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1 Khatyrka meteorite, a recently described CV3 carbonaceous chondrite.
2 covered in the Khatyrka meteorite, a new CV3 carbonaceous chondrite.
3 5 and 0.050) and similar in color to some CM carbonaceous chondrites.
4 6O by an amount similar to that in CAIs from carbonaceous chondrites.
5  10(-5), indistinguishable from most CAIs in carbonaceous chondrites.
6 bsorption feature similar to CM- and CI-type carbonaceous chondrites.
7 bonate platform at the impact site, and most carbonaceous chondrites.
8 hondrites, which are distinct from all other carbonaceous chondrites.
9 e same region of the accretion disk as other carbonaceous chondrites.
10 d mineralogically similar to CI (Ivuna-type) carbonaceous chondrites.
11 richer in aromatics compared to less altered carbonaceous chondrites.
12  anomalies, which differ from those of other carbonaceous chondrites.
13 ts similar to primordial organics from other carbonaceous chondrites.
14 celadus' core needs to be similar to that of carbonaceous chondrites.
15 applied to aqueously formed carbonates in CM carbonaceous chondrites.
16 ic analogues are the volatile-rich CI and CM carbonaceous chondrites.
17 kylphosphonic acids have been recovered from carbonaceous chondrites.
18  iron meteorites with isotopic affinities to carbonaceous chondrites.
19  dust component may be comparable to that of carbonaceous chondrites.
20 bout 5,000 per thousand in organic matter in carbonaceous chondrites.
21 ame hydrogen isotopic composition as that of carbonaceous chondrites.
22 ns, some comets, and as a minor component in carbonaceous chondrites.
23 5)N-enriched organics from aqueously altered carbonaceous chondrites.
24 ces in fine-grained matrices of a variety of carbonaceous chondrites.
25 nts relative to the Sun's photosphere and CI carbonaceous chondrites.
26 s, other organic compounds and carbonates in carbonaceous chondrites.
27 ratios similar to the planetary component of carbonaceous chondrites.
28  isotopically anomalous noble gases found in carbonaceous chondrites.
29 orted by the identification of SiC grains in carbonaceous chondrites.
30 t abundance ratios equivalent to those of C1 carbonaceous chondrites.
31               They are probably analogues of carbonaceous chondrites(2,3) and are essential for under
32 hat has been linked to organic-rich hydrated carbonaceous chondrites(3).
33 th the ruthenium (Ru) isotope composition of carbonaceous chondrites(5,11), which is distinct from th
34 at the boulders are more porous than typical carbonaceous chondrites(6) and that their surroundings a
35 ponding to dense boulders similar to typical carbonaceous chondrites(6).
36 vered nine presolar silicate grains from the carbonaceous chondrite Acfer 094.
37 c microbial community was grown with the CM2 carbonaceous chondrite Aguas Zarcas as the sole carbon,
38 e, we show that chondrules and matrix in the carbonaceous chondrite Allende have complementary (183)W
39                   The D/H values of water in carbonaceous chondrites also argue against an influx of
40  mantle compositions between pyrolite and C1 carbonaceous chondrite and a lower mantle potential temp
41 on-rich (4 to 5 weight %), aqueously altered carbonaceous chondrite and contains high concentrations
42 egolith breccia composed of CM (Mighei)-type carbonaceous chondrite and highly reduced xenolithic mat
43 ocarbons resemble those in aqueously altered carbonaceous chondrites and are consistent with an abiot
44 r derivatives in the interstellar medium and carbonaceous chondrites and could close the gap of times
45  data point to a possible connection between carbonaceous chondrites and differentiated planetary mat
46 ygen isotopic diversity among CV, CM, and CI carbonaceous chondrites and displacement of the terrestr
47 stinguishable from that of the bulk water in carbonaceous chondrites and similar to that of terrestri
48  in the Earth is highly depleted relative to carbonaceous chondrites and solar abundances.
