ライフサイエンスコーパス: meteorite

1 +/- 10% CAIs (two to three times that of any meteorite).

2 iscovery of trapped atmospheric gases in one meteorite.

3 been reported previously for this or any CI meteorite.

4 e a natural shock that affected the Khatyrka meteorite.

5 known natural quasicrystals, in the Khatyrka meteorite.

6 olcanic province and impact of the Chicxulub meteorite.

7 measurements conducted on an iron-containing meteorite.

8 stal to be identified, was found in the same meteorite.

9 ls relevant to meteorites, including Martian meteorites.

10 em from the recognition of numerous basaltic meteorites.

11 scientific value as archives of old ice and meteorites.

12 it marked compositional differences from the meteorites.

13 nd have lower manganese/iron ratios than the meteorites.

14 ted in isolated occurrences in other Martian meteorites.

15 Gusev crater on Mars and of martian basaltic meteorites.

16 e the carrier of anomalous (22)Ne in ancient meteorites.

17 the Vestoids and howardite-eucrite-diogenite meteorites.

18 been determined to be indigenous to numerous meteorites.

19 asaltic howardite-eucrite-diogenite class of meteorites.

20 f anhydrous phases in carbonaceous chondrite meteorites.

21 ce Vesta-family asteroids (Vestoids) and HED meteorites.

22 oposed experimental protocol and its use for meteorites.

23 s of howardite, eucrite, and diogenite (HED) meteorites.

24 found in life on Earth have been detected in meteorites.

25 tic nucleobases along with vitamins found in meteorites.

26 y system in shergottite-nakhlite-chassignite meteorites.

27 relative to the Earth, Moon, Mars, and bulk meteorites.

28 containing material comparable to chondritic meteorites.

29 aracteristic of apatite in igneous rocks and meteorites.

30 of the difference in colour of asteroids and meteorites.

31 ry disks, and X-ray flare effects on ancient meteorites.

32 isotopically different from most macroscopic meteorites.

33 s to determine orbits and fall positions for meteorites.

34 ynthetic effects that may be present in iron meteorites.

35 heir higher abundance in thermally processed meteorites.

36 t was isotopically most similar to enstatite meteorites.

37 ater and their minimum age by erosion of the meteorites.

38 c matter found in the carbonaceous chondrite meteorites.

39 data for the Earth, the Moon and chondritic meteorites.

40 avier magnesium compositions than chondritic meteorites.

41 t productive regions on Earth for collecting meteorites.

42 le planets such as early Earth by comets and meteorites.

43 , previously molten, spherules found in most meteorites.

44 ere pairs are separate fragments of a single meteorite), 8 nakhlites (5 plus 3 pairs), Allan Hills 84

45 y be due to englacial solar warming, whereby meteorites a few tens of centimetres below the ice surfa

46 Here we show that the Tissint meteorite, a 2011 meteorite fall, contains virtually all

47 ite, was recently discovered in the Khatyrka meteorite, a new CV3 carbonaceous chondrite.

48 naturally and was discovered in the Khatyrka meteorite, a recently described CV3 carbonaceous chondri

49 Al71Ni24Fe5, was discovered in the Khatyrka meteorite, a recently described CV3 carbonaceous chondri

50 When combined with data from the martian meteorites, a general model can be constructed that cons

51 c imaging of the Imilac and Esquel pallasite meteorites, a group of meteorites consisting of centimet

52 Among the Almahata Sitta meteorites, a unique trachyandesite lava (with an oxygen

53 over-abundance is a 'late veneer'--a flux of meteorites added to the Earth after core formation as a

54 bled the rapid recovery of the Sutter's Mill meteorite after a rare 4-kiloton of TNT-equivalent aster

55 Carbonate minerals in the Martian meteorite ALH 84001 have been dated to approximately 3.9

56 osition of the carbonate globules in martian meteorite ALH 84001.

57 Martian meteorite ALH84001 (ALH) is the oldest known igneous roc

58 rust--the approximately 4.1 billion-year-old meteorite Allan Hills 84001 (ALH84001).

