NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite

We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Liu, Nan [verfasserIn] Ogliore, Ryan C. [verfasserIn] Vacher, Lionel G. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2020

Schlagwörter:	Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter

Übergeordnetes Werk:	Enthalten in: Geochimica et cosmochimica acta - New York, NY [u.a.] : Elsevier, 1950, 283, Seite 243-264
Übergeordnetes Werk:	volume:283 ; pages:243-264

DOI / URN:	10.1016/j.gca.2020.05.026

Katalog-ID:	ELV004355458

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024	7		\|a 10.1016/j.gca.2020.05.026 \|2 doi
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100	1		\|a Liu, Nan \|e verfasserin \|0 (orcid)0000-0002-4456-4065 \|4 aut
245	1	0	\|a NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
264		1	\|c 2020
336			\|a nicht spezifiziert \|b zzz \|2 rdacontent
337			\|a Computermedien \|b c \|2 rdamedia
338			\|a Online-Ressource \|b cr \|2 rdacarrier
520			\|a We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago.
650		4	\|a Carbonaceous chondrite
650		4	\|a Vesta
650		4	\|a Howardite Kapoeta
650		4	\|a NanoSIMS
650		4	\|a Isotopic anomalies
650		4	\|a Presolar grains
650		4	\|a Organic matter
700	1		\|a Ogliore, Ryan C. \|e verfasserin \|0 (orcid)0000-0001-8165-6252 \|4 aut
700	1		\|a Vacher, Lionel G. \|e verfasserin \|0 (orcid)0000-0003-4230-6748 \|4 aut
773	0	8	\|i Enthalten in \|t Geochimica et cosmochimica acta \|d New York, NY [u.a.] : Elsevier, 1950 \|g 283, Seite 243-264 \|h Online-Ressource \|w (DE-627)300898797 \|w (DE-600)1483679-8 \|w (DE-576)120883465 \|x 0016-7037 \|7 nnns
773	1	8	\|g volume:283 \|g pages:243-264
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912			\|a GBV_ILN_2021
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912			\|a GBV_ILN_4112
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912			\|a GBV_ILN_4126
912			\|a GBV_ILN_4242
912			\|a GBV_ILN_4251
912			\|a GBV_ILN_4305
912			\|a GBV_ILN_4313
912			\|a GBV_ILN_4323
912			\|a GBV_ILN_4324
912			\|a GBV_ILN_4326
912			\|a GBV_ILN_4333
912			\|a GBV_ILN_4334
912			\|a GBV_ILN_4335
912			\|a GBV_ILN_4338
912			\|a GBV_ILN_4393
936	b	k	\|a 38.32 \|j Geochemie
936	b	k	\|a 39.29 \|j Theoretische Astronomie: Sonstiges
951			\|a AR
952			\|d 283 \|h 243-264

