Cenki 2022 uht granulitic terranes

src/pages/models/cenki-2022-uht-granulitic-terranes/assets/.gitkeep

@@ -0,0 +1 @@
+

src/pages/models/cenki-2022-uht-granulitic-terranes/graphics/.gitkeep

@@ -0,0 +1 @@
+

src/pages/models/cenki-2022-uht-granulitic-terranes/index.md

@@ -0,0 +1,182 @@
+---
+templateKey: model
+slug: cenki-2022-uht-granulitic-terranes
+title: 'Timing of partial melting and granulite formation during the genesis of high
+  to ultra‐high temperature terranes: Insight from numerical experiments'
+date: '2024-10-25T06:41:30.000Z'
+featuredpost:
+for_codes:
+  - 370401
+status:
+  - completed
+doi: https://doi.org/10.25914/aaen-nc33
+url: https://mate.science//models/cenki-2022-uht-granulitic-terranes
+creditText: 'Cenki-Tok or Cenki, B., Rey, Patrice F.., Arcay, D., & Giordani, J. (2024).
+  Timing of partial melting and granulite formation during the genesis of high to
+  ultra‐high temperature terranes: Insight from numerical experiments [Data set].
+  AuScope, National Computational Infrastructure. https://doi.org/aaen-nc33'
+software:
+  name: Underworld 2
+  doi: https://doi.org/10.5281/zenodo.3975252
+  url_source: ''
+licence:
+  licence_url: https://creativecommons.org/licenses/by/4.0/legalcode
+  licence_image: ../../../img/licence/by.png
+  description: Creative Commons Attribution 4.0 International
+  licence_file: license.txt
+submitter:
+  name: Bénédicte
+  family_name: Cenki-Tok or Cenki
+  ORCID: https://orcid.org/0000-0001-7649-4498
+creators:
+  - name: Bénédicte
+    family_name: Cenki-Tok or Cenki
+    ORCID: 0000-0001-7649-4498
+  - name: Patrice
+    family_name: Rey
+    ORCID: 0000-0002-1767-8593
+  - name: Diane
+    family_name: Arcay
+    ORCID: 0000-0001-6773-0807
+  - name: Julian
+    family_name: Giordani
+    ORCID: 0000-0003-4515-9296
+associated_publication:
+  title: 'Timing of partial melting and granulite formation during the genesis of
+    high to ultra‐high temperature terranes: Insight from numerical experiments'
+  url: http://dx.doi.org/10.1111/ter.12577
+  doi: 10.1111/ter.12577
+  publisher: Wiley
+  journal: Terra Nova
+  date: 2022-1-14
+  authors:
+    - name: Bénédicte
+      family_name: Cenki
+    - name: Patrice F.
+      family_name: Rey
+    - name: Diane
+      family_name: Arcay
+    - name: Julian
+      family_name: Giordani
+compute_info:
+  name: ''
+  organisation: ''
+  url: ''
+  doi: ''
+research_tags:
+  - HT‐UHT terranes
+  - Orogenic cycle
+compute_tags:
+  - Python
+  - Finite Element
+funder:
+  - name: ''
+    doi: ''
+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.
+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.
+images:
+  landing_image:
+    src: ./graphics/Figure2_v9.png
+    caption: ' 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).'
+  graphic_abstract:
+    src: ./graphics/Figure3_v6.png
+    caption: ' Figure 3. Depth – time profiles indicating the onset of partial melting
+      and granulite formation through the evolution of the models.'
+  model_setup:
+    src: ''
+    caption: ''
+animation:
+  src:
+  caption: ''
+model_setup_info:
+  url: ''
+  summary: "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: \r\n\r\ni) 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.\r\n\r\nThese 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."
+model_files:
+  url: ''
+  notes: ''
+  file_tree: ''
+  existing_identifier: https://github.com/underworld-community/cenki-et-al-UHT-granulitic-terranes
+  nci_file_path: 
+    https://thredds.nci.org.au/thredds/catalog/nm08/MATE/cenki-2022-uht-granulitic-terranes/catalog.html
+  include: true
+dataset:
+  url: ''
+  notes: ''
+  existing_identifier: ''
+  nci_file_path: 
+    https://thredds.nci.org.au/thredds/catalog/nm08/MATE/cenki-2022-uht-granulitic-terranes/catalog.html
+  include: true
+metadataFile: ro-crate-metadata.json
+---