59 w that remanent magnetization in the eucrite meteorite Allan Hills A81001 formed during cooling on Ve

60 The meteorite also contains heretofore unobserved phases of

61 The discovery of new nucleobase analogs in meteorites also expands the prebiotic molecular inventor

62 es, including a chondrule from the Murchison meteorite and a cometary dust grain (Iris) from NASA's S

63 ponent of the CR2 Grave Nunataks (GRA) 95229 meteorite and found it to be of more primitive compositi

64 ation method has been applied to the Allende meteorite and four powdered standard reference materials

65 dy of ancient solar system materials such as meteorites and comet dust, we can recognize evidence for

66 Given that meteorites and comets have reached the Earth since it fo

67 ns (CAIs) occur in all classes of chondritic meteorites and contain refractory minerals predicted to

68 in the inner Solar System bodies, including meteorites and extra-terrestrial ices, and on the early

69 Since then, the study of martian meteorites and findings from missions have been linked.

70 Lonsdaleite is known on Earth only in meteorites and impact craters, and its presence strongly

71 At this time, meteorites and interplanetary dust particles delivered o

72 are among the oldest known pristine basaltic meteorites and record the earliest stages of planet form

73 Laboratory studies of meteorites and robotic exploration of Mars reveal scant

74 h are commonly the main remanence carrier in meteorites and rocks, can record and retain high-fidelit

75 aterial (like that found in a major class of meteorites and some comet surfaces), whereas the bright

76 with characteristics of martian shergottite meteorites and suggests a dichotomy formation time appro

77 the differences between the compositions of meteorites and surface rocks can be explained by differe

78 rgottites, nakhlaites, chassignites) Martian meteorites and terrestrial atmospheric carbonates.

79 Enstatite meteorites and the Earth were formed from the same isoto

80 itlockite with implications for interpreting meteorites and the need for future sample return.

81 he absence of a firm link between individual meteorites and their asteroidal parent bodies, asteroids

82 Taking into account the old ages of eucrite meteorites and their similarity to Earth's isotopic rati

83 of more primitive composition than in other meteorites and to release abundant free ammonia upon hyd

84 actionated compared to primitive, chondritic meteorites and, by inference, the primordial disk from w

85 d these compounds and others in carbonaceous meteorites and/or as low temperature (laboratory) reacti

86 rocks and impact melts, lunar and asteroidal meteorites, and an ancient martian meteorite record ther

87 consistent with literature data for IVA iron meteorites, and indicating that the metal-silicate diffe

88 ry of organic materials via comets, (micro-) meteorites, and interplanetary dust particles to the pri

89 r data suggest a lithification mechanism for meteorites, and provide a 'speed limit' constraint on ma

90 the interstellar medium, comets, chondritic meteorites, and terrestrial planets; we include an updat

91 f the physics of impacts, space transport of meteorites, and the potentiality of microorganisms to un

92 rgy proton beams in the presence of powdered meteorites, and the products of the catalyzed resulting

93 Organic compounds occur in some chondritic meteorites, and their signatures on solar system bodies

94 s ratio caused by the impact of a chondritic meteorite are indicative of projectile size, if the solu

95 tacama Desert, Chile, and from the Murchison meteorite are successfully analyzed using both technique

96 An impact origin for chondrules implies that meteorites are a byproduct of planet formation rather th

97 Chondritic meteorites are asteroidal fragments that retain records

98 So far, the few nucleobases reported in meteorites are biologically common and lacked the struct

99 Chondritic meteorites are considered the most primitive remnants of

100 lts demonstrate that the purines detected in meteorites are consistent with products of ammonium cyan

101 The great majority of basaltic meteorites are derived from the asteroid 4 Vesta.

102 These meteorites are feldspar-rich, with andesite bulk composi

103 Chondritic meteorites are fragments of asteroids, the building bloc

104 Tiny dust grains extracted from primitive meteorites are identified to have originated in the atmo

105 matter (IOM) isolated from the carbonaceous meteorites are interpreted as a heritage of the interste

106 Chondritic meteorites are made of primitive components that record

107 quilibration and sulphide-rich nature of the meteorites are most consistent with an origin as partial

108 Spacecraft data suggest that martian meteorites are not representative of older, more volumin

109 llection data shows that iron and stony-iron meteorites are significantly under-represented from thes

110 Most Martian meteorites are suggested to have been excavated from 3 t

111 Whereas most martian meteorites are young (< 1.3 Ga), the spread of whole roc

112 prebiotic alternatives (using the Murchison meteorite as a model for pre-biotic plausibility).

