Experimental constraints on the solidification of a nominally dry lunar magma ocean
The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralog...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Lin, Yanhao [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2017 |
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| Rechteinformationen: |
Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Earth & planetary science letters - Amsterdam [u.a.] : Elsevier, 1966, 471(2017), Seite 104-116 |
|---|---|
| Übergeordnetes Werk: |
volume:471 ; year:2017 ; pages:104-116 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.epsl.2017.04.045 |
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OLC1998990346 |
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| 520 | |a The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. | ||
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10.1016/j.epsl.2017.04.045 doi PQ20171228 (DE-627)OLC1998990346 (DE-599)GBVOLC1998990346 (PRQ)e1751-8cfda21e9113bdd9d394c4dcdb53c7f08eae65706a50a35666dfa105079db5550 (KEY)0055337920170000471000000104experimentalconstraintsonthesolidificationofanomin DE-627 ger DE-627 rakwb eng 550 DNB TE 1000 AVZ rvk TE AVZ rvk 38.35 bkl 39.29 bkl Lin, Yanhao verfasserin aut Experimental constraints on the solidification of a nominally dry lunar magma ocean 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess lunar magma ocean lunar petrology lunar crust experimental petrology Tronche, Elodie J oth Steenstra, Edgar S oth van Westrenen, Wim oth Enthalten in Earth & planetary science letters Amsterdam [u.a.] : Elsevier, 1966 471(2017), Seite 104-116 (DE-627)129882534 (DE-600)300203-2 (DE-576)015178501 0012-821X nnns volume:471 year:2017 pages:104-116 http://dx.doi.org/10.1016/j.epsl.2017.04.045 Volltext https://www.sciencedirect.com/science/article/pii/S0012821X1730239X http://www.narcis.nl/publication/RecordID/oai:research.vu.nl:publications%2F60a9eb64-32ec-48cb-9652-c9ad550ef177 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_21 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4323 TE 1000 TE 38.35 AVZ 39.29 AVZ AR 471 2017 104-116 |
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10.1016/j.epsl.2017.04.045 doi PQ20171228 (DE-627)OLC1998990346 (DE-599)GBVOLC1998990346 (PRQ)e1751-8cfda21e9113bdd9d394c4dcdb53c7f08eae65706a50a35666dfa105079db5550 (KEY)0055337920170000471000000104experimentalconstraintsonthesolidificationofanomin DE-627 ger DE-627 rakwb eng 550 DNB TE 1000 AVZ rvk TE AVZ rvk 38.35 bkl 39.29 bkl Lin, Yanhao verfasserin aut Experimental constraints on the solidification of a nominally dry lunar magma ocean 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess lunar magma ocean lunar petrology lunar crust experimental petrology Tronche, Elodie J oth Steenstra, Edgar S oth van Westrenen, Wim oth Enthalten in Earth & planetary science letters Amsterdam [u.a.] : Elsevier, 1966 471(2017), Seite 104-116 (DE-627)129882534 (DE-600)300203-2 (DE-576)015178501 0012-821X nnns volume:471 year:2017 pages:104-116 http://dx.doi.org/10.1016/j.epsl.2017.04.045 Volltext https://www.sciencedirect.com/science/article/pii/S0012821X1730239X http://www.narcis.nl/publication/RecordID/oai:research.vu.nl:publications%2F60a9eb64-32ec-48cb-9652-c9ad550ef177 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_21 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4323 TE 1000 TE 38.35 AVZ 39.29 AVZ AR 471 2017 104-116 |
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10.1016/j.epsl.2017.04.045 doi PQ20171228 (DE-627)OLC1998990346 (DE-599)GBVOLC1998990346 (PRQ)e1751-8cfda21e9113bdd9d394c4dcdb53c7f08eae65706a50a35666dfa105079db5550 (KEY)0055337920170000471000000104experimentalconstraintsonthesolidificationofanomin DE-627 ger DE-627 rakwb eng 550 DNB TE 1000 AVZ rvk TE AVZ rvk 38.35 bkl 39.29 bkl Lin, Yanhao verfasserin aut Experimental constraints on the solidification of a nominally dry lunar magma ocean 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess lunar magma ocean lunar petrology lunar crust experimental petrology Tronche, Elodie J oth Steenstra, Edgar S oth van Westrenen, Wim oth Enthalten in Earth & planetary science letters Amsterdam [u.a.] : Elsevier, 1966 471(2017), Seite 104-116 (DE-627)129882534 (DE-600)300203-2 (DE-576)015178501 0012-821X nnns volume:471 year:2017 pages:104-116 http://dx.doi.org/10.1016/j.epsl.2017.04.045 Volltext https://www.sciencedirect.com/science/article/pii/S0012821X1730239X http://www.narcis.nl/publication/RecordID/oai:research.vu.nl:publications%2F60a9eb64-32ec-48cb-9652-c9ad550ef177 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_21 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4323 TE 1000 TE 38.35 AVZ 39.29 AVZ AR 471 2017 104-116 |
