez, I. and Lebonnois, S., '''Latitudinal variation of clouds' structure responsible for Venus' cold collar''', Icarus, vol.314, pp.1 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.05.011
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.487 (2018). DOI: https://doi.org/10.1038/s41561-018-0157-x
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.965 (2018). DOI: https://doi.org/10.1038/s41561-018-0257-7
* Lefèvre, M.; Lebonnois, S. and Spiga, A., '''Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear''', Journal of Geophysical Research (Planets), vol.123, pp.2773 (2018). DOI: https://doi.org/10.1029/2018JE005679

[[Category:Venus-Model]]
[[Category:Venus-LMDZ]]

Overview of the Venus PCM

2026-03-23T11:02:11Z

Mlefevre: /* 2025 */

Welcome to the overview page of the Venus Planetary Climate Model

== The Venus PCM (Planetary Climate Model) ==

In a nutshell the Venus PCM is a suite of models combining the Venus physics package and a dynamical core which may be LMDZ (the historical lon-lat grid), DYNAMICO (a more recent icosahedral dynamical core) or [[WRF dynamical core for LES/mesoscale simulations|'''WRF''']] (limited area dynamical core).

== Getting started ==
The traditional Venus PCM - LMDZ (formerly know as the IPSL Venus GCM) is the most commonly used version. For a first try at installing running the Venus PCM we recommend you start from the [[Quick Install and Run Venus PCM]] page. You will also most likely be interested in all the pages tagged as "Venus-Model" or "Venus-LMDZ" in the [[Special:Categories|Categories]] section.

== Bibliography ==

Some recent reference articles:
==== 2025 ====
*Lai, D., T. Li, S. Lebonnois, and M. Lefèvre, '''Stationary wave dynamics in Venus's upper clouds: Morphology and forcing from Akatsuki/LIR and Venus planetary climate model analyses''', Astronomy and Astrophysics, 704, A286 (2025). DOI: https://doi.org/10.1051/0004-6361/202557330
*Lefèvre, M., S. Lebonnois, A. Spiga, and F. Forget, '''The Effect of Near-Surface Winds on Surface Temperature and Dust Transport on Venus''', Journal of Geophysical Research (Planets), 130, e2025JE009133 (2025). DOI: https://doi.org/10.1029/2025JE009133
*Egan, J. V., W. Feng, A. D. Jame, J. Manners, D. R. Marsh, S. Lebonnois, F. Lefèvre, A. Stolzenbach, and J. M. C. Plane, '''Is OSSO a Significant Contributor to the Unknown UV Absorber in Venus' Atmosphere?''', Geophysical Research Letters, 52, e2024GL113090 (2025). DOI: https://doi.org/10.1029/2024GL113090
*Cohen, M., J. Holmes, S. Lewis, M. Patel, and S. Lebonnois, '''Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation''', The Astrophysical Journal, 980, L11 (2025). DOI: https://doi.org/10.3847/2041-8213/adade9

==== 2024 ====
*Martinez, A., J.-Y. Chaufray, S. Lebonnois, F. Gonzàlez-Galindo, F. Lefèvre, and G. Gilli, '''Three-dimensional Venusian ionosphere model''', Icarus, 415, 116035 (2024). DOI: https://doi.org/10.1016/j.icarus.2024.116035
*Lai, D., S. Lebonnois, and T. Li, '''Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM''', Journal of Geophysical Research (Planets), 129, e2023JE008253 (2024). DOI: https://doi.org/10.1029/2023JE008253
*Lefèvre, M., F. Lefèvre, E. Marcq, A. Määttänen, A. Stolzenbach, and N. Streel, '''Impact of the Turbulent Vertical Mixing on Chemical and Cloud Species in the Venus Cloud Layer''', Geophysical Research Letters, 51, e2024GL108771 (2024). DOI: https://doi.org/10.1029/2024GL108771
==== 2023 ====
* Stolzenbach, A.; Lefèvre, F.; Lebonnois, S. and Määttänen, A., '''Three-dimensional modeling of Venus photochemistry and clouds''', Icarus, vol.395, pp.115447 (2023). DOI: https://doi.org/10.1016/j.icarus.2023.115447
* Martinez, A.; Lebonnois, S.; Millour, E.; Pierron, T.; Moisan, E.; Gilli, G. and Lefèvre, F., '''Exploring the variability of the venusian thermosphere with the IPSL Venus GCM''', Icarus, vol.389, pp.115272 (2023). DOI: https://doi.org/10.1016/j.icarus.2022.115272
==== 2022 ====
* Lefèvre, M.; Marcq, E. and F. Lefèvre., F. , '''The Impact of Turbulent Vertical Mixing in the Venus Clouds on Chemical Tracers''', Icarus, 86, 115148 (2022). DOI: https://doi.org/10.1016/j.icarus.2022.115148
* Lefèvre, M., '''Venus boundary layer dynamics: eolian transport and convective vortex''', Icarus, 387, 115167 (2022) DOI: https://doi.org/10.1016/j.icarus.2022.115167
==== 2021 ====
* Navarro, T.; Gilli, G.; Schubert, G.; Lebonnois, S.; Lefèvre, F. and Quirino, D., '''Venus' upper atmosphere revealed by a GCM: I. Structure and variability of the circulation''', Icarus, vol.366, pp.114400 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114400
* Gilli, G.; Navarro, T.; Lebonnois, S.; Quirino, D.; Silva, V.; Stolzenbach, A.; Lefèvre, F. and Schubert, G., '''Venus upper atmosphere revealed by a GCM: II. Model validation with temperature and density measurements''', Icarus, vol.366, pp.114432 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114432
==== 2020 ====
* Lefèvre, M.; Spiga, A. and Lebonnois, S., '''Mesoscale modeling of Venus' bow-shape waves''', Icarus, vol.335, pp.113376 (2020). DOI: https://doi.org/10.1016/j.icarus.2019.07.010
==== 2018 ====
* Lebonnois, S.; Schubert, G.; Forget, F. and Spiga, A., '''Planetary boundary layer and slope winds on Venus''', Icarus, vol.314, pp.149 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.06.006
* Garate-Lopez, I. and Lebonnois, S., '''Latitudinal variation of clouds' structure responsible for Venus' cold collar''', Icarus, vol.314, pp.1 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.05.011
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.487 (2018). DOI: https://doi.org/10.1038/s41561-018-0157-x
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.965 (2018). DOI: https://doi.org/10.1038/s41561-018-0257-7
* Lefèvre, M.; Lebonnois, S. and Spiga, A., '''Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear''', Journal of Geophysical Research (Planets), vol.123, pp.2773 (2018). DOI: https://doi.org/10.1029/2018JE005679

[[Category:Venus-Model]]
[[Category:Venus-LMDZ]]

Overview of the Venus PCM

2025-07-09T09:00:32Z

Mlefevre: /* Bibliography */

Welcome to the overview page of the Venus Planetary Climate Model

== The Venus PCM (Planetary Climate Model) ==

In a nutshell the Venus PCM is a suite of models combining the Venus physics package and a dynamical core which may be LMDZ (the historical lon-lat grid), DYNAMICO (a more recent icosahedral dynamical core) or [[WRF dynamical core for LES/mesoscale simulations|'''WRF''']] (limited area dynamical core).

