ライフサイエンスコーパス: chondrite

1 a and primitive undifferentiated meteorites (chondrites).

2 e Khatyrka meteorite, a new CV3 carbonaceous chondrite.

3 orite, a recently described CV3 carbonaceous chondrite.

4 roximately +14 parts per million relative to chondrite.

5 r thousand in organic matter in carbonaceous chondrites.

6 re depleted in volatile elements relative to chondrites.

7 isotopic composition as that of carbonaceous chondrites.

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

9 that of some deep mantle plumes rather than chondrites.

10 rich inclusion similar to those found in CV3 chondrites.

11 anoglobules that are ubiquitous in primitive chondrites.

12 dominate the most primitive meteorites, the chondrites.

13 rlier than the parent bodies of the ordinary chondrites.

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

15 rained matrices of a variety of carbonaceous chondrites.

16 served in refractory inclusions in primitive chondrites.

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

18 in accretionary rims around chondrules in CM chondrites.

19 nic compounds and carbonates in carbonaceous chondrites.

20 r to the planetary component of carbonaceous chondrites.

21 anomalous noble gases found in carbonaceous chondrites.

22 identification of SiC grains in carbonaceous chondrites.

23 explain the petrologically diverse nature of chondrites.

24 atios equivalent to those of C1 carbonaceous chondrites.

25 and similar in color to some CM carbonaceous chondrites.

26 nt similar to that in CAIs from carbonaceous chondrites.

27 Al-rich objects from unequilibrated ordinary chondrites.

28 stinguishable from most CAIs in carbonaceous chondrites.

29 primordial organics from other carbonaceous chondrites.

30 ture similar to CM- and CI-type carbonaceous chondrites.

31 on in all primitive meteorites except the CI-chondrites.

32 lighter Ni isotopic composition compared to chondrites.

33 rm at the impact site, and most carbonaceous chondrites.

34 ich are distinct from all other carbonaceous chondrites.

35 re abundant in carbonaceous but not ordinary chondrites.

36 of the accretion disk as other carbonaceous chondrites.

37 igarano-type, Mighei-type, and Renazzo-type) chondrites.

38 rt a close relationship between Ryugu and CI chondrites.

39 solar system, are based on the spectra of CI chondrites.

40 red chondrules, which are ubiquitous in many chondrites.

41 tes with isotopic affinities to carbonaceous chondrites.

42 oxidation state or petrological type of the chondrites.

43 on Ceres is lower than in the aforementioned chondrites.

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

45 ut coeval to chondrule formation in ordinary chondrites.

46 organics from aqueously altered carbonaceous chondrites.

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

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

49 needs to be similar to that of carbonaceous chondrites.

50 ueously formed carbonates in CM carbonaceous chondrites.

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

52 acids have been recovered from carbonaceous chondrites.

53 nt may be comparable to that of carbonaceous chondrites.

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

55 ), solar-wind-irradiated material(16) and CI chondrites(17).

56 They are probably analogues of carbonaceous chondrites(2,3) and are essential for understanding plan

57 linked to organic-rich hydrated carbonaceous chondrites(3).

58 ium (Ru) isotope composition of carbonaceous chondrites(5,11), which is distinct from that of the mod

59 rs are more porous than typical carbonaceous chondrites(6) and that their surroundings are covered wi

60 nse boulders similar to typical carbonaceous chondrites(6).

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

62 unevenly distributed throughout the various chondrite accretion regions.

63 esolar silicate grains from the carbonaceous chondrite Acfer 094.

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

65 ommunity was grown with the CM2 carbonaceous chondrite Aguas Zarcas as the sole carbon, energy and nu

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

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

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

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

70 5 weight %), aqueously altered carbonaceous chondrite and contains high concentrations of presolar g

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

72 o a possible connection between carbonaceous chondrites and differentiated planetary materials, sugge

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

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

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

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

77 he Moon is similar to those of the Earth and chondrites and reflects both the relative homogeneity of

78 hile the distinct isotopic composition of CI chondrites and Ryugu may reflect their formation further

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

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

81 t addition to the collection of carbonaceous chondrites and still preserves pristine extraterrestrial

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

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

84 +/- 0.5 per cent higher than the average for chondrites and that the initial (142)Nd/(144)Nd ratio of

