ライフサイエンスコーパス: meteorite

1 ent Earth, Mars, and the early solar system (meteorites).

2 known natural quasicrystals, in the Khatyrka meteorite.

3 olcanic province and impact of the Chicxulub meteorite.

4 measurements conducted on an iron-containing meteorite.

5 bide grains extracted from the Murchison CM2 meteorite.

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

7 iscovery of trapped atmospheric gases in one meteorite.

8 e a natural shock that affected the Khatyrka meteorite.

9 in aqueously altered carbonaceous chondrite meteorites.

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

11 c matter found in the carbonaceous chondrite meteorites.

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

13 t productive regions on Earth for collecting meteorites.

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

15 , previously molten, spherules found in most meteorites.

16 em from the recognition of numerous basaltic meteorites.

17 scientific value as archives of old ice and meteorites.

18 it marked compositional differences from the meteorites.

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

20 ted in isolated occurrences in other Martian meteorites.

21 Gusev crater on Mars and of martian basaltic meteorites.

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

23 the Vestoids and howardite-eucrite-diogenite meteorites.

24 been determined to be indigenous to numerous meteorites.

25 asaltic howardite-eucrite-diogenite class of meteorites.

26 f anhydrous phases in carbonaceous chondrite meteorites.

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

28 oposed experimental protocol and its use for meteorites.

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

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

31 y system in shergottite-nakhlite-chassignite meteorites.

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

33 containing material comparable to chondritic meteorites.

34 aracteristic of apatite in igneous rocks and meteorites.

35 of the difference in colour of asteroids and meteorites.

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

37 r shock-metamorphosed carbonaceous chondrite meteorites.

38 nguished from most of the OM in carbonaceous meteorites.

39 abundance and species of cyanide present in meteorites.

40 ites, breccias, mineral separates, and lunar meteorites.

41 ls relevant to meteorites, including Martian meteorites.

42 heir higher abundance in thermally processed meteorites.

43 avier magnesium compositions than chondritic meteorites.

44 tic nucleobases along with vitamins found in meteorites.

45 t was isotopically most similar to enstatite meteorites.

46 Laboratory experiments on centimetre-scale meteorites(3) have been extrapolated and buttressed with

47 ved in high-temperature condensates found in meteorites(5).

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

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

50 similar to the previously reported Khatyrka meteorite - a CV chondrite containing near-identical all

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

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

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

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

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

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

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

58 he systems formed, which is analogous to how meteorite abundances inform our understanding of the ear

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

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

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

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

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

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

65 -billion-year-old (Ga) carbonates in Martian meteorite, Allan Hills 84001, preserve indigenous nitrog

66 The meteorite also contains heretofore unobserved phases of

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

68 the methane contents of a variety of Martian meteorites, analogue terrestrial basalts and analogue te

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

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

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

72 s to the degree of aqueous alteration of the meteorite and indicates that parent body processing infl

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

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

75 ata for H and Cl in apatite from three lunar meteorites and discuss possible mechanisms for Cl isotop

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

96 Such meteorites are altered by ejection from their parent bod

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 However, meteorites are chemically inhomogeneous, and superconduc

100 Chondritic meteorites are composed of primitive components formed d

101 Chondritic meteorites are considered the most primitive remnants of

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

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

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

109 Calcium-aluminum-rich inclusions (CAIs) in meteorites are the first solids to have formed in the So

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

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

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

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

114 de the next step towards an understanding of meteorite biogeochemistry.

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

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

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

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

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

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

121 Meteorites can contain a wide range of material phases d

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

123 Studying them and their samples, including meteorites, can help us to learn how the Earth was made

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

125 Among the primitive meteorite classes, Enstatite Chondrites (EC) are believe

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

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

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

129 ositions of amino acids and polyols found in meteorites compared to terrestrial biology and propose a

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

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

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

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

134 Meteorites contain a wide range of oxygen isotopic compo

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

136 Carbonaceous meteorites contain clues to prebiotic chemistry because

137 We show that EC meteorites contain sufficient hydrogen to have delivered

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

139 The Khatyrka meteorite contains both icosahedral and decagonal quasic

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

141 more quinones in extracts from carbonaceous meteorites could serve as coupling agents and that subst

142 Carbonaceous meteorites deliver a variety of organic compounds to Ear

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

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

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

146 ccan eruptions began, continuing through the meteorite event.