== Getting started ==
The traditional Venus PCM - LMDZ (formerly know as the IPSL Venus GCM) is the most commonly used version. For a first try at installing running the Venus PCM we recommend you start from the [[Quick Install and Run Venus PCM]] page. You will also most likely be interested in all the pages tagged as "Venus-Model" or "Venus-LMDZ" in the [[Special:Categories|Categories]] section.

== Bibliography ==

Some recent reference articles:
==== 2025 ====
*Cohen, M., J. Holmes, S. Lewis, M. Patel, and S. Lebonnois, '''Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation''', The Astrophysical Journal, 980, L11 (2025). DOI: https://doi.org/10.3847/2041-8213/adade9
==== 2024 ====
*Martinez, A., J.-Y. Chaufray, S. Lebonnois, F. Gonzàlez-Galindo, F. Lefèvre, and G. Gilli, '''Three-dimensional Venusian ionosphere model''', Icarus, 415, 116035 (2024). DOI: https://doi.org/10.1016/j.icarus.2024.116035
*Lai, D., S. Lebonnois, and T. Li, '''Planetary-Scale Wave Activity in Venus Cloud Layer Simulated by the Venus PCM''', Journal of Geophysical Research (Planets), 129, e2023JE008253 (2024). DOI: https://doi.org/10.1029/2023JE008253
*Lefèvre, M., F. Lefèvre, E. Marcq, A. Määttänen, A. Stolzenbach, and N. Streel, '''Impact of the Turbulent Vertical Mixing on Chemical and Cloud Species in the Venus Cloud Layer''', Geophysical Research Letters, 51, e2024GL108771 (2024). DOI: https://doi.org/10.1029/2024GL108771
==== 2023 ====
* Stolzenbach, A.; Lefèvre, F.; Lebonnois, S. and Määttänen, A., '''Three-dimensional modeling of Venus photochemistry and clouds''', Icarus, vol.395, pp.115447 (2023). DOI: https://doi.org/10.1016/j.icarus.2023.115447
* Martinez, A.; Lebonnois, S.; Millour, E.; Pierron, T.; Moisan, E.; Gilli, G. and Lefèvre, F., '''Exploring the variability of the venusian thermosphere with the IPSL Venus GCM''', Icarus, vol.389, pp.115272 (2023). DOI: https://doi.org/10.1016/j.icarus.2022.115272
==== 2022 ====
* Lefèvre, M.; Marcq, E. and F. Lefèvre., F. , '''The Impact of Turbulent Vertical Mixing in the Venus Clouds on Chemical Tracers''', Icarus, 86, 115148 (2022). DOI: https://doi.org/10.1016/j.icarus.2022.115148
* Lefèvre, M., '''Venus boundary layer dynamics: eolian transport and convective vortex''', Icarus, 387, 115167 (2022) DOI: https://doi.org/10.1016/j.icarus.2022.115167
==== 2021 ====
* Navarro, T.; Gilli, G.; Schubert, G.; Lebonnois, S.; Lefèvre, F. and Quirino, D., '''Venus' upper atmosphere revealed by a GCM: I. Structure and variability of the circulation''', Icarus, vol.366, pp.114400 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114400
* Gilli, G.; Navarro, T.; Lebonnois, S.; Quirino, D.; Silva, V.; Stolzenbach, A.; Lefèvre, F. and Schubert, G., '''Venus upper atmosphere revealed by a GCM: II. Model validation with temperature and density measurements''', Icarus, vol.366, pp.114432 (2021). DOI: https://doi.org/10.1016/j.icarus.2021.114432
==== 2020 ====
* Lefèvre, M.; Spiga, A. and Lebonnois, S., '''Mesoscale modeling of Venus' bow-shape waves''', Icarus, vol.335, pp.113376 (2020). DOI: https://doi.org/10.1016/j.icarus.2019.07.010
==== 2018 ====
* Lebonnois, S.; Schubert, G.; Forget, F. and Spiga, A., '''Planetary boundary layer and slope winds on Venus''', Icarus, vol.314, pp.149 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.06.006
* Garate-Lopez, I. and Lebonnois, S., '''Latitudinal variation of clouds' structure responsible for Venus' cold collar''', Icarus, vol.314, pp.1 (2018). DOI: https://doi.org/10.1016/j.icarus.2018.05.011
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.487 (2018). DOI: https://doi.org/10.1038/s41561-018-0157-x
* Navarro, T.; Schubert, G. and Lebonnois, S., '''Author Correction: Atmospheric mountain wave generation on Venus and its influence on the solid planet's rotation rate''', Nature Geoscience, vol.11, pp.965 (2018). DOI: https://doi.org/10.1038/s41561-018-0257-7
* Lefèvre, M.; Lebonnois, S. and Spiga, A., '''Three-Dimensional Turbulence-Resolving Modeling of the Venusian Cloud Layer and Induced Gravity Waves: Inclusion of Complete Radiative Transfer and Wind Shear''', Journal of Geophysical Research (Planets), vol.123, pp.2773 (2018). DOI: https://doi.org/10.1029/2018JE005679

[[Category:Venus-Model]]
[[Category:Venus-LMDZ]]

WRF dynamical core for LES/mesoscale simulations

2025-06-19T11:59:01Z

Mlefevre: /* Studies with PCM+WRF */

== Introduction ==

WRF is a mesoscale numerical weather prediction system designed for both atmospheric research and operational forecasting applications over the Earth's atmosphere: see [https://www.mmm.ucar.edu/models/wrf WRF presentation].

In the PCM, we take advantage of the dynamical core of the WRF model to run LES (large-eddy simulations) or mesoscale simulations.

To do so, we take the WRF model, remove all its physical packages related to the Earth's atmosphere, and plug in the physical package from the PCM (either Venus, Mars, Titan, or Generic).

A description of the various equations solved by WRF can be found here: [https://opensky.ucar.edu/islandora/object/technotes%3A588 Skamarock et al. (2019, 2021)].

