ライフサイエンスコーパス: chondrite

1 a and primitive undifferentiated meteorites (chondrites).

2 orite, a recently described CV3 carbonaceous chondrite.

3 roximately +14 parts per million relative to chondrite.

4 e Khatyrka meteorite, a new CV3 carbonaceous chondrite.

5 on Ceres is lower than in the aforementioned chondrites.

6 dominate the most primitive meteorites, the chondrites.

7 rlier than the parent bodies of the ordinary chondrites.

8 ich are likely to be the parent bodies of LL chondrites.

9 rained matrices of a variety of carbonaceous chondrites.

10 served in refractory inclusions in primitive chondrites.

11 to the Sun's photosphere and CI carbonaceous chondrites.

12 in accretionary rims around chondrules in CM chondrites.

13 nic compounds and carbonates in carbonaceous chondrites.

14 r to the planetary component of carbonaceous chondrites.

15 anomalous noble gases found in carbonaceous chondrites.

16 identification of SiC grains in carbonaceous chondrites.

17 explain the petrologically diverse nature of chondrites.

18 atios equivalent to those of C1 carbonaceous chondrites.

19 and similar in color to some CM carbonaceous chondrites.

20 nt similar to that in CAIs from carbonaceous chondrites.

21 n the bulk silicate Earth are the same as in chondrites.

22 Al-rich objects from unequilibrated ordinary chondrites.

23 stinguishable from most CAIs in carbonaceous chondrites.

24 ut coeval to chondrule formation in ordinary chondrites.

25 65), was found in the same beds that yield L chondrites.

26 has a greater (142)Nd/(144)Nd ratio than do chondrites.

27 needs to be similar to that of carbonaceous chondrites.

28 ueously formed carbonates in CM carbonaceous chondrites.

29 are the volatile-rich CI and CM carbonaceous chondrites.

30 acids have been recovered from carbonaceous chondrites.

31 nt may be comparable to that of carbonaceous chondrites.

32 oxidation state or petrological type of the chondrites.

33 r thousand in organic matter in carbonaceous chondrites.

34 re depleted in volatile elements relative to chondrites.

35 isotopic composition as that of carbonaceous chondrites.

36 ts, and as a minor component in carbonaceous chondrites.

37 that of some deep mantle plumes rather than chondrites.

38 rich inclusion similar to those found in CV3 chondrites.

39 anoglobules that are ubiquitous in primitive chondrites.

40 erved s-process deficiency, which produced a chondrite 146Sm-142Nd isochron consistent with previous

41 ratio or Fe content, which suggests that C1 chondrite accretion models are insufficient to explain t

42 unevenly distributed throughout the various chondrite accretion regions.

43 esolar silicate grains from the carbonaceous chondrite Acfer 094.

44 h regions are consistent with those of LL5-6 chondrites after continuum removal.

45 at chondrules and matrix in the carbonaceous chondrite Allende have complementary (183)W anomalies re

46 The D/H values of water in carbonaceous chondrites also argue against an influx of water ice fro

47 sitions between pyrolite and C1 carbonaceous chondrite and a lower mantle potential temperature of 15

48 mportant phase as a mineral in the Tenham L6 chondrite and approved by the International Mineralogica

49 5 weight %), aqueously altered carbonaceous chondrite and contains high concentrations of presolar g

50 ia composed of CM (Mighei)-type carbonaceous chondrite and highly reduced xenolithic materials.

51 diversity among CV, CM, and CI carbonaceous chondrites and displacement of the terrestrial planets f

52 per million in the 138Ba/136Ba ratio between chondrites and Earth.

53 arable to values for carbonates in CI and CM chondrites and for several classes of differentiated met

54 ly -5 per thousand, consistent with those of chondrites and other planetary body.

55 from that of the bulk water in carbonaceous chondrites and similar to that of terrestrial water, imp

56 is highly depleted relative to carbonaceous chondrites and solar abundances.

57 f 26Al are present throughout the classes of chondrites and strengthens the notion that 26Al was wide

58 to 0.040 per mil) as compared with primitive chondrites and terrestrial standards.

