ライフサイエンスコーパス: crater

1 ed the South Pole/Aitken basin or asymmetric cratering).

2 t within a distance of up to 180 km from the crater.

3 cient volcanic hydrothermal setting in Gusev crater.

4 and drilled sedimentary deposits within Gale crater.

5 s identified similar deposits within Occator crater.

6 ble gases in a mudstone on the floor of Gale Crater.

7 in the subsurface structure of the Chicxulub crater.

8 infilling events that occurred within the VK crater.

9 il from the Rocknest aeolian bedform in Gale crater.

10 he 35-million-year-old Chesapeake Bay impact crater.

11 phur, chlorine and zinc) to soils from Gusev crater.

12 he deposit, including outliers close to Gale crater.

13 reflect the presence of a buried ~17 x 13-km crater.

14 ight percent) in the Columbia Hills of Gusev crater.

15 c matter ejected during the formation of the crater.

16 cceleration as the rover climbs through Gale crater.

17 rmation, and thermal anomalies in the summit crater.

18 kilometers close to the 50-kilometer Ernutet crater.

19 nside the 150-kilometer-diameter Gale impact crater.

20 environment fed by rivers draining into the crater.

21 stribution, and an apparent absence of large craters.

22 ould have an icy crust with few or no impact craters.

23 d monitor the morphology of resulting impact craters.

24 crater morphology as that of asteroid impact craters.

25 gs, such as near volcanic activity or impact craters.

26 s, crater central peaks, and numerous simple craters.

27 een excavated from 3 to 7 km diameter impact craters.

28 issue and estimate the depth of the ablation craters.

29 existence of crosscut small-diameter impact craters.

30 dances across the entire surface, and impact craters.

31 hereas the farside is mountainous and deeply cratered.

32 surface cannot solely be explained by impact cratering.

33 The resulting conical crater (0.6 mum x 130 nm ) morphology in a Au-coated gla

34 ly triggered by bolide impacts, resulting in craters ~30 km in diameter and occurring perhaps a few m

35 The simulated impact produced a transient crater, ~390 kilometers in diameter, that was not mainta

36 und methane concentrations found in the Gale crater(4) would require an unknown process that can rapi

37 tunity has investigated the rim of Endeavour Crater, a large ancient impact crater on Mars.

38 masked and fades into the background as the craters age.

39 l tens of millions of years, consistent with crater ages.

40 Surface rocks from the Gusev crater analysed by the Spirit rover are much older (abou

41 ced inward from the wall, infilling both the crater and an internal lake basin to a thickness of at l

42 curred planetwide some of which entered Gale crater and combined with water roaring down from Mt.

43 urface, it imaged a 25- to-30-meter-diameter crater and evidence of a high-angle ballistic ejecta plu

44 The crater and proximal effects of the largest known young m

45 is constrained by the formation of Victoria crater and their minimum age by erosion of the meteorite

46 temporal dataset, we detected 222 new impact craters and found 33 per cent more craters (with diamete

47 ndom creases and craters to aligned creases, craters and lines, and the size of the pattern from mill

48 However, although studies of existing craters and returned samples offer insight into the proc

49 tratigraphic relationship between identified craters and the redder material indicates that surface r

50 es include both those associated with impact craters and those that do not appear to have any correla

51 quency and associated water volumes in Istok crater, and show that debris flows occurred at Earth-lik

52 ce, lack of superposed large-diameter impact craters, and the existence of crosscut small-diameter im

53 These dark materials, often associated with craters, appear in ejecta and crater walls, and their py

54 e deposits in the ocean sediment at the bomb crater are widespread and high levels of contamination r

55 e heavily cratered, but the largest expected craters are absent.

56 have favored relaxation, yet large unrelaxed craters are also present.

57 Superposed impact craters are common and eolian bedforms are sparse.

58 Impact craters are the most obvious indication of asteroid impa

59 products from a known cosmic impact (Meteor Crater, Arizona) and from the 1945 Trinity nuclear airbu

60 Rimmed grooves, lineations and elongate craters around Mare Imbrium shape much of the nearside M

61 ciding with a long-lived lake system in Gale Crater at approximately 3.5 Ga.

62 soil along the rim of a 450-m diameter fresh crater at the Chang'e-3 (CE-3) landing site, investigate

63 h distinct material exposed at several fresh craters becomes gradually masked and fades into the back

64 s within both Pu'u O'o Vent and Halema'uma'u Crater began to drain and the summit caldera began to de

65 esting that the deficit of large terrestrial craters between 300 million and 650 million years ago re

66 Based on stratigraphy near the crater, between 7.5 x 10(14) and 2.5 x 10(15) g of black

67 In general, the wedge-crater beveling protocol is shown to provide a powerful

68 ed between 90 and 300 K using a unique wedge-crater beveling strategy that allows these parameters to

69 Surface roughness at the SIMS crater bottoms is characterized by AFM as a function of

70 Parts of Ceres' surface are heavily cratered, but the largest expected craters are absent.

71 rounding terrain and the interiors of nearby craters, but not as bright as the interior walls.