== Studies with PCM+WRF ==

Descriptions of the application of WRF dynamical core with the PCM can be found in:

- [https://theses.hal.science/tel-04861192 Noé CLEMENT's PhD thesis] (chapter 3) for the Generic PCM.

- [https://theses.hal.science/tel-02924996 Maxence Lefevre's PhD thesis] for the Venus PCM.

- [https://theses.hal.science/tel-00347021 Aymeric Spiga's PhD thesis] for the Mars PCM

Studies with the PCM coupled to the WRF dynamical core have been done using WRF V2, WRF V3, WRF V4.

Our aim is now to use WRF V4 as much as possible, which offers significant improvements in terms of numerical schemes in particular.

Here is a list of studies using the PCM coupled to the WRF dynamical core:

<table border="1">
<tr>
<th>Planet</th>
<th>Reference</th>
<th>Physical package</th>
<th>Dynamical core</th>
</tr>
<tr>
<td>Mars</td>
<td>[https://doi.org/10.1029/2008JE003242 Spiga and Forget (2009)]</td>
<td>Mars PCM</td>
<td>WRF V2</td>
</tr>
<tr>
<td>Mars</td>
<td>[https://rmets.onlinelibrary.wiley.com/doi/10.1002/qj.563 Spiga et al. (2010)]</td>
<td>Mars PCM</td>
<td>WRF V3</td>
</tr>
<tr>
<td>Venus</td>
<td>[https://agupubs.onlinelibrary.wiley.com/doi/abs/10.1029/2018JE005679 Lefèvre et al. (2018)]</td>
<td>Venus PCM</td>
<td>WRF V3</td>
</tr>
<tr>
<td>Venus</td>
<td>[https://www.sciencedirect.com/science/article/pii/S0019103519301216?via%3Dihub Lefèvre et al. (2020)]</td>
<td>Venus PCM</td>
<td>WRF V2</td>
</tr>
<tr>
<td>Exoplanets</td>
<td>[https://iopscience.iop.org/article/10.3847/1538-4357/abf2c1 Lefèvre et al. (2021)]</td>
<td>Generic PCM</td>
<td>WRF V3</td>
</tr>
<tr>
<td>Exoplanets</td>
<td>[https://doi.org/10.1051/0004-6361/202348928 Leconte et al. (2024)]</td>
<td>Generic PCM</td>
<td>WRF V4</td>
</tr>
<tr>
<td>Uranus, Neptune</td>
<td>[https://doi.org/10.1051/0004-6361/202348936 Clément et al. (2024)]</td>
<td>Generic PCM</td>
<td>WRF V4</td>
</tr>
</table>

== Remarks ==

For advanced users:

When compiling the model, the flags:

<syntaxhighlight lang="text">
#ifndef MESOSCALE
use ...
#else
use ...
</syntaxhighlight>

select lines compiled depending on the configuration.

== WRF equations ==

Below is a synthesis of equations solved by WRF.

[[File:WRF_dynamical_core.png]]

== Installing PCM+WRF ==

=== Terrestrial WRF ===

Compiling terrestrial [https://www2.mmm.ucar.edu/wrf/OnLineTutorial/compilation_tutorial.php WRF] is a good first step.
git clone --recurse-submodules https://github.com/wrf-model/WRF

=== WRF+PCM ===

On ADASTRA

[[Category:Generic-Model]]
[[Category:Mars-Model]]
[[Category:Venus-Model]]
[[Category:Titan-Model]]

Using MeSU

2023-12-13T13:45:20Z

Mlefevre: /* Compiling the WRF on MeSU */

This page provides some information for those who use the Sorbonne Université clusters MeSU

== How to access the cluster ==
You need first to open an account (this is of course reserved to people in labs connected to Sorbonne Université) then proceed to this page: https://sacado.sorbonne-universite.fr/mesu/index.php/accounts-and-access/

Once you have an account you can ssh to the cluster :
<syntaxhighlight lang="bash">
ssh username@mesu.dsi.upmc.fr
</syntaxhighlight>

For people not on linux : https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/how-to-connect-to-mesu/

== OS and disk space ==
As the welcome message will remind you:
<pre>
__ __ ____ _ _
| \/ | ___/ ___|| | | |
| |\/| |/ _ \___ \| | | |
| | | | __/___) | |_| |
|_| |_|\___|____/ \___/

⢎⡑ ⢀⡀ ⡀⣀ ⣇⡀ ⢀⡀ ⣀⡀ ⣀⡀ ⢀⡀ ⡇⢸ ⣀⡀ ⠄ ⡀⢀ ⢀⡀ ⡀⣀ ⢀⣀ ⠄ ⣰⡀ ⢠⡂
⠢⠜ ⠣⠜ ⠏ ⠧⠜ ⠣⠜ ⠇⠸ ⠇⠸ ⠣⠭ ⠣⠜ ⠇⠸ ⠇ ⠱⠃ ⠣⠭ ⠏ ⠭⠕ ⠇ ⠘⠤ ⠣⠭

https://sacado.sorbonne-universite.fr/mesu
mesu@sorbonne-universite.fr

beta: 144x 24 Intel Haswell CPUs, 128 GB RAM
gamma: 2x 12 Intel Haswell CPUs, 2 NVidia K5200, 256 GB RAM
</pre>
This is Ubuntu Linux and the "HOME" is quite limited in size. Most work should be done on the '''/scratchbeta''' disks.

It is up to you to tailor your environment. By default it is quite bare; it is up to you to load the modules you'll need to have access to specific software or compilers or libraries (and versions thereof).
To know what modules are available:
<syntaxhighlight lang="bash">
module avail
</syntaxhighlight>
To load a given module, here the Panoply software:
<syntaxhighlight lang="bash">
module load panoply
</syntaxhighlight>

The list of available software is available at https://sacado.sorbonne-universite.fr/mesu/index.php/usage/available-software/

== Compiling the PCMs on MeSU ==

To do

== Compiling WRF on MeSU ==

To do

Environment:
<syntaxhighlight lang="bash">
module load intel/intel-compilers-18.2/18.2
module load intel/intel-mpi/2018.2
module load intel/intel-cmkl-18.0/18.0
export NETCDF="/home/lefevrema/NETCDF/netcdf-4.0.1"
export NETCDF_INCDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/include/"
export NETCDF_LIBDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/lib/"
export WHERE_MPI="/opt/dev/intel/2018_Update2/impi/2018.2.199/bin64"
</syntaxhighlight>

== Submit your job ==
MeSU Supercomputer uses a queuing system to match users jobs with available computing resources.

Users submit their programs to the job scheduler (PBS), which maintains a queue of jobs and distributes them on the compute nodes according to the servers status, scheduling policies and jobs parameters (number of compute nodes / cores, estimated execution time, required memory, etc.).

