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Section 1: Summary of your model
Model Submitter:
Bénédicte Cenki-Tok or Cenki (0000-0001-7649-4498)
Model Creator(s):
- Bénédicte Cenki-Tok or Cenki (0000-0001-7649-4498)
- Patrice Rey (0000-0002-1767-8593)
- Diane Arcay (0000-0001-6773-0807)
- Julian Giordani (0000-0003-4515-9296)
Model slug:
cenki-2022-uht-granulitic-terranes-1
(this will be the name of the model repository when created)
Model name:
Timing of partial melting and granulite formation during the genesis of high to ultra‐high temperature terranes: Insight from numerical experiments
License:
Creative Commons Attribution 4.0 International
Model Category:
- model published in study
Model Status:
- completed
Associated Publication title:
Short description:
Long-lived high to ultra-high temperature (HT-UHT) granulitic terranes formed throughout Earth's history. Yet, the detailed processes involved in their formation remain unresolved and notably the sequence of appearance and duration of migmatisation and granulites conditions in the orogenic cycle. These processes can be evaluated by analytical and numerical models. First, solving the steady-state heat equation allows underlining the interdependency of the parameters controlling the crustal geotherm at thermal equilibrium. Second, performing two-dimensional thermo-mechanical experiments of an orogenic cycle, from shortening to gravitational collapse, allows to consider non-steady-state geotherms and understand how deformation velocity may affect the relative timing of migmatite and granulite formation. These numerical experiments with elevated radiogenic heat production and slow shortening rates allow the formation of large volumes of prograde migmatites and granulites going through the sillimanite field as observed in many HT-UHT terranes. Finally, the interplay between these parameters can explain the difference in predicted pressure-temperature-time paths that can be compared with the natural rock archive.
Abstract:
Long‐lived high to ultra‐high temperature (HT‐UHT) granulitic terranes formed throughout Earth's history. Yet, the detailed processes involved in their formation remain unresolved and notably the sequence of appearance and duration of migmatisation and granulites conditions in the orogenic cycle. These processes can be evaluated by analytical and numerical models. First, solving the steady‐state heat equation allows underlining the interdependency of the parameters controlling the crustal geotherm at thermal equilibrium. Second, performing two‐dimensional thermo‐mechanical experiments of an orogenic cycle, from shortening to gravitational collapse, allows to consider non‐steady‐state geotherms and understand how deformation velocity may affect the relative timing of migmatite and granulite formation. These numerical experiments with elevated radiogenic heat production and slow shortening rates allow the formation of large volumes of prograde migmatites and granulites going through the sillimanite field as observed in many HT‐UHT terranes. Finally, the interplay between these parameters can explain the difference in predicted pressure‐temperature‐time paths that can be compared with the natural rock archive.
Funder(s):
- European Union's Horizon 2020 research and innovation program under grant agreement no 793978
Section 2: your model code, output data
No embargo on model contents requested
Include model code:
True
Model code existing URL/DOI:
https://github.com/underworld-community/cenki-et-al-UHT-granulitic-terranes
Include model output data:
True
Section 3: software framework and compute details
Software Framework DOI/URL:
Found software: Underworld 2
Name of primary software framework:
Underworld 2
Software & algorithm keywords:
- Python
- Finite Element
Section 4: web material (for mate.science)
Landing page image:
Caption: Figure2_v9.pdf
Figure 2. A-B. Model geometry, initial conditions as well as geotherm, viscosity and density profiles. The circles pattern superimposed on the continental crust represents the finite strain ellipses. White squares represent the Lagrangian particles recording the PTt paths presented in Fig. 4. A. Initial conditions for models RHP2_diff, mimicking a Proterozoic highly differentiated and highly radiogenic crust. B. Initial conditions for model RHP1_unif, simulating a Phanerozoic uniform and less radiogenic crust. C-J. Orogenic modeling results showing two snapshots for each model: i) shortening-delamination and ii) collapse. Shortening velocity is either slow (0.24 cm.y-1, C-F) or fast (2.4 cm.y-1, G-J).
Animation:
Filename: []()
Graphic abstract:
Caption: Figure3_v6.pdf
Figure 3. Depth – time profiles indicating the onset of partial melting and granulite formation through the evolution of the models.
Model setup figure:
Filename: []()
Description: The numerical models are performed with Underworld, a well-tested open-source finite element code, to solve the equations of conservation of momentum, mass, and energy for an incompressible fluid on a Cartesian Eulerian mesh (Moresi et al., 2007; Beucher et al., 2019). The 2D thermo-mechanical experiments involve a geological model of dimensions 480 km x 160 km discretized over a computational grid made of 240 x 80 elements. The initial setup consists of a 35 km or 40 km thick crust with 20 km of air-like material above, and mantle below (Fig. 2A-B). Each model runs through three stages:
i) a shortening phase during which the crust thickens to ~ 60 km with either a slow total velocity of 0.24 cm/yr during 70 My or a fast total velocity of 2.4 cm/yr during ~ 7 My (delivering a strain rate averaged over the length of the model of $1.6 \times 10^{-16} s^{-1}$ and $1.6 \times 10^{-15} s^{-1}$ respectively); ii) a rapid increase in BHF (from $0.020 W/m^2$ to $0.030 W/m^2$) over 2.5 My while the velocities imposed on the vertical boundaries are set to zero (vx = vy = 0 cm/yr) mimicking the thermal impact of a mantle delamination phase; iii) a relaxation phase in which the crust returns to normal thickness under slow extensional boundary conditions (total velocity of 0.10 cm/yr) associated with a decrease in BHF from $0.030 W/m^2$ to $0.020 W/m^2$ in ~ 70 My. Details of modeling procedures, rheological and thermal parameters, as well as the input Python script, are available as supplementary data.