Indexfelder

author_variant	n l nl r c o rc rco l g v lg lgv
matchkey_str	article:00167037:2020----::aoisstpcnetgtooxnlticroaeucatf
hierarchy_sort_str	2020
bklnumber	38.32 39.29
publishDate	2020
allfields	10.1016/j.gca.2020.05.026 doi (DE-627)ELV004355458 (ELSEVIER)S0016-7037(20)30345-8 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Liu, Nan verfasserin (orcid)0000-0002-4456-4065 aut NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter Ogliore, Ryan C. verfasserin (orcid)0000-0001-8165-6252 aut Vacher, Lionel G. verfasserin (orcid)0000-0003-4230-6748 aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 283, Seite 243-264 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:283 pages:243-264 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 283 243-264
spelling	10.1016/j.gca.2020.05.026 doi (DE-627)ELV004355458 (ELSEVIER)S0016-7037(20)30345-8 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Liu, Nan verfasserin (orcid)0000-0002-4456-4065 aut NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter Ogliore, Ryan C. verfasserin (orcid)0000-0001-8165-6252 aut Vacher, Lionel G. verfasserin (orcid)0000-0003-4230-6748 aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 283, Seite 243-264 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:283 pages:243-264 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 283 243-264
allfields_unstemmed	10.1016/j.gca.2020.05.026 doi (DE-627)ELV004355458 (ELSEVIER)S0016-7037(20)30345-8 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Liu, Nan verfasserin (orcid)0000-0002-4456-4065 aut NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter Ogliore, Ryan C. verfasserin (orcid)0000-0001-8165-6252 aut Vacher, Lionel G. verfasserin (orcid)0000-0003-4230-6748 aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 283, Seite 243-264 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:283 pages:243-264 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 283 243-264
allfieldsGer	10.1016/j.gca.2020.05.026 doi (DE-627)ELV004355458 (ELSEVIER)S0016-7037(20)30345-8 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Liu, Nan verfasserin (orcid)0000-0002-4456-4065 aut NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter Ogliore, Ryan C. verfasserin (orcid)0000-0001-8165-6252 aut Vacher, Lionel G. verfasserin (orcid)0000-0003-4230-6748 aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 283, Seite 243-264 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:283 pages:243-264 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 283 243-264
allfieldsSound	10.1016/j.gca.2020.05.026 doi (DE-627)ELV004355458 (ELSEVIER)S0016-7037(20)30345-8 DE-627 ger DE-627 rda eng 550 DE-600 38.32 bkl 39.29 bkl Liu, Nan verfasserin (orcid)0000-0002-4456-4065 aut NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite 2020 nicht spezifiziert zzz rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago. Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter Ogliore, Ryan C. verfasserin (orcid)0000-0001-8165-6252 aut Vacher, Lionel G. verfasserin (orcid)0000-0003-4230-6748 aut Enthalten in Geochimica et cosmochimica acta New York, NY [u.a.] : Elsevier, 1950 283, Seite 243-264 Online-Ressource (DE-627)300898797 (DE-600)1483679-8 (DE-576)120883465 0016-7037 nnns volume:283 pages:243-264 GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393 38.32 Geochemie 39.29 Theoretische Astronomie: Sonstiges AR 283 243-264
language	English
source	Enthalten in Geochimica et cosmochimica acta 283, Seite 243-264 volume:283 pages:243-264
sourceStr	Enthalten in Geochimica et cosmochimica acta 283, Seite 243-264 volume:283 pages:243-264
format_phy_str_mv	Article
bklname	Geochemie Theoretische Astronomie: Sonstiges
institution	findex.gbv.de
topic_facet	Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter
dewey-raw	550
isfreeaccess_bool	false
container_title	Geochimica et cosmochimica acta
authorswithroles_txt_mv	Liu, Nan @@aut@@ Ogliore, Ryan C. @@aut@@ Vacher, Lionel G. @@aut@@
publishDateDaySort_date	2020-01-01T00:00:00Z
hierarchy_top_id	300898797
dewey-sort	3550
id	ELV004355458
language_de	englisch
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The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. 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author	Liu, Nan
spellingShingle	Liu, Nan ddc 550 bkl 38.32 bkl 39.29 misc Carbonaceous chondrite misc Vesta misc Howardite Kapoeta misc NanoSIMS misc Isotopic anomalies misc Presolar grains misc Organic matter NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
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topic_title	550 DE-600 38.32 bkl 39.29 bkl NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite Carbonaceous chondrite Vesta Howardite Kapoeta NanoSIMS Isotopic anomalies Presolar grains Organic matter
topic	ddc 550 bkl 38.32 bkl 39.29 misc Carbonaceous chondrite misc Vesta misc Howardite Kapoeta misc NanoSIMS misc Isotopic anomalies misc Presolar grains misc Organic matter
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title	NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
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title_full	NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
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author_browse	Liu, Nan Ogliore, Ryan C. Vacher, Lionel G.
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title_sort	nanosims isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
title_auth	NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
abstract	We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago.
abstractGer	We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago.
abstract_unstemmed	We report on the investigation of presolar grains and organic matter (OM) in 14 xenolithic carbonaceous clasts (C-clasts) identified in the Kapoeta howardite based on high-resolution NanoSIMS hydrogen, carbon, nitrogen, and oxygen isotopic imaging data. The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago.
collection_details	GBV_USEFLAG_U SYSFLAG_U GBV_ELV SSG-OPC-GGO SSG-OPC-AST GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_150 GBV_ILN_151 GBV_ILN_224 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2027 GBV_ILN_2034 GBV_ILN_2038 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2056 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2190 GBV_ILN_2336 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4313 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4393
title_short	NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite
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author2	Ogliore, Ryan C. Vacher, Lionel G.
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up_date	2024-07-06T22:42:44.482Z
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The 14 C-clasts are ∼50–200 μm in size and consist of one CM-like and 13 CI-like clasts, which are classified based on their mineralogies. The clasts from this study are likely sourced from an ice-bearing parent body, either an icy asteroid or a comet, originating from the outer solar system according to the following mineralogical observations: (1) in two CI-like clasts, embayments of magnetite grains between the C-clast and the host howardite point to aqueous alteration occurring on Vesta as a result of melting the ice embedded in the C-clasts; (2) all of the C-clasts, especially the 13 CI-like clasts, likely originated from the same parent body, because (i) the 14 C-clasts are clustered in the thin section, and (ii) the clasts show a much higher ratio of CI-like to CM-like clasts with respect to those reported in the literature. Four presolar silicon carbide (SiC) and two presolar silicate grains were identified in the C-clasts. In addition, all the C-clasts contain moderate bulk D- and 15N-enrichments with the presence of sub-micron to micron-sized D and 15N hotspots, indicating the presence of primitive organic material. Comparison of the abundances and isotopic compositions of presolar grains and OM in these C-clasts with literature data for different samples of primitive extraterrestrial material provides support for (1) the genetic linkage of xenolithic C-clasts to highly aqueously altered but minimally heated carbonaceous chondritic materials and (2) a homogeneous distribution of circumstellar and interstellar materials in the protoplanetary disk. The low amounts of heat experienced by the C-clasts suggest that they arrived at Vesta and/or Vestoids at low speeds after the late heavy bombardment in the inner solar system ∼3.5–4.0 Gyr ago.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Carbonaceous chondrite</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Vesta</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Howardite Kapoeta</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">NanoSIMS</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Isotopic anomalies</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Presolar grains</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Organic matter</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ogliore, Ryan C.</subfield><subfield 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NanoSIMS isotopic investigation of xenolithic carbonaceous clasts from the kapoeta howardite

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