The interface with PBS is done via a text file – the PBS script – created by the user, which will define your job requirements and execution steps. This file is mainly comprised of two sections :
* the header in which you specify the job requirements (execution time, number of CPU cores to use, memory requirements…) in the form of PBS directives
* the body in which you will write the commands to load specific software, define environment variables, and run your job.

More information https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/job-submission/

Here is an example of job script to run using 24 cpus:
<syntaxhighlight lang="bash">
#!/bin/bash
#PBS -q beta
#PBS -l select=1:ncpus=24
#PBS -l place=free:exclhost
#PBS -l walltime=23:59:00
#PBS -N RUN_GCM
#PBS -j oe

# Load your environment
source ../trunk/LMDZ.COMMON/arch/arch-X64_MESU.env

# Go to job directory
cd $PBS_O_WORKDIR
cd ./RUN_DIR

#Magic trick
ulimit -s unlimited

mpirun gcm.e > gcm.out 2>&1
</syntaxhighlight>

Submitting your job to the PBS scheduler is easy once you have authored the corresponding PBS script file, using the qsub command:

<syntaxhighlight lang="bash">
qsub ./myScript
</syntaxhighlight>

[[Category:FAQ]]

Using MeSU

2023-12-13T13:45:10Z

Mlefevre: Changed the arch in the job script

This page provides some information for those who use the Sorbonne Université clusters MeSU

== How to access the cluster ==
You need first to open an account (this is of course reserved to people in labs connected to Sorbonne Université) then proceed to this page: https://sacado.sorbonne-universite.fr/mesu/index.php/accounts-and-access/

Once you have an account you can ssh to the cluster :
<syntaxhighlight lang="bash">
ssh username@mesu.dsi.upmc.fr
</syntaxhighlight>

For people not on linux : https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/how-to-connect-to-mesu/

== OS and disk space ==
As the welcome message will remind you:
<pre>
__ __ ____ _ _
| \/ | ___/ ___|| | | |
| |\/| |/ _ \___ \| | | |
| | | | __/___) | |_| |
|_| |_|\___|____/ \___/

⢎⡑ ⢀⡀ ⡀⣀ ⣇⡀ ⢀⡀ ⣀⡀ ⣀⡀ ⢀⡀ ⡇⢸ ⣀⡀ ⠄ ⡀⢀ ⢀⡀ ⡀⣀ ⢀⣀ ⠄ ⣰⡀ ⢠⡂
⠢⠜ ⠣⠜ ⠏ ⠧⠜ ⠣⠜ ⠇⠸ ⠇⠸ ⠣⠭ ⠣⠜ ⠇⠸ ⠇ ⠱⠃ ⠣⠭ ⠏ ⠭⠕ ⠇ ⠘⠤ ⠣⠭

https://sacado.sorbonne-universite.fr/mesu
mesu@sorbonne-universite.fr

beta: 144x 24 Intel Haswell CPUs, 128 GB RAM
gamma: 2x 12 Intel Haswell CPUs, 2 NVidia K5200, 256 GB RAM
</pre>
This is Ubuntu Linux and the "HOME" is quite limited in size. Most work should be done on the '''/scratchbeta''' disks.

It is up to you to tailor your environment. By default it is quite bare; it is up to you to load the modules you'll need to have access to specific software or compilers or libraries (and versions thereof).
To know what modules are available:
<syntaxhighlight lang="bash">
module avail
</syntaxhighlight>
To load a given module, here the Panoply software:
<syntaxhighlight lang="bash">
module load panoply
</syntaxhighlight>

The list of available software is available at https://sacado.sorbonne-universite.fr/mesu/index.php/usage/available-software/

== Compiling the PCMs on MeSU ==

To do

== Compiling the WRF on MeSU ==

To do

Environment:
<syntaxhighlight lang="bash">
module load intel/intel-compilers-18.2/18.2
module load intel/intel-mpi/2018.2
module load intel/intel-cmkl-18.0/18.0
export NETCDF="/home/lefevrema/NETCDF/netcdf-4.0.1"
export NETCDF_INCDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/include/"
export NETCDF_LIBDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/lib/"
export WHERE_MPI="/opt/dev/intel/2018_Update2/impi/2018.2.199/bin64"
</syntaxhighlight>

== Submit your job ==
MeSU Supercomputer uses a queuing system to match users jobs with available computing resources.

Users submit their programs to the job scheduler (PBS), which maintains a queue of jobs and distributes them on the compute nodes according to the servers status, scheduling policies and jobs parameters (number of compute nodes / cores, estimated execution time, required memory, etc.).

The interface with PBS is done via a text file – the PBS script – created by the user, which will define your job requirements and execution steps. This file is mainly comprised of two sections :
* the header in which you specify the job requirements (execution time, number of CPU cores to use, memory requirements…) in the form of PBS directives
* the body in which you will write the commands to load specific software, define environment variables, and run your job.

More information https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/job-submission/

Here is an example of job script to run using 24 cpus:
<syntaxhighlight lang="bash">
#!/bin/bash
#PBS -q beta
#PBS -l select=1:ncpus=24
#PBS -l place=free:exclhost
#PBS -l walltime=23:59:00
#PBS -N RUN_GCM
#PBS -j oe

# Load your environment
source ../trunk/LMDZ.COMMON/arch/arch-X64_MESU.env

# Go to job directory
cd $PBS_O_WORKDIR
cd ./RUN_DIR

#Magic trick
ulimit -s unlimited

mpirun gcm.e > gcm.out 2>&1
</syntaxhighlight>

Submitting your job to the PBS scheduler is easy once you have authored the corresponding PBS script file, using the qsub command:

<syntaxhighlight lang="bash">
qsub ./myScript
</syntaxhighlight>

[[Category:FAQ]]

Using MeSU

2023-12-13T13:43:48Z

Mlefevre: Creation of the page about the usage the MeSU computer

This page provides some information for those who use the Sorbonne Université clusters MeSU

== How to access the cluster ==
You need first to open an account (this is of course reserved to people in labs connected to Sorbonne Université) then proceed to this page: https://sacado.sorbonne-universite.fr/mesu/index.php/accounts-and-access/

Once you have an account you can ssh to the cluster :
<syntaxhighlight lang="bash">
ssh username@mesu.dsi.upmc.fr
</syntaxhighlight>

For people not on linux : https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/how-to-connect-to-mesu/

== OS and disk space ==
As the welcome message will remind you:
<pre>
__ __ ____ _ _
| \/ | ___/ ___|| | | |
| |\/| |/ _ \___ \| | | |
| | | | __/___) | |_| |
|_| |_|\___|____/ \___/