59 ary material similar to average carbonaceous chondrites and that the noble gases in Earth's atmospher

60 r this effect, the (142)Nd/(144)Nd ratios of chondrites and the accessible Earth are indistinguishabl

61 he ratio of (142)Nd/(144)Nd between ordinary chondrites and the Earth must be due to a process differ

62 sotopic composition of the abundant ordinary chondrites and the primitive (16)O-rich component of CAI

63 sotopic composition of the abundant ordinary chondrites and the primitive 16O-rich component of CAIs.

64 We show that metal-rich carbonaceous chondrites and their components have a unique isotopic s

65 ns within two carbonaceous Renazzo-type (CR) chondrites and two interplanetary dust particles (IDPs)

66 of the four major classes: iron, stony iron, chondrites, and achondrites.

67 samples is less aromatic than that in the CR chondrites, and its functional group chemistry is mainly

68 ry (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are

69 Matrix olivines in the Allende carbonaceous chondrite are believed to have formed by condensation pr

70 rich inclusion from the Allende carbonaceous chondrite are correlated with beryllium/boron in a manne

71 , enstatite, Rumuruti and primitive ordinary chondrites are about 6 times, 9 times and 15-37 times lo

72 Organic grains in CR chondrites are associated with carbonates and elemental

73 Carbonaceous chondrites are asteroidal meteorites that contain abunda

74 Carbonaceous chondrites are considered to represent the 'average' Sol

75 drogen (D/H) values of water in carbonaceous chondrites are distinct from those in comets and Saturn'

76 Carbonaceous chondrites are meteoritic fragments of asteroids that av

77 to cometary bodies, metal-rich carbonaceous chondrites are samples of planetesimals that accreted be

78 um-rich inclusions (CAIs) from enstatite (E) chondrites are similar to those of CAIs from other chond

79 Carbonaceous chondrites are the most primitive rocks available to us,

80 oplets and, judging from their abundances in chondrites, are the products of one of the most energeti

81 f chemical elements in primitive meteorites (chondrites), as building blocks of terrestrial planets,

82 alite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine

83 nalyses of organic compounds in carbonaceous chondrites because of their implications for organic che

84 actions in the highly metamorphosed ordinary chondrite breccia Villalbeto de la Pena (L6).

85 rite group; they are depleted relative to CI chondrites, but are enriched relative to bulk compositio

86 topes of potassium compared to the Earth and chondrites (by around 0.4 parts per thousand).

87 r rocks compared with those of the Earth and chondrites can be best explained as the result of the in

88 CAIs from all chondrite classes formed under oxidizing conditions that

89 ites are similar to those of CAIs from other chondrite classes.

90 nanometers) are consistent with an ordinary chondrite composition for which the measured mean densit

91 , there must be many asteroids with ordinary-chondrite compositions in near-Earth orbits.

92 Carbonaceous chondrite condensate olivine grains from two distinct pe

93 te and sylvite within the Monahans (1998) H5 chondrite contain aqueous fluid inclusions.

94 Halite crystals from the Zag H3-6 chondrite contain essentially pure (monoisotopic) xenon-

95 asurements of 14 chondrules from the Allende chondrite define a (26)Al isochron with (26)Al/(27)Al =

96 Bulk carbonaceous chondrites display a deficit of approximately 100 parts

97 Osmium from metamorphosed bulk chondrites does not have isotope anomalies, implying tha

98 Here we show that, compared with chondrites, Earth's precursor bodies were enriched in ne

99 ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as Myr after calcium-al

100 similarity of mantle, crust and carbonaceous chondrites establishes that there were no nebular reserv

101 solar nebula and were transported into the E chondrite formation region.

102 Because carbonaceous chondrites formed 4.5 billion years ago, the results are

103 Although chondrites formed at greater heliocentric distances and

104 e that chondrules and metal grains in the CB chondrites formed from a vapour-melt plume produced by a

105 om the reducing conditions under which the E chondrites formed.

106 Among these, Renazzo-type (CR) chondrites found in Antarctica appear remarkably pristin

107 that the majority of chondrules from a given chondrite group formed in a narrow time interval.

108 nt abundances are characteristic for a given chondrite group; they are depleted relative to CI chondr

109 lack of evidence for this material in other chondrite groups requires isolation from the outer Solar

110 iform CI-like chemistry across the different chondrite groups.