113 (again, using the contents of the Murchison meteorite as our estimator).

114 However, taking meteorites as a guide, most models assume that the Earth

115 ntitative imaging of a multidomain Pallasite meteorite at a 10 mum LA-spot size.

116 es of prebiotic appeal and never detected in meteorites before.

117 gh-energy proton) synthesis experiments, and meteorite bodies.

118 gets" for meteorites was offset by declining meteorite bombardment rates.

119 t both observations can be explained if late meteorite bombardment triggered the onset of the current

120 ave benefited from accretion of carbonaceous meteorites both directly with soluble compounds and, for

121 heavy isotopes of Si relative to chondritic meteorites by 50-100 ppm/amu.

122 logs in formic acid extracts of 12 different meteorites by liquid chromatography-mass spectrometry.

123 ough thermal conductivity (for example, iron meteorites) can sink at a rate sufficient to offset the

124 valine enrichments in these two carbonaceous meteorites cannot be the result of interference from oth

125 stribution of chemical elements in primitive meteorites (chondrites), as building blocks of terrestri

126 m Mars, Vesta and primitive undifferentiated meteorites (chondrites).

127 tellar medium (ISM) and also in carbonaceous meteorites (CM) such as Murchison.

128 However, meteorite collection data shows that iron and stony-iron

129 re more ancient than any known sample in our meteorite collection, making them prime candidates for s

130 fragile it was not previously represented in meteorite collections.

131 consistent with howardite-eucrite-diogenite meteorites coming from Vesta.

132 surface reflects the composition of the HED meteorites, confirming the formation of Vesta's crust by

133 However, the history inferred from martian meteorites conflicts with results from recent Mars missi

134 ter-sized mineral carbonates in the ALH84001 meteorite; consequently, the identification of Martian p

135 and Esquel pallasite meteorites, a group of meteorites consisting of centimetre-sized metallic and s

136 Meteorites contain a wide range of oxygen isotopic compo

137 Ten of the meteorites contain abiotic macromolecular carbon (MMC) p

138 Carbonaceous meteorites contain clues to prebiotic chemistry because

139 The Murchison and Lonewolf Nunataks 94102 meteorites contained a diverse suite of nucleobases, whi

140 The Khatyrka meteorite contains both icosahedral and decagonal quasic

141 found with chiral excesses, suggesting that meteorites could have contributed to the origin of homoc

142 Spacecraft and meteorite data now provide a global view of the chemistr

143 Carbonaceous meteorites deliver a variety of organic compounds to Ear

144 ents on iron meteorites, we demonstrate that meteorites derive from two genetically distinct nebular

145 Analyses of the meteorite diastereomeric amino acids alloisoleucine and

146 uminum-rich inclusions (CAIs) of the Allende meteorite display variable 238U/235U ratios, ranging bet

147 ion was chondritic (consistent with IAB iron meteorites, Earth, Moon, and Mars).

148 or the most primitive unaltered Antarctic CR meteorites EET 92042 and QUE 99177.

149 ccan eruptions began, continuing through the meteorite event.

150 extinction at this site to both volcanic and meteorite events via climate change.

151 Meteorites exposed to high pressures and temperatures du

152 e we show that the Tissint meteorite, a 2011 meteorite fall, contains virtually all the high-pressure

153 is a potentially initiating step in nebular meteorite formation, which would be capable of producing

154 ers of magnitude slower than that of similar meteorites found in Antarctica where the slowest rates a

155 The meteorites found on Earth today apparently do not give a

156 h along the approach trajectory recovered 47 meteorites, fragments of a single body named Almahata Si

157 oluble organic composition of a carbonaceous meteorite from Antarctica that was collected and stored

158 red the crystallization and ejection ages of meteorites from a Martian volcano and find that its grow

159 Instead, the sample resembles chondritic meteorites from the asteroid belt, composed mostly of in

160 newly discovered, paired and differentiated meteorites Graves Nunatak (GRA) 06128 and GRA 06129.