49 s an important addition to the collection of carbonaceous chondrites and still preserves pristine ext
50 rom accretionary material similar to average carbonaceous chondrites and that the noble gases in Eart
51                      We show that metal-rich carbonaceous chondrites and their components have a uniq
52                         Direct links between carbonaceous chondrites and their parent bodies in the s
53 tes in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standard
54 oatoms than in IOM from primitive (CI,CM,CR) carbonaceous chondrites, and thus it is distinguished fr
55               Matrix olivines in the Allende carbonaceous chondrite are believed to have formed by co
56 ium-aluminum-rich inclusion from the Allende carbonaceous chondrite are correlated with beryllium/bor
57                                              Carbonaceous chondrites are amongst the most chemically
58                                              Carbonaceous chondrites are asteroidal meteorites that c
59                                              Carbonaceous chondrites are considered to represent the
60  deuterium/hydrogen (D/H) values of water in carbonaceous chondrites are distinct from those in comet
61                                              Carbonaceous chondrites are less shocked than ordinary c
62                                              Carbonaceous chondrites are meteoritic fragments of aste
63 at, similarly to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals tha
64 tope variations among these organics in most carbonaceous chondrites are strongly correlated with mas
65                                              Carbonaceous chondrites are the most primitive rocks ava
66                        Water is preserved in carbonaceous chondrites as hydroxyl and/or H(2)O molecul
67 directed to analyses of organic compounds in carbonaceous chondrites because of their implications fo
68 suggest the micrometeorite is derived from a carbonaceous chondrite (best matched to a CO chondrite)
69 he anomalies are larger and more variable in carbonaceous chondrite (CC) meteorites than in noncarbon
70                                              Carbonaceous chondrites (CCs) contain the earliest prese
71           A long-standing question regarding carbonaceous chondrites (CCs) is how the CCs' organics w
72 richments in heavier zinc isotopes in heated carbonaceous chondrites compared to the typical ranges f
73 1) to 10(-1 )mol/kg across the full range of carbonaceous chondrite compositions and reaction conditi
74                                              Carbonaceous chondrite condensate olivine grains from tw
75 late accretion of chondrites, with a notable carbonaceous chondrite contribution.
76 d that the K and Rb isotopic compositions of carbonaceous chondrites correlate with their abundance d
77 hybasalt fragment enclosed in a Renazzo-type carbonaceous chondrite (CR).
78 ow-degree partial melting of a Vigarano-type carbonaceous chondrite (CV) from the oxidized subgroup a
79                                         Bulk carbonaceous chondrites display a deficit of approximate
80 e and carboxylic acids in a highly primitive carbonaceous chondrite (DOM 08006) with ~ 20 nm spatial
81          The similarity of mantle, crust and carbonaceous chondrites establishes that there were no n
82 be meteorite is the most accurately recorded carbonaceous chondrite fall.
83   We analyze short-lived uranium isotopes in carbonaceous chondrites, finding excesses of 234-uranium
84                                      Because carbonaceous chondrites formed 4.5 billion years ago, th
85 ocks across the S2 impact event (37 to 58 km carbonaceous chondrite) forming part of the 3.26 Ga Fig
86 st reservoirs prior to their delivery to the carbonaceous-chondrite-forming region, which likely resi
87 u and CI chondrites are higher than in other carbonaceous chondrite groups but are similar to that of
88 drules in the metal-rich CB (Bencubbin-like) carbonaceous chondrites Gujba (4,562.7 +/- 0.5 Myr) and
89  in space and attempts to find fullerenes in carbonaceous chondrites have been unsuccessful.
90 the rare pre-solar grains in the matrixes of carbonaceous chondrites have been used to identify some
91 les from Ryugu are comparable to unheated CI carbonaceous chondrites; however, reflectance spectra of
92 drogen to those present in aqueously altered carbonaceous chondrites; however, the concentration of i
93 ns in some iron, nickel metal grains from CH carbonaceous chondrites imply formation at temperatures
94 s were originally 16O-rich, but that in most carbonaceous chondrite inclusions some minerals exchange
95  that the paleomagnetism of chondrules in CO carbonaceous chondrites indicates the presence of a 101
96 surpassing significantly the levels found in carbonaceous chondrites, indicating either a significant
97  the molybdenum isotopic composition of bulk carbonaceous chondrites is distinctly different from the
98 rkite (CuAl2) and cupalite (CuAl) in the CV3 carbonaceous chondrite Khatyrka has posed a mystery as t
99 n a fragment of the quasicrystal-bearing CV3 carbonaceous chondrite Khatyrka recovered from fine-grai
100 e delivery of most of Earth's volatiles from carbonaceous chondrite-like precursors.
101 ate accretion of a late veneer consisting of carbonaceous-chondrite-like material after core formatio
102 ther isotope systems, then late accretion of carbonaceous-chondrite-like material must contribute ~ 3
103 late veneer contained substantial amounts of carbonaceous-chondrite-like materials with their charact
104 er was a approximately 170-km-diameter body (carbonaceous-chondrite-like) that broke up 160(-20)+30My
105  isotopic differences do not exist, and that carbonaceous chondrites, mantle and crust all have the s
106 tion of primordial organic matter within the carbonaceous chondrite Maribo that is distinct from the
107 of accreted interplanetary dust particles or carbonaceous chondrite material.