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10.1016/j.epsl.2017.04.045 doi PQ20171228 (DE-627)OLC1998990346 (DE-599)GBVOLC1998990346 (PRQ)e1751-8cfda21e9113bdd9d394c4dcdb53c7f08eae65706a50a35666dfa105079db5550 (KEY)0055337920170000471000000104experimentalconstraintsonthesolidificationofanomin DE-627 ger DE-627 rakwb eng 550 DNB TE 1000 AVZ rvk TE AVZ rvk 38.35 bkl 39.29 bkl Lin, Yanhao verfasserin aut Experimental constraints on the solidification of a nominally dry lunar magma ocean 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess lunar magma ocean lunar petrology lunar crust experimental petrology Tronche, Elodie J oth Steenstra, Edgar S oth van Westrenen, Wim oth Enthalten in Earth & planetary science letters Amsterdam [u.a.] : Elsevier, 1966 471(2017), Seite 104-116 (DE-627)129882534 (DE-600)300203-2 (DE-576)015178501 0012-821X nnns volume:471 year:2017 pages:104-116 http://dx.doi.org/10.1016/j.epsl.2017.04.045 Volltext https://www.sciencedirect.com/science/article/pii/S0012821X1730239X http://www.narcis.nl/publication/RecordID/oai:research.vu.nl:publications%2F60a9eb64-32ec-48cb-9652-c9ad550ef177 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_21 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4323 TE 1000 TE 38.35 AVZ 39.29 AVZ AR 471 2017 104-116 |
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10.1016/j.epsl.2017.04.045 doi PQ20171228 (DE-627)OLC1998990346 (DE-599)GBVOLC1998990346 (PRQ)e1751-8cfda21e9113bdd9d394c4dcdb53c7f08eae65706a50a35666dfa105079db5550 (KEY)0055337920170000471000000104experimentalconstraintsonthesolidificationofanomin DE-627 ger DE-627 rakwb eng 550 DNB TE 1000 AVZ rvk TE AVZ rvk 38.35 bkl 39.29 bkl Lin, Yanhao verfasserin aut Experimental constraints on the solidification of a nominally dry lunar magma ocean 2017 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. Nutzungsrecht: © Elsevier B.V. © info:eu-repo/semantics/closedAccess lunar magma ocean lunar petrology lunar crust experimental petrology Tronche, Elodie J oth Steenstra, Edgar S oth van Westrenen, Wim oth Enthalten in Earth & planetary science letters Amsterdam [u.a.] : Elsevier, 1966 471(2017), Seite 104-116 (DE-627)129882534 (DE-600)300203-2 (DE-576)015178501 0012-821X nnns volume:471 year:2017 pages:104-116 http://dx.doi.org/10.1016/j.epsl.2017.04.045 Volltext https://www.sciencedirect.com/science/article/pii/S0012821X1730239X http://www.narcis.nl/publication/RecordID/oai:research.vu.nl:publications%2F60a9eb64-32ec-48cb-9652-c9ad550ef177 GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-GEO SSG-OLC-AST SSG-OPC-GGO SSG-OPC-GEO SSG-OPC-AST GBV_ILN_21 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4323 TE 1000 TE 38.35 AVZ 39.29 AVZ AR 471 2017 104-116 |
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experimental constraints on the solidification of a nominally dry lunar magma ocean |
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Experimental constraints on the solidification of a nominally dry lunar magma ocean |
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The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. |
| abstractGer |
The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. |
| abstract_unstemmed |
The lunar magma ocean (LMO) concept has been used extensively for lunar evolution models for decades, but to date the full cooling and crystallization path of the LMO has not been studied experimentally. Here we present results of a high-pressure, high-temperature experimental study of the mineralogical and geochemical evolution accompanying the full solidification of a nominally dry LMO. Experiments used a bulk composition based on geophysical data, and assumed an initial LMO depth of 700 km. The effect of pressure within a deep magma ocean on solidification at different levels in the ocean was explicitly taken into account, by performing experiments at multiple pressures and constant temperature during each solidification step. Results show formation of a deep harzburgite (olivine + low-Ca pyroxene) layer in the first ∼50% of equilibrium crystallization. The crystallising mineral assemblage does not change until plagioclase and clinopyroxene appear at 68 PCS (per cent solid by volume), while low-Ca pyroxene stops forming. Olivine disappears at 83 PCS, and ilmenite and β-quartz start crystallizing at 91 and 96 PCS, respectively. At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. As plagioclase crystallization can be suppressed by the presence of H2O, this implies that the lunar magma ocean was water-bearing. |
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Experimental constraints on the solidification of a nominally dry lunar magma ocean |
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At 99 PCS, we observe an extremely iron-rich (26.5 wt.% FeO) residual LMO liquid. Our results differ substantially from the oft-cited LMO solidification study of Snyder et al. (1992), which was based on a limited number of experiments at a single pressure. Differences include the mineralogy of the deepest sections of the solidified LMO (harzburgitic instead of dunitic), the formation of SiO2 in the lunar interior, and the development of extreme iron enrichment in the last remaining dregs of the LMO. Our findings shed new light on several aspects of lunar petrology, including the formation of felsic and iron-rich magmas in the Moon. Finally, based on our experiments the lunar crust, consisting of the light minerals plagioclase and quartz, would reach a thickness of ∼67.5 km. This is far greater than crustal thickness estimates from recent GRAIL mission gravitational data (34–43 km, Wieczorek et al., 2013). Although the initial depth of the LMO has an effect on the thickness of crust produced, this effect is not large enough to explain this discrepancy. Inefficient plagioclase segregation, trapping of magma in cumulate reservoirs, and Al sequestration in spinel cannot explain the discrepancy either. 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