111 metal-rich CB (Bencubbin-like) carbonaceous chondrites Gujba (4,562.7 +/- 0.5 Myr) and Hammadah al H

112 Osmium extracted from unequilibrated bulk chondrites has isotope anomalies consistent with an inso

113 attempts to find fullerenes in carbonaceous chondrites have been unsuccessful.

114 solar grains in the matrixes of carbonaceous chondrites have been used to identify some sources of th

115 Enstatite chondrites have often been considered to be closely rela

116 oximately 50 chondrules from CV and ordinary chondrites) have an inferred minimum bulk initial ((26)A

117 (Cr)] in the bulk silicate Earth relative to chondrites, however, remain debated between leading cand

118 se present in aqueously altered carbonaceous chondrites; however, the concentration of iron on Ceres

119 SE) might have an Sm/Nd ratio 6% higher than chondrites (i.e., the BSE is superchondritic).

120 on, nickel metal grains from CH carbonaceous chondrites imply formation at temperatures from 1370 to

121 red in the metal from several unequilibrated chondrites, implying a 60Fe/56Fe ratio of approximately

122 ally 16O-rich, but that in most carbonaceous chondrite inclusions some minerals exchanged oxygen isot

123 d anomalous iron meteorites and H, L, and LL chondrites indicate that their parent bodies accreted ra

124 essure phases never observed before in a CV3 chondrite, indicating that an impact shock generated a h

125 per cubic centimeter, about half that of CM chondrites, indicating a porous interior structure.

126 e isotopic homogeneity of metamorphosed bulk chondrites is consistent with extremely effective mixing

127 um isotopic composition of bulk carbonaceous chondrites is distinctly different from the accepted ave

128 We contend that the amount of CAIs in CV chondrites is two to three times as low as the 10 volume

129 and cupalite (CuAl) in the CV3 carbonaceous chondrite Khatyrka has posed a mystery as to what extrat

130 of the quasicrystal-bearing CV3 carbonaceous chondrite Khatyrka recovered from fine-grained, clay-ric

131 y-like body (or, alternatively, an enstatite-chondrite-like body) rich in sulfur to the early Earth w

132 han with simple accretion of a volatile-rich chondrite-like body.

133 oximately 170-km-diameter body (carbonaceous-chondrite-like) that broke up 160(-20)+30Myr ago in the

134 the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed and Myr after CAI

135 depletions in volatile elements relative to chondrites, making them ideal samples with which to stud

136 ferences do not exist, and that carbonaceous chondrites, mantle and crust all have the same 37Cl/35Cl

137 the shock compression of analogue precursor chondrite material was probed using state of the art dyn

138 nterplanetary dust particles or carbonaceous chondrite material.

139 We infer that carbonaceous chondrite matrices are not pristine: they formed from a

140 latile-rich nature of chondrule rims and the chondrite matrix.

141 c materials, such as water-rich carbonaceous chondrites, may be the source of volatiles, suggesting t

142 and calcium depletions, relative to ordinary chondrites, may represent signatures of limited partial

143 hows that carbon in the Allende carbonaceous chondrite meteorite is predominantly a poorly crystallin

144 ole chondrules from the Allende carbonaceous chondrite meteorite show that some aluminum-rich Allende

145 ized acid residues from several carbonaceous chondrite meteorites (for example, the C delta component

146 ecursor materials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particle

147 ions (CAIs) from the unequilibrated ordinary chondrite meteorites Quinyambie and Semarkona are enrich

148 matching the most commonly falling ordinary chondrite meteorites), however, are seen among small bod

149 ble organic matter found in the carbonaceous chondrite meteorites.

150 ap those of anhydrous phases in carbonaceous chondrite meteorites.

151 rules in the oxidized, aqueously altered CV3 chondrite Mokoia have large excesses of radiogenic chrom

152 400 degrees C) pyrolysis of the carbonaceous chondrite Murchison with chloride or perchlorate as chlo

153 ic matter (IOM) isolated from a carbonaceous chondrite (Murchison, CM2).