108                                We infer that carbonaceous chondrite matrices are not pristine: they f
109                      In this framework, most carbonaceous chondrites may have originated from regions
110                    Isotopic variations among carbonaceous chondrites may thus reflect fractionation o
111       Exogenic materials, such as water-rich carbonaceous chondrites, may be the source of volatiles,
112 microscopy, shows that carbon in the Allende carbonaceous chondrite meteorite is predominantly a poor
113 rements of whole chondrules from the Allende carbonaceous chondrite meteorite show that some aluminum
114 vered in oxidized acid residues from several carbonaceous chondrite meteorites (for example, the C de
115 onsistent with those in chemically primitive carbonaceous chondrite meteorites that experienced paren
116 ntation to form breccias, which dominate the carbonaceous chondrite meteorites(14).
117 ly composed of materials similar to those of carbonaceous chondrite meteorites, particularly the CI (
118 mall fraction of hydrated materials, such as carbonaceous chondrite meteorites, which originated in t
119  similar to those found in aqueously altered carbonaceous chondrite meteorites.
120 ilar to thermally and/or shock-metamorphosed carbonaceous chondrite meteorites.
121 to the insoluble organic matter found in the carbonaceous chondrite meteorites.
122 instead overlap those of anhydrous phases in carbonaceous chondrite meteorites.
123 sical properties remain poorly known because carbonaceous chondrite meteoroids tend not to survive en
124 erature (150-400 degrees C) pyrolysis of the carbonaceous chondrite Murchison with chloride or perchl
125 of HMT and functionalized HMT species in the carbonaceous chondrites Murchison, Murray, and Tagish La
126 soluble organic matter (IOM) isolated from a carbonaceous chondrite (Murchison, CM2).
127 radual accumulation of hydrogen by infall of carbonaceous chondrites--observed as clasts in some howa
128 e for Earth's collision with a rare swarm of carbonaceous chondrites or comets at the onset of the Yo
129 hould therefore be higher than those seen in carbonaceous chondrites or comets.
130 drogen and nitrogen isotopic compositions in carbonaceous chondrite organic matter reach and even exc
131  plate for the ancient impact environment of carbonaceous chondrite parent bodies.
132 iencies of small FeNi metal grains among the carbonaceous chondrite parent bodies.
133                                        These carbonaceous chondrites provide the first unequivocal ev
134 ctron microscope observations of the Allende carbonaceous chondrite provided evidence of widespread h
135 ort high-precision K and Rb isotopic data of carbonaceous chondrites, providing new insights into the
136 bility in barium, neodymium, and samarium in carbonaceous chondrites reflects the distinct stellar nu
137                            These results for carbonaceous chondrites reveal that late accretion, cons
138 s are ubiquitous in star-forming regions and carbonaceous chondrites, serving as essential intermedia
139 urements of 7 AOAs from weakly metamorphosed carbonaceous chondrites show large, mass-dependent, ligh
140                                              Carbonaceous chondrites such as the Murchison meteorite,
141 grains in the matrix of the Alais (class CI) carbonaceous chondrite, suggesting that these meteoritic
142 y with a cryo-stage of the aqueously altered carbonaceous chondrite Sutter's Mill.
143 Khatyrka meteorite, a recently described CV3 carbonaceous chondrite that experienced shock metamorphi
144                                A new type of carbonaceous chondrite, the Tagish Lake meteorite, exhib
145       Although fluid alteration is common in carbonaceous chondrites, the discovery of margarite with
146                 Analyses have now shown this carbonaceous chondrite to contain a suite of soluble org
147 oidal magnetite grain within the Tagish Lake carbonaceous chondrite to demonstrate that the interlock
148 leomagnetic measurements of chondrules in CO carbonaceous chondrites to investigate the existence and
149 mium isotopic signature is consistent with a carbonaceous chondrite-type impactor.
150           We determine that a combination of carbonaceous chondrite-type materials were responsible f
151 space, have been discovered in three CV-type carbonaceous chondrites via Raman imaging and electron m
152 boxylic acids from Murchison meteorite, a C2 carbonaceous chondrite which fell in Australia in 1969.
153 e Fe isotopic composition of the Orgueil CI1 carbonaceous chondrite, which best approximates the sola
154 type (CI) chondrites are distinct from other carbonaceous chondrites, which has led to the suggestion

 
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