⢎⡑ ⢀⡀ ⡀⣀ ⣇⡀ ⢀⡀ ⣀⡀ ⣀⡀ ⢀⡀ ⡇⢸ ⣀⡀ ⠄ ⡀⢀ ⢀⡀ ⡀⣀ ⢀⣀ ⠄ ⣰⡀ ⢠⡂
⠢⠜ ⠣⠜ ⠏ ⠧⠜ ⠣⠜ ⠇⠸ ⠇⠸ ⠣⠭ ⠣⠜ ⠇⠸ ⠇ ⠱⠃ ⠣⠭ ⠏ ⠭⠕ ⠇ ⠘⠤ ⠣⠭

https://sacado.sorbonne-universite.fr/mesu
mesu@sorbonne-universite.fr

beta: 144x 24 Intel Haswell CPUs, 128 GB RAM
gamma: 2x 12 Intel Haswell CPUs, 2 NVidia K5200, 256 GB RAM
</pre>
This is Ubuntu Linux and the "HOME" is quite limited in size. Most work should be done on the '''/scratchbeta''' disks.

It is up to you to tailor your environment. By default it is quite bare; it is up to you to load the modules you'll need to have access to specific software or compilers or libraries (and versions thereof).
To know what modules are available:
<syntaxhighlight lang="bash">
module avail
</syntaxhighlight>
To load a given module, here the Panoply software:
<syntaxhighlight lang="bash">
module load panoply
</syntaxhighlight>

The list of available software is available at https://sacado.sorbonne-universite.fr/mesu/index.php/usage/available-software/

== Compiling the PCMs on MeSU ==

To do

== Compiling the WRF on MeSU ==

To do

Environment:
<syntaxhighlight lang="bash">
module load intel/intel-compilers-18.2/18.2
module load intel/intel-mpi/2018.2
module load intel/intel-cmkl-18.0/18.0
export NETCDF="/home/lefevrema/NETCDF/netcdf-4.0.1"
export NETCDF_INCDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/include/"
export NETCDF_LIBDIR="/home/lefevrema/NETCDF/netcdf-4.0.1/lib/"
export WHERE_MPI="/opt/dev/intel/2018_Update2/impi/2018.2.199/bin64"
</syntaxhighlight>

== Submit your job ==
MeSU Supercomputer uses a queuing system to match users jobs with available computing resources.

Users submit their programs to the job scheduler (PBS), which maintains a queue of jobs and distributes them on the compute nodes according to the servers status, scheduling policies and jobs parameters (number of compute nodes / cores, estimated execution time, required memory, etc.).

The interface with PBS is done via a text file – the PBS script – created by the user, which will define your job requirements and execution steps. This file is mainly comprised of two sections :
* the header in which you specify the job requirements (execution time, number of CPU cores to use, memory requirements…) in the form of PBS directives
* the body in which you will write the commands to load specific software, define environment variables, and run your job.

More information https://sacado.sorbonne-universite.fr/mesu/index.php/usage/howtos/job-submission/

Here is an example of job script to run using 24 cpus:
<syntaxhighlight lang="bash">
#!/bin/bash
#PBS -q beta
#PBS -l select=1:ncpus=24
#PBS -l place=free:exclhost
#PBS -l walltime=23:59:00
#PBS -N RUN_GCM
#PBS -j oe

# Load your environment
source ../trunk/LMDZ.COMMON/arch/arch-ifort_MESOIPSL.env

# Go to job directory
cd $PBS_O_WORKDIR
cd ./RUN_DIR

#Magic trick
ulimit -s unlimited

mpirun gcm.e > gcm.out 2>&1
</syntaxhighlight>

Submitting your job to the PBS scheduler is easy once you have authored the corresponding PBS script file, using the qsub command:

<syntaxhighlight lang="bash">
qsub ./myScript
</syntaxhighlight>

[[Category:FAQ]]

Overview of the Venus PCM

2023-10-19T12:32:34Z

Mlefevre: /* Bibliography */

Other GCM Configurations worth knowing about

2022-10-14T14:03:52Z

Mlefevre: /* Proxima b with LES */

== 3D lon-lat LMDZ setup ==

=== early Mars ===

It is already described in the [https://lmdz-forge.lmd.jussieu.fr/mediawiki/Planets/index.php/Quick_Install_and_Run ''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 (waiting for the SVN update by Ehouarn)

=== 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, to have a chance to model the equatorial oscillation, meridional cell circulations and/or a seasonal inter-hemispheric circulation, a giant planet GCM must also include a high vertical resolution. Indeed, 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. This implies that the propagation of dynamic instabilities, waves and turbulence should be resolved as far as possible along the vertical. Contrary to horizontal resolution, it doesn't really exist a criterion (similar to $$L_D$$) to determine the most suitable vertical grid resolution and still an adjustable parameter according to the processes to be represented. However, we advise the user to set a vertical resolution of at least 5 grid points per scale height as first stage.
Finally, these atmospheres are cold, with long radiative response time which needs radiative transfer computations over decade-long years of Jupiter (given that a Jupiter year $$\approx$$ 12 Earth years), Saturn ( a Saturn year $$\approx$$ 30 Earth years), Uranus (a Uranus year $$\approx$$ 84 earth years) or Neptune (a Neptune year $$\approx$$ 169 Earth years), depending on the chosen 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 numerically stable for massive parallel ressource computations: [[The_DYNAMICO_dynamical_core | 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
<syntaxhighlight lang="bash">
git clone https://gitlab.in2p3.fr/ipsl/projets/dynamico/dynamico.git ICOSAGCM
cd ICOSAGCM
git checkout 90f7138a60ebd3644fbbc42bc9dfa22923386385
</syntaxhighlight>

'''ICOSA_LMDZ''': the interface using to link LMDZ.GENERIC physical packages and ICOSAGCM
<syntaxhighlight lang="bash">
svn update -r 2655 -q ICOSA_LMDZ
</syntaxhighlight>

'''XIOS (XML Input Output Server)''': the library to interpolate input/output fields between the icosahedral and longitude/latitude regular grids on fly
<syntaxhighlight lang="bash">
svn co -r 2319 -q http://forge.ipsl.jussieu.fr/ioserver/svn/XIOS/trunk XIOS
</syntaxhighlight>

If you haven't already download '''LMDZ.COMMON''', '''LMDZ.GENERIC''', '''IOIPSL''', '''ARCH''', you can use the '''install.sh''' script provided by the Github repository.