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

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

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

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

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

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

91 Direct links between carbonaceous chondrites and their parent bodies in the solar system a

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

93 carbonaceous chondrite (best matched to a CO chondrite) and entered the atmosphere a high speed (~16

94 thwest Africa 1172 (NWA 1172; an H5 ordinary chondrite) and releases free soluble metals, with Ni ion

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

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

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

98 n IOM from primitive (CI,CM,CR) carbonaceous chondrites, and thus it is distinguished from most of th

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

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

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

102 Carbonaceous chondrites are amongst the most chemically primitive sol

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

104 Carbonaceous chondrites are asteroidal meteorites that contain abunda

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

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

107 Carbonaceous chondrites are less shocked than ordinary chondrites, re

108 Carbonaceous chondrites are meteoritic fragments of asteroids that av

109 hat matrices of the most unaltered CM and CV chondrites are overall CI-like (Ivuna-type) (similar to

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

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

112 ns among these organics in most carbonaceous chondrites are strongly correlated with mass-independent

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

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

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

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

117 spectra are reproduced by heating Orgueil CI chondrite at 300 degrees C under reducing conditions, wh

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

119 icrometeorite is derived from a carbonaceous chondrite (best matched to a CO chondrite) and entered t

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

121 aribo represents one of the least altered CM chondrite breccias found to date and contains primordial

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

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

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

125 Carbonaceous chondrites (CCs) contain the earliest preserved Solar Sy

126 ong-standing question regarding carbonaceous chondrites (CCs) is how the CCs' organics were sourced a

127 CAIs from all chondrite classes formed under oxidizing conditions that

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

129 heavier zinc isotopes in heated carbonaceous chondrites compared to the typical ranges for chondritic

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

131 mol/kg across the full range of carbonaceous chondrite compositions and reaction conditions considere

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

133 Carbonaceous chondrite condensate olivine grains from two distinct pe

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

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

136 reviously reported Khatyrka meteorite - a CV chondrite containing near-identical alloys and the only

137 hich is a thermally-metamorphosed H ordinary chondrite contains a primitive xenolithic clast that was

138 ment enclosed in a Renazzo-type carbonaceous chondrite (CR).

139 tial melting of a Vigarano-type carbonaceous chondrite (CV) from the oxidized subgroup at a depth whe

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

141 Bulk carbonaceous chondrites display a deficit of approximately 100 parts

142 Chondrites display isotopic variations for moderately vo

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

144 lic acids in a highly primitive carbonaceous chondrite (DOM 08006) with ~ 20 nm spatial resolution us

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

146 Enstatite chondrite (EC) meteorites have similar isotopic composit

147 g the primitive meteorite classes, Enstatite Chondrites (EC) are believed to share a common origin wi

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

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

150 e anhydrous primary minerals in Ryugu and CI chondrites exhibit a bimodal distribution of oxygen isot

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

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

153 Although chondrites formed at greater heliocentric distances and

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

155 es, therefore, demonstrate that Ryugu and CI chondrites formed in a reservoir that was different from

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

157 he S2 impact event (37 to 58 km carbonaceous chondrite) forming part of the 3.26 Ga Fig Tree Group, S

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

159 By subjecting CM chondrite fragments to fast, open system, cyclic heating

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

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

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

163 ractory, and Nb/Ta is fairly constant across chondrite groups, this can only be explained by a prefer

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

165 gregate and the clast are unique among known chondrite groups.

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

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

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

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

170 Enstatite chondrites have often been considered to be closely rela

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

172 lyses in micro-milled phase separates of EH3 chondrites, here we report the presence of significantly

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

174 u are comparable to unheated CI carbonaceous chondrites; however, reflectance spectra of Ryugu sample

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

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

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

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

179 impact and alteration history of L6 ordinary chondrites in general.

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

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

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

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

184 gnificantly the levels found in carbonaceous chondrites, indicating either a significant concentratio

185 bulk silicate Earth (BSE) estimate based on chondrites is 0.052 +/- 0.006 per mille heavier than the

186 the elevated delta(30)Si of BSE compared to chondrites is consistent with earlier conclusions that l

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

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

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

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

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

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

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

194 ined by Earth's early accretion of enstatite chondrite-like impactors, followed by accretion of incre

195 of a late veneer consisting of carbonaceous-chondrite-like material after core formation had ceased(

196 systems, then late accretion of carbonaceous-chondrite-like material must contribute ~ 30-100% of the

197 If Earth is comprised primarily of enstatite-chondrite-like material, as indicated by other isotope s

198 creasingly oxidized impactors and minimal CI chondrite-like materials before and during the Moon-form

199 ontained substantial amounts of carbonaceous-chondrite-like materials with their characteristic (100)

200 egassing, as metamorphic devolatilization on chondrite-like precursors is insufficient to account for

201 most of Earth's volatiles from carbonaceous chondrite-like precursors.