161 ow-extinct (182)Hf, among five magmatic iron meteorite groups.

162 and (33)S enrichments in other magmatic iron meteorite groups.

163 graphy and variability in shock level across meteorite groups.

164 , the origin and formation of nucleobases in meteorites has been debated for over 50 y.

165 he anhydrous nature of merrillite in Martian meteorites has been interpreted as evidence of water-lim

166 se feldspar-rich mesostasis in the Lafayette meteorite have been replaced by carbonate.

167 show that the Earth, the Moon and enstatite meteorites have almost indistinguishable isotopic compos

168 Achondrite meteorites have anomalous enrichments in (33)S, relative

169 es are essential for life as we know it, and meteorites have been delivering them to the Earth since

170 0 Myr-old limestone >100 fossil L-chondritic meteorites have been recovered, representing the markedl

171 direct samples is the shock compression all meteorites have experienced, which can alter meteorite m

172 Most Martian meteorites have relatively young crystallization ages (1

173 the most commonly falling ordinary chondrite meteorites), however, are seen among small bodies the or

174 esolving the timing of crustal processes and meteorite impact events is central to understanding the

175 and a second, smaller warming at the time of meteorite impact.

176 Previous shock experiments demonstrated that meteorite impacts on ancient oceans would have provided

177 more than half of the distinct known Martian meteorites, including 30 shergottites (28 plus 2 pairs,

178 lite by shock-compression levels relevant to meteorites, including Martian meteorites.

179 relative to other asteroids and carbonaceous meteorites, indicate that the phyllosilicates were forme

180 The composition of the Sutter's Mill meteorite insoluble organic material was studied both in

181 Primitive meteorites, interplanetary dust particles, and comets co

182 any different exogenous materials, including meteorites, interplanetary dust particles, and interstel

183 We use the oxidation of iron in stony meteorites investigated by the Mars Exploration Rover Op

184 ts, are commensurable with those observed in meteorite IOM.

185 ether the igneous histor y inferred from the meteorites is applicable to Mars as a whole.

186 the compositions of the Earth and chondritic meteorites is at the center of many important debates.

187 of bulk silicate Earth relative to primitive meteorites is consistent with the depletion of lithophil

188 ty and complexity of organic matter found in meteorites is rapidly expanding our knowledge and unders

189 emerged very quickly after the deposition of meteorites (less than a few years).

190 composition Al(63)Cu(24)Fe(13), is part of a meteorite, likely formed in the early solar system about

191 lved anomalous (33)S depletions in IIIF iron meteorites (<-0.02 per mil), and (33)S enrichments in ot

192 tanding the origin of pallasites, stony-iron meteorites made mainly of olivine crystals and FeNi meta

193 osition of formamide ices mixed with an FeNi meteorite material treated with laser-induced dielectric

194 of and reactions between the alloys and the meteorite matrix.

195 stallize the high-pressure phases in shocked meteorites may correspond to shock pressure durations ac

196 Carbon-rich meteorites may have been important sources of organic co

197 The organic matter in meteorites might have formed in the interstellar medium

198 and their relation to thermal processing in meteorites might shed new light on our understanding of

199 meteorites have experienced, which can alter meteorite mineralogy.

200 hyl amino acid isovaline was found in the CM meteorite Murchison (L(ee) = 18.5 +/- 2.6%) and the CI m

201 with FTIR analyses for FAN clasts from lunar meteorite Northwest Africa (NWA) 2995.