Once each part of the GCM is downloaded, you are able to compile it.
Firstly, you have to define your [[The_Target_Architecture_("arch")_Files | target architecture file ]] (hereafter named YOUR_ARCH_FILE) where you will fill in all the necessary information about the local environment, where libraries are located, which compiler, and compiler options will be used, etc.
Some architecture files related to specific machines are provided in the '''ARCH''' directory.

The main specificity of DYNAMICO-giant is that every main parts of the model ('''ICOSAGCM''', '''LMDZ.COMMON''' and '''LMDZ.GENERIC''') are compiled as libraries, and settings and running configuration are managed by the '''ICOSA_LMDZ''' interface.

First, you have to compile '''IOIPSL''',
<syntaxhighlight lang="bash">
cd ../IOIPSL
./makeioipsl_fcm -prod -parallel -arch YOUR_ARCH_FILE -arch_path ../ARCH -j 8 -full
cd -
</syntaxhighlight>
then '''XIOS''' library,
<syntaxhighlight lang="bash">
cd ../XIOS
./make_xios --prod --arch YOUR_ARCH_FILE --arch_path ../ARCH --job 8 --full
cd -
</syntaxhighlight>
the physics packaging,
<syntaxhighlight lang="bash">
cd ../LMDZ.COMMON
./makelmdz_fcm -p std -p_opt "-b 20x25 -s 2" -prod -parallel mpi -libphy -io xios -arch YOUR_ARCH_FILE -arch_path ../ARCH -j 8 -full
cd -
</syntaxhighlight>
the dynamical core '''DYNAMICO''' (located in '''ICOSAGCM''' directory, named from the icosahedral shape of the horizontal mesh),
<syntaxhighlight lang="bash">
cd ../ICOSAGCM
./make_icosa -prod -parallel mpi -external_ioipsl -with_xios -arch YOUR_ARCH_FILE -arch_path ../ARCH -job 8 -full
cd -
</syntaxhighlight>
and finally the '''ICOSA_LMDZ''' interface
<syntaxhighlight lang="bash">
cd ../ICOSA_LMDZ
./build --job 8 --full
</syntaxhighlight>
and your executable programs should appeared in ''ICOSA_LMDZ/bin'' subdirectory, as:
'''icosa_lmdz.exe''' and '''xios_server.exe'''

All these compiling steps are summed up in ''make_isoca_lmdz'' program that should be adapted to your own computational settings.
<syntaxhighlight lang="bash">
./make_icosa_lmdz -p std -p_opt "-b 20x25 -s 2" -parallel mpi -arch YOUR_ARCH_FILE -arch_path ../ARCH -job 8 -full
</syntaxhighlight>

Now you can move your two executable files to your working directory and start to run your own simulation of Jupiter or a Hot Jupiter, as what follows.

Note: If you are using the GitHub file architecture (https://github.com/aymeric-spiga/dynamico-giant), you should be able to compile the model directly from your working directory (for instance Jupiter) by using the ''compile_occigen.sh'' program, which has to be adapted to your machine/cluster.

=== Jupiter with DYNAMICO ===
Using a new dynamical core implies new setting files, in addition or as a replacement of those relevant to '''LMDZ.COMMON''' dynamical core using.

There are two kind of setting files:

'''A first group relevant to DYNAMICO:'''

- [[The ''context_dynamico.xml'' Input File|''context_dynamico.xml'']]: Configuration file for '''DYNAMICO''' for reading and writing files using '''XIOS''', mainly used when you want to check the installation of '''ICOSAGCM''' with [[The_DYNAMICO_dynamical_core | an ''Held and Suarez'' test case]]. When your installation, compilation and run environment is fully functional, the dynamic core output files will not (necessarily) be useful and you can disable their writing.

- [[The context_input_dynamico.xml Input File|''context_input_dynamico.xml'']]:

- [[The file_def_dynamico.xml Input File|''file_def_dynamico.xml'']]: Definition of output diagnostic files which will be written into the output files only related to '''ICOSAGCM'''.

- [[The field_def_dynamico.xml Input File|''field_def_dynamico.xml'']]: Definition of all existing variables that can be output from DYNAMICO.

- [[The tracer.def Input File|''tracer.def'']]: Definition of the name and physico-chemical properties of the tracers which will be advected by the dynamical core. For now, there is two files related to tracers, we are working to harmonise it.

''' A second group relevant to LMDZ.GENERIC physical packages: '''

- [[The context_lmdz_physics.xml Input File|''context_lmdz_physics.xml'']]: File in which are defined the horizontal grid, vertical coordinate, output file(s) definition, with the setting of frequency output writing, time unit, geophysical variables to be written, etc. Each new geophysical variables added here have to be defined in the ''field_def_physics.xml'' file.

- [[The field_def_physics.xml Input File|''field_def_physics.xml'']]: Definition of all existing variables that can be output from the physical packages interfaced with '''DYNAMICO'''. This is where you will add each geophysical fields that you want to appear in the ''Xhistins.nc'' output files. For instance, related to the ''thermal plume scheme'' using for Jupiter's tropospheric dynamics, we have added the following variables:
<syntaxhighlight lang="xml" line>
<field id="h2o_vap"
long_name="Vapor mass mixing ratio"
unit="kg/kg" />
<field id="h2o_ice"
long_name="Vapor mass mixing ratio"
unit="kg/kg" />
<field id="detr"
long_name="Detrainment"
unit="kg/m2/s" />
<field id="entr"
long_name="Entrainment"
unit="kg/m2/s" />
<field id="w_plm"
long_name="Plume vertical velocity"
unit="m/s" />
</syntaxhighlight>

- [[The_callphys.def_Input_File|''callphys.def'']]: This setting file is used either with '''DYNAMICO''' or '''LMDZ.COMMON''' and allows the user to choose the physical parametrisation schemes and their appropriate main parameter values relevant to the planet being simulated. In our case of Jupiter, there are some specific parametrisations that should be added or modified from the example given as link at the beginning of this line:
<syntaxhighlight lang="bash" line>
# Diurnal cycle ? if diurnal=false, diurnally averaged solar heating
diurnal = .false. #.true.
# Seasonal cycle ? if season=false, Ls stays constant, to value set in "start"
season = .true.
# Tidally resonant orbit ? must have diurnal=false, correct rotation rate in newstart
tlocked = .false.
# Tidal resonance ratio ? ratio T_orbit to T_rotation
nres = 1
# Planet with rings?
rings_shadow = .false.
# Compute latitude-dependent gravity field??
oblate = .true.
# Include non-zero flattening (a-b)/a?
flatten = 0.06487
# Needed if oblate=.true.: J2
J2 = 0.01470
# Needed if oblate=.true.: Planet mean radius (m)
Rmean = 69911000.
# Needed if oblate=.true.: Mass of the planet (*1e24 kg)
MassPlanet = 1898.3
# use (read/write) a startfi.nc file? (default=.true.)
startphy_file = .false.
# constant value for surface albedo (if startphy_file = .false.)
surfalbedo = 0.0
# constant value for surface emissivity (if startphy_file = .false.)
surfemis = 1.0