These experiments focus on two end-member crustal structures with average values of total RHP at ~ $1 \mu W/m^3$ and ~ $2 \mu W/m^3$ (Fig. 2). A value of ~ $1 \mu W/m^3$ is in line with RHP calculations predicted from the present-day composition of the bulk continental crust determined by Taylor and McLennan (1995). Models RHP1_unif mimic a Phanerozoic orogenic cycle involving a continental crust with a uniform RHP ($1.0483 \mu W/m^3$) yielding an initial Moho temperature of 650°C at 40 km depth (Fig. 1A). However, Mareschal and Jaupart (2013), Artemieva et al. (2017), and Gard et al. (2019) showed that the crustal RHP may have been higher than ~ $1 \mu W/m^3$ during the Proterozoic, having varied between ~ $0.8 \mu W/m^3$ and ~ $4 \mu W/m^3$ between 0.5 Ga and 2.5 Ga with an average RHP close to ~ $2 \mu W/m^3$. In addition, recent studies reveal that, in tectonically stable regions, the upper crust’s RHP may be higher than in the lower crust (Goes et al., 2020; Alessio et al., 2020). The conditions for model RHP2_diff include a total average RHP of ~ $2.0922 \mu W/m^3$ with high RHP in the upper crust (~ $5 \mu W/m^3$) that decreases exponentially with a length scale factor $h_c$ of 20 km yielding an initial Moho temperature at 35 km depth of 650°C (Fig. 1D). Models RHP2_diff aim at approaching thermal conditions of a differentiated crust prevailing during the Proterozoic.
Errors and Warnings
Associated Publication Error fetching metadata with application/ld+json from https://api.crossref.org/works/https://doi.org/10.1111/ter.12577: 406 Client Error: Not Acceptable for url: https://api.crossref.org/works/https://doi.org/10.1111/ter.12577 Software Framework DOI/URI doi.org metadata record succesfully extracted in json-ld format Software Repository Warning: no repository URL provided. Submitter ORCID metadata record succesfully extracted in json-ld format
Model creators
ORCID metadata record succesfully extracted in json-ld format
ORCID metadata record succesfully extracted in json-ld format
ORCID metadata record succesfully extracted in json-ld format
ORCID metadata record succesfully extracted in json-ld format
Model Repository Slug
Warning: slug should be in the format familyname-year-keyword
Warning: Model repo cannot be created with proposed slug cenki-2022-uht-granulitic-terranes.
Either propose a new slug or repo will be created with name cenki-2022-uht-granulitic-terranes-1.
Scientific keywords
Warning: No keywords given
Could not parse Embargo date. Check format is
Model code/inputs notes
Warning: No notes provided.
Model creators
Error: no data creators found
Model output DOI
Warning: No DOI/URI provided.
Model data notes
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Model data size
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Invalid size stringComputer URI/DOI
Warning: No URI/DOI provided.
Animation
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Model setup figure Warning: No image uploaded.
Next steps
- once the
model_reviewersteam has approved the model, we will create a repository for your model
-> submitter ORCID (or name)
https://orcid.org/0000-0001-7649-4498
-> slug
cenki-2022-uht-granulitic-terranes
-> license
CC-BY-4.0
-> alternative license URL
No response
-> model category
model published in study
-> model status
completed
-> associated publication DOI
https://doi.org/10.1111/ter.12577
-> model creators
0000-0001-7649-4498 0000-0002-1767-8593 0000-0001-6773-0807 0000-0003-4515-9296
-> title
No response
-> description
Long-lived high to ultra-high temperature (HT-UHT) granulitic terranes formed throughout Earth's history. Yet, the detailed processes involved in their formation remain unresolved and notably the sequence of appearance and duration of migmatisation and granulites conditions in the orogenic cycle. These processes can be evaluated by analytical and numerical models. First, solving the steady-state heat equation allows underlining the interdependency of the parameters controlling the crustal geotherm at thermal equilibrium. Second, performing two-dimensional thermo-mechanical experiments of an orogenic cycle, from shortening to gravitational collapse, allows to consider non-steady-state geotherms and understand how deformation velocity may affect the relative timing of migmatite and granulite formation. These numerical experiments with elevated radiogenic heat production and slow shortening rates allow the formation of large volumes of prograde migmatites and granulites going through the sillimanite field as observed in many HT-UHT terranes. Finally, the interplay between these parameters can explain the difference in predicted pressure-temperature-time paths that can be compared with the natural rock archive.