202 We report data on the martian meteorite Northwest Africa (NWA) 7034, which shares some

203 Here we show that the meteorite Northwest Africa (NWA) 7533 (paired with meteo

204 ite Northwest Africa (NWA) 7533 (paired with meteorite NWA 7034) is a polymict breccia consisting of

205 different aliquots of the Gibeon (IVA) iron meteorite obtained over a period of 6 months show identi

206 is of the organic composition of selected CR meteorites of different petrographic classification and

207 were compared with those obtained for other meteorites of diverse classifications (Murray, GRA 95229

208 unds were found to be present in a set of 61 meteorites of diverse petrological classes.

209 Some meteorites of the carbonaceous chondritic type deliver u

210 The carbonaceous meteorites of the Renazzo-type family (CR) have recently

211 ochemical characteristics with known martian meteorites of the SNC (i.e., shergottite, nakhlite, and

212 Evidence of (176)Hf excess in select meteorites older than 4556Ma was suggested to be caused

213 ally lower than typical impact velocities of meteorites on the early Earth.

214 ate large numbers of englacially transported meteorites onto their surface.

215 s mantle and show it to be consistent with a meteorite or fractionated solar nebula source.

216 terials, perhaps akin to enstatite chondrite meteorites or anhydrous cometary dust particles.

217 tation of derived building blocks of life by meteorites or comets to planet Earth are discussed in th

218 mpacting at the sea surface, such as falling meteorites, or the missing Malaysian Aeroplane MH370.

219 Murchison (L(ee) = 18.5 +/- 2.6%) and the CI meteorite Orgueil (L(ee) = 15.2 +/- 4.0%).

220 The findings appear to trace CR2 meteorites' origin to cosmochemical regimes where ammoni

221 Recently one anomalous meteorite, Osterplana 065 (Ost 65), was found in the sam

222 ino acids of extraterrestrial origin in many meteorites over the last 50 years have revolutionized th

223 rely match laboratory reflectance spectra of meteorites owing to a 'space weathering' process that ra

224 Understanding core formation in meteorite parent bodies is critical for constraining the

225 tracted interval of core formation, the iron meteorite parent bodies probably accreted concurrently ~

226 an extended aqueous alteration phase on the meteorite parent bodies.

227 Their number matches the known distinct meteorite parent bodies.

228 of carbon speciation at a molecular level in meteorite parent bodies.

229 Because the meteorite parent body would likely be classified as a V-

230 la, but was almost certainly modified in the meteorites' parent bodies.

231 Prior to becoming chondritic meteorites, primordial solids were a poorly consolidated

232 This had tremendous consequences for the meteorite production and cratering rate during several m

233 High-pressure minerals in meteorites provide clues for the impact processes that e

234 Basaltic meteorites provide evidence that, like the terrestrial p

235 We will also discuss the unique window that meteorites provide into the chemistry that preceded life

236 The nonracemic amino acids of meteorites provide the only natural example of molecular

237 The geochemistry of Martian meteorites provides a wealth of information about the so

238 One complication of using meteorites rather than direct samples is the shock compr

239 for our earlier conclusion that the Khatyrka meteorite reached heterogeneous high temperatures [1100

240 steroidal meteorites, and an ancient martian meteorite record thermal metamorphic events with ages th

241 ay explain several observed anomalies in the meteorite record: a near absence of detectable (no extre

242 The combined asteroid and meteorite reflectance spectra identify the asteroid as F

243 on is the largest enantiomeric excess in any meteorite reported to date, and the Orgueil measurement

244 Meteorites represent the only samples available for stud

245 Here we show that some Martian meteorites, representing basic igneous rocks, liberate a

246 Finally, we will address the future of meteorite research, including asteroid sample return mis

247 med on mixtures of terrestrial standards and meteorite samples demonstrate that the method is accurat

248 memory of events pre-dating this cataclysmic meteorite shower.

249 Analysis of one of these meteorites shows it to be an achondrite, a polymict urei

250 reported Pb-Pb dates of the basaltic angrite meteorites, some of which have been used extensively as

251 Although the meteorite source locations are unknown, impact ejection

252 cal Raman imaging spectroscopy on 11 martian meteorites, spanning about 4.2 billion years of martian

253 hese small areas of glacial ice are known as meteorite stranding zones, where upward-flowing ice comb

254 n the modern atmosphere and those of martian meteorites such as ALH 84001 implies that the martian re

255 rocarbons (PAHs) as detected in carbonaceous meteorites such as in Murchison.