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

203 Ryugu's samples are CI chondrite-like, rich in water and organic material, and

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

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

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

207 rdial organic matter within the carbonaceous chondrite Maribo that is distinct from the majority of o

208 net witnessed a massive infall of ordinary L chondrite material about 466 million years ago(1-3) that

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

210 nterplanetary dust particles or carbonaceous chondrite material.

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

212 experiments at 3-7 km s(-1) using analogs of chondrite matrices reveal evidence of local heating in t

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

214 In this framework, most carbonaceous chondrites may have originated from regions around the b

215 Isotopic variations among carbonaceous chondrites may thus reflect fractionation of distinct du

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

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

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

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

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

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

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

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

224 -(176)Hf/(177)Hf composition within error of chondrite meteorites, which include the likely parent bo

225 of hydrated materials, such as carbonaceous chondrite meteorites, which originated in the outer Sola

226 hose found in aqueously altered carbonaceous chondrite meteorites.

227 ap those of anhydrous phases in carbonaceous chondrite meteorites.

228 ally and/or shock-metamorphosed carbonaceous chondrite meteorites.

229 r than those in Ivuna-type carbonaceous (CI) chondrite meteorites.

230 ble organic matter found in the carbonaceous chondrite meteorites.

231 ies remain poorly known because carbonaceous chondrite meteoroids tend not to survive entry to Earth'

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

233 400 degrees C) pyrolysis of the carbonaceous chondrite Murchison with chloride or perchlorate as chlo

234 nctionalized HMT species in the carbonaceous chondrites Murchison, Murray, and Tagish Lake.

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

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

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

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

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

240 Here we show that the Kakowa (L6) ordinary chondrite (OC) preserves both shock-melt veins and pocke

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

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

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

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

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

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

247 Previous assignments of CI chondrite parent bodies, i.e., chemically most primitive

248 ates early-forming bodies from later-forming chondrite parent bodies, which accreted 2 to 3 million y

249 e ancient impact environment of carbonaceous chondrite parent bodies.

250 an, in connection with the break-up of the L-chondrite parent body, do we observe an anomalous microm

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

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

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

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

255 ision K and Rb isotopic data of carbonaceous chondrites, providing new insights into the cause of the

256 , we report cyanide abundance in a set of CM chondrites ranging from 50 +/- 1 to 2472 +/- 38 nmol.g(-

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

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

259 us chondrites are less shocked than ordinary chondrites, regardless of the degree of aqueous alterati

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

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

262 se for solar-wind-irradiated material and CI chondrites, requiring the presence of nebular neon in th

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

264 ponents from a common reservoir, implying CI chondrites/Ryugu may have formed in the same region of t

265 Chondrite samples were composed of silicates (olivine, p

266 ous in star-forming regions and carbonaceous chondrites, serving as essential intermediates in metabo

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

268 AOAs from weakly metamorphosed carbonaceous chondrites show large, mass-dependent, light Si isotope

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

270 Carbonaceous chondrites such as the Murchison meteorite, which landed

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

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

273 kinship to aqueously altered CI (Ivuna-type) chondrites, suggesting similar origins.

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

275 terials is more similar to that of enstatite chondrites than previously proposed(1,2).

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

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

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

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

280 h fluid alteration is common in carbonaceous chondrites, the discovery of margarite with an OC oxygen

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

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

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

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

285 te grain within the Tagish Lake carbonaceous chondrite to demonstrate that the interlocking crystal a

286 easurements of chondrules in CO carbonaceous chondrites to investigate the existence and nature of th

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

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

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

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

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

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

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

294 luble Cr are highly variable in Ryugu and CI chondrites, whereas those of Ti are relatively uniform.

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

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

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

298 alies indistinguishable from Ivuna-type (CI) chondrites, which are distinct from all other carbonaceo

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

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