# the rad. transfer is computed every "iradia" physical timestep
iradia = 160
# folder in which correlated-k data is stored ?
corrkdir = Jupiter_HITRAN2012_REY_ISO_NoKarko_T460K_article2019_gauss8p8_095
# Uniform absorption coefficient in radiative transfer?
graybody = .false.
# Characteristic planetary equilibrium (black body) temperature
# This is used only in the aerosol radiative transfer setup. (see aerave.F)
tplanet = 100.
# Output global radiative balance in file 'rad_bal.out' - slow for 1D!!
meanOLR = .false.
# Variable gas species: Radiatively active ?
varactive = .false.
# Computes atmospheric specific heat capacity and
# could calculated by the dynamics, set in callphys.def or calculeted from gases.def.
# You have to choose: 0 for dynamics (3d), 1 for forced in callfis (1d) or 2: computed from gases.def (1d)
# Force_cpp and check_cpp_match are now deprecated.
cpp_mugaz_mode = 0
# Specific heat capacity in J K-1 kg-1 [only used if cpp_mugaz_mode = 1]
cpp = 11500.
# Molecular mass in g mol-1 [only used if cpp_mugaz_mode = 1]
mugaz = 2.30
### DEBUG
# To not call abort when temperature is outside boundaries:
strictboundcorrk = .false.
# To not stop run when temperature is greater than 400 K for H2-H2 CIA dataset:
strictboundcia = .false.
# Add temperature sponge effect after radiative transfer?
callradsponge = .false.

Fat1AU = 1366.0

## Other physics options
## ~~~~~~~~~~~~~~~~~~~~~
# call turbulent vertical diffusion ?
calldifv = .false.
# use turbdiff instead of vdifc ?
UseTurbDiff = .true.
# call convective adjustment ?
calladj = .true.
# call thermal plume model ?
calltherm = .true.
# call thermal conduction in the soil ?
callsoil = .false.
# Internal heat flux (matters only if callsoil=F)
intheat = 7.48
# Remove lower boundary (e.g. for gas giant sims)
nosurf = .true.
#########################################################################
## extra non-standard definitions for Earth
#########################################################################

## Thermal plume model options
## ~~~~~~~~~~~~~~~~~~~~~~~~~~~
dvimpl = .true.
r_aspect_thermals = 2.0
tau_thermals = 0.0
betalpha = 0.9
afact = 0.7
fact_epsilon = 2.e-4
alpha_max = 0.7
fomass_max = 0.5
pres_limit = 2.e5

## Tracer and aerosol options
## ~~~~~~~~~~~~~~~~~~~~~~~~~~
# Ammonia cloud (Saturn/Jupiter)?
aeronh3 = .true.
size_nh3_cloud = 10.D-6
pres_nh3_cloud = 1.1D5 # old: 9.D4
tau_nh3_cloud = 10. # old: 15.
# Radiatively active aerosol (Saturn/Jupiter)?
aeroback2lay = .true.
optprop_back2lay_vis = optprop_jupiter_vis_n20.dat
optprop_back2lay_ir = optprop_jupiter_ir_n20.dat
obs_tau_col_tropo = 4.0
size_tropo = 5.e-7
pres_bottom_tropo = 8.0D4
pres_top_tropo = 1.8D4
obs_tau_col_strato = 0.1D0
# Auroral aerosols (Saturn/Jupiter)?
aeroaurora = .false.
size_aurora = 3.e-7
obs_tau_col_aurora = 2.0

# Radiatively active CO2 aerosol?
aeroco2 = .false.
# Fixed CO2 aerosol distribution?
aerofixco2 = .false.
# Radiatively active water aerosol?
aeroh2o = .false.
# Fixed water aerosol distribution?
aerofixh2o = .false.
# basic dust opacity
dusttau = 0.0
# Varying H2O cloud fraction?
CLFvarying = .false.
# H2O cloud fraction if fixed?
CLFfixval = 0.0
# fixed radii for cloud particles?
radfixed = .false.
# number mixing ratio of CO2 ice particles
Nmix_co2 = 100000.
# number mixing ratio of water particles (for rafixed=.false.)
Nmix_h2o = 1.e7
# number mixing ratio of water ice particles (for rafixed=.false.)
Nmix_h2o_ice = 5.e5
# radius of H2O water particles (for rafixed=.true.):
rad_h2o = 10.e-6
# radius of H2O ice particles (for rafixed=.true.):
rad_h2o_ice = 35.e-6
# atm mass update due to tracer evaporation/condensation?
mass_redistrib = .false.

## Water options
## ~~~~~~~~~~~~~
# Model water cycle
water = .true.
# Model water cloud formation
watercond = .true.
# Model water precipitation (including coagulation etc.)
waterrain = .true.
# Use simple precipitation scheme?
precip_scheme = 1
# Evaporate precipitation?
evap_prec = .true.
# multiplicative constant in Boucher 95 precip scheme
Cboucher = 1.
# Include hydrology ?
hydrology = .false.
# H2O snow (and ice) albedo ?
albedosnow = 0.6
# Maximum sea ice thickness ?
maxicethick = 10.
# Freezing point of seawater (degrees C) ?
Tsaldiff = 0.0
# Evolve surface water sources ?
sourceevol = .false.

## CO2 options
## ~~~~~~~~~~~
# call CO2 condensation ?
co2cond = .false.
# Set initial temperature profile to 1 K above CO2 condensation everywhere?
nearco2cond = .false.
</syntaxhighlight>

- [[The_gases.def_Input_file|''gases.def'']]: File containing the gas composition of the atmosphere you want to model, with their molar mixing ratios.
<syntaxhighlight lang="bash" line>
# gases
5
H2_
He_
CH4
C2H2
C2H6
0.863
0.134
0.0018
1.e-7
1.e-5
# First line is number of gases
# Followed by gas names (always 3 characters)
# and then molar mixing ratios.
# mixing ratio -1 means the gas is variable.
</syntaxhighlight>

- [[The jupiter_const.def Input File|''jupiter_const.def'']]: Files that gather all orbital and physical parameters of Jupiter.