-> abstract
No response
-> scientific keywords
No response
-> funder
European Union's Horizon 2020 research and innovation program under grant agreement no 793978
-> model embargo?
No response
-> include model code ?
-> model code/inputs DOI
https://github.com/underworld-community/cenki-et-al-UHT-granulitic-terranes
-> model code/inputs notes
No response
-> include model output data?
-> data creators
No response
-> model output data DOI
No response
-> model output data notes
No response
-> model output data size
No response
-> software framework DOI/URI
https://doi.org/10.5281/zenodo.3975252
-> software framework source repository
No response
-> name of primary software framework (e.g. Underworld, ASPECT, Badlands, OpenFOAM)
Underworld 2
-> software framework authors
No response
-> software & algorithm keywords
Python, Finite Element
-> computer URI/DOI
No response
-> add landing page image and caption
Figure2_v9.pdf
Figure 2. A-B. Model geometry, initial conditions as well as geotherm, viscosity and density profiles. The circles pattern superimposed on the continental crust represents the finite strain ellipses. White squares represent the Lagrangian particles recording the PTt paths presented in Fig. 4. A. Initial conditions for models RHP2_diff, mimicking a Proterozoic highly differentiated and highly radiogenic crust. B. Initial conditions for model RHP1_unif, simulating a Phanerozoic uniform and less radiogenic crust. C-J. Orogenic modeling results showing two snapshots for each model: i) shortening-delamination and ii) collapse. Shortening velocity is either slow (0.24 cm.y-1, C-F) or fast (2.4 cm.y-1, G-J).
-> add an animation (if relevant)
No response
-> add a graphic abstract figure (if relevant)
Figure3_v6.pdf
Figure 3. Depth – time profiles indicating the onset of partial melting and granulite formation through the evolution of the models.
-> add a model setup figure (if relevant)
No response
-> add a description of your model setup
The numerical models are performed with Underworld, a well-tested open-source finite element code, to solve the equations of conservation of momentum, mass, and energy for an incompressible fluid on a Cartesian Eulerian mesh (Moresi et al., 2007; Beucher et al., 2019). The 2D thermo-mechanical experiments involve a geological model of dimensions 480 km x 160 km discretized over a computational grid made of 240 x 80 elements. The initial setup consists of a 35 km or 40 km thick crust with 20 km of air-like material above, and mantle below (Fig. 2A-B). Each model runs through three stages:
i) a shortening phase during which the crust thickens to ~ 60 km with either a slow total velocity of 0.24 cm/yr during 70 My or a fast total velocity of 2.4 cm/yr during ~ 7 My (delivering a strain rate averaged over the length of the model of $1.6 \times 10^{-16} s^{-1}$ and $1.6 \times 10^{-15} s^{-1}$ respectively); ii) a rapid increase in BHF (from $0.020 W/m^2$ to $0.030 W/m^2$) over 2.5 My while the velocities imposed on the vertical boundaries are set to zero (vx = vy = 0 cm/yr) mimicking the thermal impact of a mantle delamination phase; iii) a relaxation phase in which the crust returns to normal thickness under slow extensional boundary conditions (total velocity of 0.10 cm/yr) associated with a decrease in BHF from $0.030 W/m^2$ to $0.020 W/m^2$ in ~ 70 My. Details of modeling procedures, rheological and thermal parameters, as well as the input Python script, are available as supplementary data.
These experiments focus on two end-member crustal structures with average values of total RHP at ~ $1 \mu W/m^3$ and ~ $2 \mu W/m^3$ (Fig. 2). A value of ~ $1 \mu W/m^3$ is in line with RHP calculations predicted from the present-day composition of the bulk continental crust determined by Taylor and McLennan (1995). Models RHP1_unif mimic a Phanerozoic orogenic cycle involving a continental crust with a uniform RHP ($1.0483 \mu W/m^3$) yielding an initial Moho temperature of 650°C at 40 km depth (Fig. 1A). However, Mareschal and Jaupart (2013), Artemieva et al. (2017), and Gard et al. (2019) showed that the crustal RHP may have been higher than ~ $1 \mu W/m^3$ during the Proterozoic, having varied between ~ $0.8 \mu W/m^3$ and ~ $4 \mu W/m^3$ between 0.5 Ga and 2.5 Ga with an average RHP close to ~ $2 \mu W/m^3$. In addition, recent studies reveal that, in tectonically stable regions, the upper crust’s RHP may be higher than in the lower crust (Goes et al., 2020; Alessio et al., 2020). The conditions for model RHP2_diff include a total average RHP of ~ $2.0922 \mu W/m^3$ with high RHP in the upper crust (~ $5 \mu W/m^3$) that decreases exponentially with a length scale factor $h_c$ of 20 km yielding an initial Moho temperature at 35 km depth of 650°C (Fig. 1D). Models RHP2_diff aim at approaching thermal conditions of a differentiated crust prevailing during the Proterozoic.
Please provide any feedback on the model submission process?
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