Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites
Abstract We studied 149 pyroxenes from 69 pyroxene‐bearing micrometeorites collected from deep‐sea sediments of the Indian Ocean and South Pole Water Well at Antarctica, Amundsen‐Scott South Pole station. The minor elements in pyroxenes from micrometeorites are present in the ranges as follows: MnO...
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crwiley:10.1111/maps.13105 2023-12-03T10:09:27+01:00 Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites Rudraswami, N. G. Fernandes, D. De Araujo, Agnelo Shyam Prasad, M. Taylor, S. Ministry of Earth Sciences 2018 http://dx.doi.org/10.1111/maps.13105 https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fmaps.13105 https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.13105 en eng Wiley http://onlinelibrary.wiley.com/termsAndConditions#vor Meteoritics & Planetary Science volume 53, issue 10, page 2035-2050 ISSN 1086-9379 1945-5100 Space and Planetary Science Geophysics journal-article 2018 crwiley https://doi.org/10.1111/maps.13105 2023-11-09T13:59:28Z Abstract We studied 149 pyroxenes from 69 pyroxene‐bearing micrometeorites collected from deep‐sea sediments of the Indian Ocean and South Pole Water Well at Antarctica, Amundsen‐Scott South Pole station. The minor elements in pyroxenes from micrometeorites are present in the ranges as follows: MnO ~0.0–0.4 wt%, Al 2 O 3 ~0.0–1.5 wt%, CaO ~0.0–1.0 wt%, Cr 2 O 3 ~0.3–0.9 wt%, and FeO ~0.5–4 wt%. Their chemical compositions suggest that pyroxene‐bearing micrometeorites are mostly related to precursors from carbonaceous chondrites rather than ordinary chondrites. The Fe/(Fe+Mg) ratio of the pyroxenes and olivines in micrometeorites shows similarities to carbonaceous chondrites with values lying between 0 and 0.2, and those with values beyond this range are dominated by ordinary chondrites. Atmospheric entry of the pyroxene‐bearing micrometeorites is expected to have a relatively low entry velocity of <16 km s −1 and high zenith angle (70–90°) to preserve their chemical compositions. In addition, similarities in the pyroxene and olivine mineralogical compositions between carbonaceous chondrites and cometary particles suggest that dust in the solar system is populated by materials from different sources that are chemically similar to each other. Our results on pyroxene chemical compositions reveal significant differences with those from ordinary chondrites. The narrow range in olivine and pyroxene chemical compositions are similar to those from carbonaceous chondrites, and a small proportion to ordinary chondrites indicates that dust is largely sourced from carbonaceous chondrite‐type bodies. Article in Journal/Newspaper Amundsen-Scott Antarc* Antarctica South pole South pole Wiley Online Library (via Crossref) Indian South Pole Amundsen-Scott ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen Scott South Pole Station ENVELOPE(0.000,0.000,-90.000,-90.000) Amundsen-Scott South Pole Station ENVELOPE(139.273,139.273,-89.998,-89.998) Meteoritics & Planetary Science 53 10 2035 2050 |
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Open Polar |
collection |
Wiley Online Library (via Crossref) |
op_collection_id |
crwiley |
language |
English |
topic |
Space and Planetary Science Geophysics |
spellingShingle |
Space and Planetary Science Geophysics Rudraswami, N. G. Fernandes, D. De Araujo, Agnelo Shyam Prasad, M. Taylor, S. Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
topic_facet |
Space and Planetary Science Geophysics |
description |
Abstract We studied 149 pyroxenes from 69 pyroxene‐bearing micrometeorites collected from deep‐sea sediments of the Indian Ocean and South Pole Water Well at Antarctica, Amundsen‐Scott South Pole station. The minor elements in pyroxenes from micrometeorites are present in the ranges as follows: MnO ~0.0–0.4 wt%, Al 2 O 3 ~0.0–1.5 wt%, CaO ~0.0–1.0 wt%, Cr 2 O 3 ~0.3–0.9 wt%, and FeO ~0.5–4 wt%. Their chemical compositions suggest that pyroxene‐bearing micrometeorites are mostly related to precursors from carbonaceous chondrites rather than ordinary chondrites. The Fe/(Fe+Mg) ratio of the pyroxenes and olivines in micrometeorites shows similarities to carbonaceous chondrites with values lying between 0 and 0.2, and those with values beyond this range are dominated by ordinary chondrites. Atmospheric entry of the pyroxene‐bearing micrometeorites is expected to have a relatively low entry velocity of <16 km s −1 and high zenith angle (70–90°) to preserve their chemical compositions. In addition, similarities in the pyroxene and olivine mineralogical compositions between carbonaceous chondrites and cometary particles suggest that dust in the solar system is populated by materials from different sources that are chemically similar to each other. Our results on pyroxene chemical compositions reveal significant differences with those from ordinary chondrites. The narrow range in olivine and pyroxene chemical compositions are similar to those from carbonaceous chondrites, and a small proportion to ordinary chondrites indicates that dust is largely sourced from carbonaceous chondrite‐type bodies. |
author2 |
Ministry of Earth Sciences |
format |
Article in Journal/Newspaper |
author |
Rudraswami, N. G. Fernandes, D. De Araujo, Agnelo Shyam Prasad, M. Taylor, S. |
author_facet |
Rudraswami, N. G. Fernandes, D. De Araujo, Agnelo Shyam Prasad, M. Taylor, S. |
author_sort |
Rudraswami, N. G. |
title |
Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
title_short |
Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
title_full |
Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
title_fullStr |
Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
title_full_unstemmed |
Perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
title_sort |
perceptive of the pyroxene‐bearing micrometeorites and their relation to chondrites |
publisher |
Wiley |
publishDate |
2018 |
url |
http://dx.doi.org/10.1111/maps.13105 https://api.wiley.com/onlinelibrary/tdm/v1/articles/10.1111%2Fmaps.13105 https://onlinelibrary.wiley.com/doi/pdf/10.1111/maps.13105 |
long_lat |
ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(0.000,0.000,-90.000,-90.000) ENVELOPE(139.273,139.273,-89.998,-89.998) |
geographic |
Indian South Pole Amundsen-Scott Amundsen Scott South Pole Station Amundsen-Scott South Pole Station |
geographic_facet |
Indian South Pole Amundsen-Scott Amundsen Scott South Pole Station Amundsen-Scott South Pole Station |
genre |
Amundsen-Scott Antarc* Antarctica South pole South pole |
genre_facet |
Amundsen-Scott Antarc* Antarctica South pole South pole |
op_source |
Meteoritics & Planetary Science volume 53, issue 10, page 2035-2050 ISSN 1086-9379 1945-5100 |
op_rights |
http://onlinelibrary.wiley.com/termsAndConditions#vor |
op_doi |
https://doi.org/10.1111/maps.13105 |
container_title |
Meteoritics & Planetary Science |
container_volume |
53 |
container_issue |
10 |
container_start_page |
2035 |
op_container_end_page |
2050 |
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1784263715220094976 |