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

148 Meteorites exposed to high pressures and temperatures du

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

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

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

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

153 erials, analogous to thermally metamorphosed meteorites found on Earth.

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

155 ginating from the metallic Ni degrees of the meteorite grains and leading to released soluble Ni(2+).

156 at of the modern mantle(12), or of any known meteorite group(5).

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

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

159 graphy and variability in shock level across meteorite groups.

160 oscale resolution ultrastructural studies of meteorite grown M. sedula coupled to electron energy los

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

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

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

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

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

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

167 0 Myr-old limestone >100 fossil L-chondritic meteorites have been recovered, representing the markedl

168 ary rocks and laboratory analyses of Martian meteorites have both reported plausible indigenous organ

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

170 Most Martian meteorites have relatively young crystallization ages (1

171 However, studies of primitive meteorites have revealed they contain extraterrestrial a

172 Enstatite chondrite (EC) meteorites have similar isotopic composition to terrestr

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 proximal effects of the largest known young meteorite impact on Earth have eluded discovery for near

176 ablishes Yarrabubba as the oldest recognised meteorite impact structure on Earth, extending the terre

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

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

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

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

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

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

183 Primitive meteorites, interplanetary dust particles, and comets co

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

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

186 The origin of diamonds in ureilite meteorites is a timely topic in planetary geology as rec

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

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

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

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

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

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

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

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

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

196 rals, unravel microbial fingerprints left on meteorite material, and provide the next step towards an

197 points to the redox processing of Fe-bearing meteorite material.

198 sized diffuse particles dispersed within the meteorite matrix.

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

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

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

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

203 meteorites have experienced, which can alter meteorite mineralogy.

204 . sedula to perform the biotransformation of meteorite minerals, unravel microbial fingerprints left

205 ntification of superconducting phases in two meteorites, Mundrabilla, a group IAB iron meteorite [R.

206 , we provide our observations on a microbial-meteorite nanoscale interface of the metal respiring the

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

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

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

210 M. sedula colonizes the stony meteorite Northwest Africa 1172 (NWA 1172; an H5 ordinar

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

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

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

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

215 Some meteorites of the carbonaceous chondritic type deliver u

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

231 Their number matches the known distinct meteorite parent bodies.

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

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

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

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

236 osition of asteroids and their connection to meteorites provide insight into geologic processes that

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

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

239 wo meteorites, Mundrabilla, a group IAB iron meteorite [R.

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

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

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

243 Exploration of microbial-meteorite redox interactions highlights the possibility

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 o alleviate this difficulty, we have studied meteorite samples with the ultrasensitive magnetic field

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

249 Analysis of the Lewis Cliff 85311 meteorite shows that its releasable cyanide is primarily

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 ses that can be precisely studied in Martian meteorites such as NWA 7533/7034.

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

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

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

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 Diogenites are a group of meteorites that are derived from the interior of the lar

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

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

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

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

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

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

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

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

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

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

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

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

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

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

279 ls outside all fields encompassing the known meteorite types.

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

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

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

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

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

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

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

287 The Zag meteorite which is a thermally-metamorphosed H ordinary

288 sted to be an unbrecciated noritic diogenite meteorite, which is confirmed by our oxygen and chromium

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

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

291 ndrules, the main constituents of chondritic meteorites, which in turn are primitive fragments of pla

292 177)Hf composition within error of chondrite meteorites, which include the likely parent bodies of Ea

293 ed materials, such as carbonaceous chondrite meteorites, which originated in the outer Solar System w

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

297 rom icy cometary bodies to fully melted iron meteorites with isotopic affinities to carbonaceous chon

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