154 EE data obtained from the GRMs, presented as chondrite normalized patterns, are in very good agreemen

155 One distinct grain from the CR chondrite NWA 852 exhibits a rim structure only visible

156 lation of hydrogen by infall of carbonaceous chondrites--observed as clasts in some howardites--and s

157 Although ordinary chondrite (OC) meteorites dominate observed falls, the i

158 e most populous class of meteorite (ordinary chondrites, OC) do not match the remotely observed surfa

159 collision with a rare swarm of carbonaceous chondrites or comets at the onset of the Younger Dryas c

160 re be higher than those seen in carbonaceous chondrites or comets.

161 must instead be composed of unsampled 'Earth chondrite' or 'Earth achondrite'.

162 trogen isotopic compositions in carbonaceous chondrite organic matter reach and even exceed those fou

163 Chronology of aqueous activity on chondrite parent bodies constrains their accretion times

164 ites to Earth following the breakup of the L-chondrite parent body.

165 fragment of the impactor that broke up the L-chondrite parent body.

166 The unique chondrules in CB chondrites probably formed in a vapour-melt plume produc

167 ope observations of the Allende carbonaceous chondrite provided evidence of widespread hydrous phases

168 its effects requires that key aspects of the chondrite record be re-evaluated: palaeomagnetism, petro

169 ium, neodymium, and samarium in carbonaceous chondrites reflects the distinct stellar nucleosynthetic

170 e conclusion that the deficiency in 142Nd in chondrites relative to terrestrial rocks reflects 146Sm

171 * and (54)Cr compositions of bulk metal-rich chondrites require significant amounts (25-50%) of primo

172 These results for carbonaceous chondrites reveal that late accretion, constrained to a

173 The ratios Br/Cl and I/Cl in all studied chondrites show a limited range, indistinguishable from

174 ndance of 146Sm and a 142Nd/144Nd at average chondrite Sm/Nd ratio that is lower than that measured i

175 Carbonaceous chondrites such as the Murchison meteorite, which landed

176 gen and nitrogen isotopic compositions of CI chondrites suggest that they were the principal source o

177 matrix of the Alais (class CI) carbonaceous chondrite, suggesting that these meteoritic sulfides may

178 r in 107Ag/109Ag to primitive, volatile-rich chondrites, suggesting that Earth accreted a considerabl

179 orite, a recently described CV3 carbonaceous chondrite that experienced shock metamorphism, local mel

180 ween the Th/Hf and (176)Hf/(177)Hf ratios in chondrites that reflects remobilization of Lu and Th dur

181 Puzzlingly, the parent bodies of ordinary chondrites (the most abundant type of meteorites) do not

182 A new type of carbonaceous chondrite, the Tagish Lake meteorite, exhibits a reflect

183 , indium and alkali elements) relative to CI chondrites, the meteorites that compositionally most clo

184 he least abundant of ordinary (H, L, and LL) chondrites, there must be many asteroids with ordinary-c

185 et between the accessible silicate Earth and chondrites therefore reflects a higher proportion of s-p

186 Analyses have now shown this carbonaceous chondrite to contain a suite of soluble organic compound

187 signature is consistent with a carbonaceous chondrite-type impactor.

188 determine that a combination of carbonaceous chondrite-type materials were responsible for the majori

189 , more oxidizing epoch in the region where E chondrites ultimately formed, or they formed at a differ

190 een discovered in three CV-type carbonaceous chondrites via Raman imaging and electron microscopy.

191 )Fe ratio of terrestrial basalts relative to chondrites was proposed to be a fingerprint of core-mant

192 ize presolar diamonds from the Efremovka CV3 chondrite were physically separated into several grain s

193 planetesimals, such as the parent bodies of chondrites, were still being formed.

194 from Murchison meteorite, a C2 carbonaceous chondrite which fell in Australia in 1969.

195 cubic metre (that is, composed of CI and CM chondrites), which yields an outer-shell thickness of 70

196 composition of the Orgueil CI1 carbonaceous chondrite, which best approximates the solar composition

197 anomalous enrichments in (33)S, relative to chondrites, which have been attributed to photochemistry

198 Chondrules are the major component of chondrites, yet little is known about their formation me