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(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 +--- diff --git a/src/pages/models/cenki-2022-uht-granulitic-terranes/license.txt b/src/pages/models/cenki-2022-uht-granulitic-terranes/license.txt new file mode 100644 index 0000000..da6ab6c --- /dev/null +++ b/src/pages/models/cenki-2022-uht-granulitic-terranes/license.txt @@ -0,0 +1,396 @@ +Attribution 4.0 International + +======================================================================= + +Creative Commons Corporation ("Creative Commons") is not a law firm and +does not provide legal services or legal advice. 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For +the avoidance of doubt, this paragraph does not form part of the +public licenses. + +Creative Commons may be contacted at creativecommons.org. + diff --git a/src/pages/models/cenki-2022-uht-granulitic-terranes/ro-crate-metadata.json b/src/pages/models/cenki-2022-uht-granulitic-terranes/ro-crate-metadata.json new file mode 100644 index 0000000..11df4d7 --- /dev/null +++ b/src/pages/models/cenki-2022-uht-granulitic-terranes/ro-crate-metadata.json @@ -0,0 +1,403 @@ +{ + "@context": [ + "https://www.researchobject.org/ro-crate/1.1/context.jsonld", + "https://raw.githubusercontent.com/codemeta/codemeta/master/codemeta.jsonld" + ], + "@graph": [ + { + "@id": "#datasetCreation", + "@type": "CreateAction", + "agent": [ + { + "@id": "https://orcid.org/0000-0001-7649-4498" + }, + { + "@id": "https://orcid.org/0000-0002-1767-8593" + }, + { + "@id": "https://orcid.org/0000-0001-6773-0807" + }, + { + "@id": "https://orcid.org/0000-0003-4515-9296" + } + ], + "description": "Running the computational model", + "endTime": "", + "instrument": { + "@id": "https://doi.org/10.5281/zenodo.3975252" + }, + "object": { + "@id": "model_code_inputs" + }, + "result": { + "@id": "model_output_data" + }, + "startTime": "" + }, + { + "@id": "./", + "@type": "Dataset", + "about": { + "@id": "https://linked.data.gov.au/def/anzsrc-for/2020/370401" + }, + "abstract": "Long\u2010lived high to ultra\u2010high temperature (HT\u2010UHT) 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\u2010state heat equation allows underlining the interdependency of the parameters controlling the crustal geotherm at thermal equilibrium. Second, performing two\u2010dimensional thermo\u2010mechanical experiments of an orogenic cycle, from shortening to gravitational collapse, allows to consider non\u2010steady\u2010state 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\u2010UHT terranes. Finally, the interplay between these parameters can explain the difference in predicted pressure\u2010temperature\u2010time paths that can be compared with the natural rock archive.", + "alternateName": "cenki-2022-uht-granulitic-terranes", + "citation": { + "@id": "http://dx.doi.org/10.1111/ter.12577" + }, + "contributor": "", + "creativeWorkStatus": "completed", + "creator": [ + { + "@id": "https://orcid.org/0000-0001-7649-4498" + }, + { + "@id": "https://orcid.org/0000-0002-1767-8593" + }, + { + "@id": "https://orcid.org/0000-0001-6773-0807" + }, + { + "@id": "https://orcid.org/0000-0003-4515-9296" + } + ], + "datePublished": "2024-10-25T06:41:30.000Z", + "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. 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