Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite
Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-g...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Wark, D. A. [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
1979 |
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| Schlagwörter: |
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| Anmerkung: |
© D. Reidel Publishing Co 1979 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Kluwer Academic Publishers, 1968, 65(1979), 2 vom: Okt., Seite 275-295 |
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| Übergeordnetes Werk: |
volume:65 ; year:1979 ; number:2 ; month:10 ; pages:275-295 |
| Links: |
|---|
| DOI / URN: |
10.1007/BF00648496 |
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| Katalog-ID: |
OLC2066137006 |
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| 520 | |a Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. | ||
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10.1007/BF00648496 doi (DE-627)OLC2066137006 (DE-He213)BF00648496-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Wark, D. A. verfasserin aut Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite 1979 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Co 1979 Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. Olivine Supernova Remnant Carbonaceous Chondrite Refractory Element Chondrite Meteorite Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 65(1979), 2 vom: Okt., Seite 275-295 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:65 year:1979 number:2 month:10 pages:275-295 https://doi.org/10.1007/BF00648496 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 65 1979 2 10 275-295 |
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10.1007/BF00648496 doi (DE-627)OLC2066137006 (DE-He213)BF00648496-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Wark, D. A. verfasserin aut Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite 1979 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Co 1979 Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. Olivine Supernova Remnant Carbonaceous Chondrite Refractory Element Chondrite Meteorite Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 65(1979), 2 vom: Okt., Seite 275-295 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:65 year:1979 number:2 month:10 pages:275-295 https://doi.org/10.1007/BF00648496 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 65 1979 2 10 275-295 |
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10.1007/BF00648496 doi (DE-627)OLC2066137006 (DE-He213)BF00648496-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Wark, D. A. verfasserin aut Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite 1979 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Co 1979 Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. Olivine Supernova Remnant Carbonaceous Chondrite Refractory Element Chondrite Meteorite Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 65(1979), 2 vom: Okt., Seite 275-295 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:65 year:1979 number:2 month:10 pages:275-295 https://doi.org/10.1007/BF00648496 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 65 1979 2 10 275-295 |
| allfieldsGer |
10.1007/BF00648496 doi (DE-627)OLC2066137006 (DE-He213)BF00648496-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Wark, D. A. verfasserin aut Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite 1979 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Co 1979 Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. Olivine Supernova Remnant Carbonaceous Chondrite Refractory Element Chondrite Meteorite Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 65(1979), 2 vom: Okt., Seite 275-295 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:65 year:1979 number:2 month:10 pages:275-295 https://doi.org/10.1007/BF00648496 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 65 1979 2 10 275-295 |
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10.1007/BF00648496 doi (DE-627)OLC2066137006 (DE-He213)BF00648496-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Wark, D. A. verfasserin aut Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite 1979 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © D. Reidel Publishing Co 1979 Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. Olivine Supernova Remnant Carbonaceous Chondrite Refractory Element Chondrite Meteorite Enthalten in Astrophysics and space science Kluwer Academic Publishers, 1968 65(1979), 2 vom: Okt., Seite 275-295 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:65 year:1979 number:2 month:10 pages:275-295 https://doi.org/10.1007/BF00648496 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_21 GBV_ILN_22 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2002 GBV_ILN_2279 GBV_ILN_2286 GBV_ILN_4012 GBV_ILN_4035 GBV_ILN_4046 GBV_ILN_4082 GBV_ILN_4103 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4700 AR 65 1979 2 10 275-295 |
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Wark, D. A. |
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Wark, D. A. ddc 520 ssgn 16,12 misc Olivine misc Supernova Remnant misc Carbonaceous Chondrite misc Refractory Element misc Chondrite Meteorite Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite |
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birth of the presolar nebula: the sequence of condensation revealed in the allende meteorite |
| title_auth |
Birth of the presolar nebula: The sequence of condensation revealed in the Allende meteorite |
| abstract |
Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. © D. Reidel Publishing Co 1979 |
| abstractGer |
Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. © D. Reidel Publishing Co 1979 |
| abstract_unstemmed |
Abstract This work applies the well-known supernova-trigger hypothesis for solar system formation to explain in detail many properties of the Allende meteorite. The Allende carbonaceous chondrite meteorite is an assemblage of millimetre- to centimetre-sized Ca-Al-rich inclusions (CAI's), fine-grained alkali-rich spinel aggregates, amoeboid olivine aggregates, olivine chondrules and sulfide chondrules set in an extremely fine-grained black matrix. Detailed isotopic, chemical and textural properties show that these components formed in the above order as independent cosmic grains. Some CAI's containmicron-sized metal nuggets in which the normally incompatible refractory (Mo, Re, W) and platinum group (Pt, Os, Ir, Ru) metals are alloyed together in approximately ‘cosmic’ proportions, suggesting that these nuggets also condensed as cosmic grains. From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model. © D. Reidel Publishing Co 1979 |
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From the consistent pattern of enclosure of earlier components on the above list within later ones, it appears that in the environment where these materials formed, condensation moved inexorably in the direction of increasing olivine and decreasing refractory element $ and^{16} $O content (from ∼4% $ excess^{16} $O to ∼‘normal’ terrestrial oxygen isotopic composition). Condensation sequences are all short and incomplete, from which it is concluded that condensing materials were soon separated from the condensing environment and isolated until all were brought together in a final ‘snowstorm’ of fine-grained, olivine crystals constituting the meteorite matrix. These major properties can be accounted for in a model in which a supernova remnant (SNR) in the ‘snowplow’ phase, whose oxygen was initially $ pure^{16} $O, pushes into a dark interstellar cloud. In the model, condensation of CAI's begins in the SNR shell when it has been diluted with ∼2500 times its mass of matter from the cloud, which also in part explains the rarity of observed isotopic anomalies in CAI's. The retardation of the SNR by the cloud propels condensed grains ahead toward the cloud under their own momentum. Continuing dilution by the cloud and continuing removal of the most refractory elements in grains can explain the evolving patterns of fractionation and depletion of refractory elements, including REE's, in successive condensates. Features such as rims on CAI's and concentric zonation of fine-grained aggregates can also be satisfied in the model. A presolar origin and a short (∼ 10 000 years) formation time for inclusions in carbonaceous chondrites are major implications of the model.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Olivine</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Supernova Remnant</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Carbonaceous Chondrite</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Refractory Element</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Chondrite Meteorite</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Astrophysics and space science</subfield><subfield code="d">Kluwer Academic Publishers, 1968</subfield><subfield code="g">65(1979), 2 vom: Okt., Seite 275-295</subfield><subfield code="w">(DE-627)129062723</subfield><subfield code="w">(DE-600)629-4</subfield><subfield code="w">(DE-576)014393522</subfield><subfield code="x">0004-640X</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:65</subfield><subfield code="g">year:1979</subfield><subfield code="g">number:2</subfield><subfield code="g">month:10</subfield><subfield code="g">pages:275-295</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/BF00648496</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-TEC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_20</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_21</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_22</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_24</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_31</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_47</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2002</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2279</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2286</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4035</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4046</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4082</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4103</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4305</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4700</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">65</subfield><subfield code="j">1979</subfield><subfield code="e">2</subfield><subfield code="c">10</subfield><subfield code="h">275-295</subfield></datafield></record></collection>
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