256 Palaeomagnetic measurements of meteorites suggest that, shortly after the birth of the

257 to the abundances found in some carbonaceous meteorites, suggesting that H(2)S may have played an imp

258 ever, recent research on apatite in the same meteorites suggests higher water content in melts.

259 alkyl amino acids found in altered CI and CM meteorites suggests that amino acids delivered by astero

260 Meteorite sulfur data are discussed in light of the pres

261 The recovered meteorites survived a record high-speed entry of 28.6 ki

262 The meteorites tested were representative of the four major

263 y differentiated object like an Ir-poor iron meteorite that is unlikely to result in an airburst or t

264 ali elements) relative to CI chondrites, the meteorites that compositionally most closely resemble th

265 Carbonaceous chondrites are asteroidal meteorites that contain abundant organic materials.

266 Angrites are rare meteorites that crystallized only a few million years af

267 more importantly, in comets and in primitive meteorites that have most probably seeded the Earth with

268 nalyses of howardite-eucrite-diogenite (HED) meteorites that indicate a differentiated parent body.

269 re we report isotopic analyses of 40 Martian meteorites that represent more than half of the distinct

270 cosmogenic exposure dating of six nakhlites, meteorites that were ejected from Mars by a single impac

271 the first documented example of an 'extinct' meteorite, that is, a meteorite type that does not fall

272 -rich spherules, dominate the most primitive meteorites, the chondrites.

273 ases in shock-melt veins in strongly shocked meteorites, the growth of high-pressure phases from the

274 The minerals within meteorites therefore hold the key to addressing numerous

275 , representing the markedly enhanced flux of meteorites to Earth following the breakup of the L-chond

276 oils from the Moon or that presently fall as meteorites to Earth.

277 ave been frustrated by the ready exposure of meteorites to terrestrial contaminants and the ubiquitou

278 d, which range from instrumental analysis of meteorites to theoretical-computational and astronomical

279 This ties the sources of Martian meteorites to those of the surface rocks through an earl

280 xample of an 'extinct' meteorite, that is, a meteorite type that does not fall on Earth today because

281 ls outside all fields encompassing the known meteorite types.

282 ype asteroid, V-type precursors for basaltic meteorites unrelated to Vesta may reside in the inner ma

283 his increasing availability of "targets" for meteorites was offset by declining meteorite bombardment

284 um and tungsten isotope measurements on iron meteorites, we demonstrate that meteorites derive from t

285 o ancient impact heating signatures in stony meteorites, we infer that the Moon formed ~4.47 billion

286 In meteorites, we observe many as part of three newly repor

287 In multiple carbonaceous meteorites, we show that both rare and common sugar mono

288 livine-bearing chondrules from the Semarkona meteorite were magnetized in a nebular field of 54 +/- 2

289 found in CI-, CM-, and CR-type carbonaceous meteorites were investigated by using liquid chromatogra

290 daleite, was discovered in the Canyon Diablo meteorite where its formation was attributed to the extr

291 arbonaceous chondrites such as the Murchison meteorite, which landed in Australia in 1969, brought so

292 m the SNC (shergottite-nakhlite-chassignite) meteorites, which are genetically related igneous rocks

293 urements of Cr stable isotopes in a range of meteorites, which deviate by up to ~0.4 per mil from tho

294 omposition of the mineral apatite in eucrite meteorites, whose parent body is the main-belt asteroid

295 We show that meteorites with a high-enough thermal conductivity (for

296 measure the W isotopic compositions of iron meteorites with a precision of better than +/-0.1 epsilo

297 es of the ages and compositions of primitive meteorites with compositions similar to the Sun have hel

298 The presence of igneous sulphides in Martian meteorites with sulphur isotope signatures indicative of

299 agnitude more indigenous water than most SNC meteorites, with up to 6000 parts per million extraterre

300 y bombardment by extraterrestrial impactors, meteorites would have provided reactive P in the form of