- [[The_traceur.def_Input_File|''traceur.def'']]: At this time, only two tracers are used for modelling Jupiter atmosphere, so the ''traceur.def'' file is summed up as follow
<syntaxhighlight lang="bash" line>
2
h2o_vap
h2o_ice
</syntaxhighlight>

''' Two additional files are used to set the running parameter of the simulation itself:'''

- [[The run_icosa.def Input File | ''run_icosa.def'']]: file containing parameters for '''ICOSAGCM''' to execute the simulation, use to determine the [[Advanced Use of the GCM | horizontal and vertical resolutions]], the number of processors, the number of subdivisions, the duration of the simulation, etc.

- ''run.def'': file which brings together all the setting files and will be reading by the interface '''ICOSA_LMDZ''' to link each part of the model ('''ICOSAGCM''', '''LMDZ.GENERIC''') with its particular setting file(s) when the library '''XIOS''' does not take action (through the ''.xml'' files).
<syntaxhighlight lang="bash" line>
###########################################################################
### INCLUDE OTHER DEF FILES (physics, specific settings, etc...)
###########################################################################
INCLUDEDEF=run_icosa.def

INCLUDEDEF=jupiter_const.def

INCLUDEDEF=callphys.def

prt_level=0

## iphysiq must be same as itau_physics
iphysiq=40
</syntaxhighlight>

=== Hot Jupiter with DYNAMICO ===

Modelling the atmosphere of Hot Jupiter is challenging because of the extreme temperature conditions, and the fact that these planets are gas giants. Therefore, using a dynamical core such as Dynamico is strongly recommended. Here, we discuss how to perform a cloudless simulation of the Hot Jupiter WASP-43 b, using Dynamico.

'''1st step''': You need to go to the github mentionned previously for Dynamico: https://github.com/aymeric-spiga/dynamico-giant. ''Git clone'' this repo on your favorite cluster, and ''checkout'' to the "hot_jupiter" branch.

'''2nd step''': Now, run the install.sh script. This script will install '''all''' the required models ('''LMDZ.COMMON''', '''LMDZ.GENERIC''','''ICOSA_LMDZ''','''XIOS''','''FCM''','''ICOSAGCM'''). At this point, you only miss '''IOIPSL'''. To install it, go to
<syntaxhighlight lang="bash">
dynamico-giant/code/LMDZ.COMMON/ioipsl/
</syntaxhighlight>

There, you will find some examples of installations script. You need to create one that will work on your cluster, with your own arch files.
During the installation of '''IOIPSL''', you might be asked for a login/password. Contact TGCC computing center to get access.

'''3rd step''': Great, now we have all we need to get started. Navigate to the ''hot_jupiter'' folder. You will find a ''compile_mesopsl.sh'' and a ''compile_occigen.sh'' script. Use them as examples to create the compile script adapted to your own cluster, then run it.
While running, I suggest that you take a look at the ''log_compile'' file. The compilation can take a while (~ 10minutes, especially because of XIOS). On quick trick to make sure that everything went right is to check the number of ''Build command finished'' messages in ''log_compile''. If everything worked out, there should be 6 of them.

'''4th step''': Okay, the model compiled, good job ! Now we need to create the initial condition for our run. In the hot_jupiter1d folder, you already have a ''temp_profile.txt'' computed with the 1D version of the LMDZ.GENERIC (see rcm1d on this page). Thus, no need to recompute a 1D model but it will be needed if you want to model another Hot Jupiter.
Navigate to the 'makestart' folder, located at
<syntaxhighlight lang="bash">
dynamico-giant/hot_jupiter/makestart/
</syntaxhighlight>
To generate the initial conditions for the 3D run, we're gonna start the model using the temperature profile from the 1D run. to do that, you will find a "job_mpi" script. Open it, and adapt it to your cluster and launch the job. This job is using 20 procs, and it runs 5 days of simulations.
If everything goes well, you should see few netcdf files appear. The important ones are '''start_icosa0.nc''', '''startfi0.nc''' and '''Xhistins.nc'''.
If you see these files, you're all set to launch a real simulation !

'''5th step''': Go back to ''hot_jupiter'' folder. There are a bunch of script to launch your simulation. Take a look at the ''astro_fat_mpi'' script, and adapt it to your cluster. Then you can launch your simulation by doing
<syntaxhighlight lang="bash">
./run_astro_fat
</syntaxhighlight>
This will start the simulation, using 90 procs. In the same folder, check if the icosa_lmdz.out file is created. This is the logfile of the simulation, while it is running. You can check there that everything is going well.

'''Important side note''': When using the ''run_astro_fat'' script to run a simulation, it will run a chained simulation, restarting the simulation from the previous state after 100 days of simulations and generating ''Xhistins.nc'' files. This is your results file, where you will find all the variables that controls your atmosphere (temperature field, wind fields, etc..).

Good luck and enjoy the generic PCM Dynamico for Hot Jupiter !

'''2nd important side note''': These 5 steps are the basic needed steps to run a simulation. If you want to tune simulations to another planet, or change other stuff, you need to take a look at '''*.def''' and '''*.xml''' files. If you're lost in all of this, take a look at the different pages of this website and/or contact us !
Also, you might want to check the wiki on the [https://github.com/aymeric-spiga/dynamico-giant ''Github''], that explains a lot of settings for Dynamico

== 3D LES setup ==

=== Proxima b with LES ===

To model the subgrid atmospheric turbulence, the WRF dynamical core coupled with the LMD Generic physics package is used. The first studied conducted was to resolve the convective activity of the substellar point of Proxami-b (Lefevre et al 2021). The impact of the stellar insolation and rotation period were studied. The files for the reference case, with a stellar flux of 880 W/m2 and an 11 days rotation period, are presented

The input_* file are the used to initialize the temperature, pressure, winds and moisture of the domain.
input_souding : altitude (km), potential temperature, water vapour (kg/kg), u, v
input_therm : normalized gas constant, isobaric heat capacity, pressure, density, temperature
input_hr : SW heating, LW heating, Large-scale heating extracted from the GCM. Only the last one is used in this configuration.

The file namelist.input is used to set up the domain parameters (resolution, grid points, etc). The file levels specifies the eta-levels of the vertical domain.

Planet is used set up the atmospheric parameters, in order : gravity (m/s2), isobaric heat capacity (J/kg/K), molecular mass (g/mol), reference temperature (K), surface pressure (Pa), planet radius (m) and planet rotation rate (s-1).

The files *.def are the parameter for the physics. Compared to GCM runs, the convective adjustment in callphys.def is turned off

The file controle.txt, equivalent of the field controle in GCM start.nc, needed to initialize some physics constants.

TBC ML

== 1D setup ==

=== rcm1d test case ===

Our 1-D forward model

TBD by Gwenael ? (you can have a look at the Generic GCM User Manual for inspiration)

=== kcm1d test case ===

Our 1-D inverse model

TBD by Guillaume or Martin