72 The dwarf planet is dominated by numerous craters, but other features are also common.

73 nergy and length difference, granular impact cratering by liquid drops follows the same energy scalin

74 l explored, our knowledge on granular impact cratering by liquid drops is still very limited.

75 Although the mechanism of granular impact cratering by solid spheres is well explored, our knowled

76 rmation about an impact even when the source crater cannot be found.

77 structures, volcanic landforms, basin rings, crater central peaks, and numerous simple craters.

78 The host rocks, which are associated with crater central peaks, peak rings, floors, and walls, are

79 The 7.5-km wide Lockne crater, central Sweden, is known to be a member of this

80 tly imprint Phobos with linear, low-velocity crater chains (catenae) that match the geometry and morp

81 hobos is criss-crossed by linear grooves and crater chains whose origin is unexplained.

82 Multiring basins, large impact craters characterized by multiple concentric topographic

83 Applying a recent model for early lunar crater chronology and an updated dynamical extrapolation

84 ributions of volcanic fissures/feeder-dykes, crater cones, dyke thicknesses, and lava flows to estima

85 ates reproduce impact spherule bed and lunar crater constraints.

86 y lead to an accretionary pile rather than a crater, contributing a hemispheric layer of extent and t

87 By impact crater counting chronology we estimated the age of the s

88 Crater counts and radiometric ages from returned samples

89 Crater densities on Nix and Hydra imply surface ages of

90 Although their size and impact crater density indicate continued activity over billions

91 ensitivity of the primary ion was its impact crater depth or the amount of surface erosion.

92 eters related to surface sensitivity (impact crater depth, implantation depth, and molecular escape d

93 oms is characterized by AFM as a function of crater depth.

94 The chronologic record of lunar cratering determined from the returned samples underpins

95 aster array (50 mum pitch distance, ablation crater diameter of approximately 20 mum).

96 a heavily cratered surface, a heterogeneous crater distribution, and an apparent absence of large cr

97 This newly discovered crater doublet provides a unique reference for impacts b

98 widely perceived as a Middle Miocene impact crater doublet.

99 e, we show a significant depletion of cerean craters down to 100-150 km in diameter.

100 The main displacement mechanism is along the crater edge.

101 iments and impact models, however, show that crater ejecta velocities are typically greater than seve

102 sed, with erosion thought to eliminate older craters, even on stable terrains.

103 layers created by Chicxulub-sized or larger cratering events4.

104 veal that many bright deposits within impact craters exhibit fresh-appearing, irregular, shallow, rim

105 Numerous craters exhibit polygonal shapes, terraces, flowlike fea

106 nd velocities of the ejecta from this unique cratering experiment are better constrained.

107 The relatively brighter crater floor is most simply explained by decreased space

108 Vinalia Faculae, in the crater floor, were sourced from the laterally extensive

109 rted by geomorphologic features such as flat crater floors with pits, lobate flows of materials, and

110 ed samples offer insight into the process of crater formation and the past cratering rate, questions

111 rmed from the dynamic uplift of rocks during crater formation.

112 The crater formed in the gravity-dominated regime; in other

113 ttle floor deposition has occurred since the crater formed more than three billion years ago.

114 e 0.7-km diameter, contemporaneous, Malingen crater, formed by the impact of a binary, presumably 'ru

115 ted to have been excavated from depth by the crater-forming process.

116 xide, made in the martian atmosphere at Gale Crater from the Curiosity rover using the Sample Analysi

117 derived from topography maps of single pulse craters from atomic force microscopy.

118 he gravity-dominated regime; in other words, crater growth was limited by gravity not surface strengt

119 ver, Ceres' surface appears devoid of impact craters > approximately 280 km.

120 he Moon, we produced a catalog of all impact craters >/=20 kilometers in diameter on the lunar surfac

121 mordial main belt of asteroids predict 10-15 craters >400 km should have formed on Ceres, the largest

122 eroid impact that formed the 66 Ma Chicxulub crater had a profound and catastrophic effect on Earth's

123 Laboratory in the sedimentary record of Gale Crater has reinvigorated the search for evidence of mart

124 icate that a significant population of large craters has been obliterated, implying that long-wavelen

125 for the origin of increased salinity in the crater have included evaporite dissolution, osmosis and

126 ters over gently sloping plains and boundary cratered highlands, as well as backwash channels where w

127 is an intensely eroded deposit north of the cratered highlands.

128 These new insights into crater hosted gas accumulation and microbial activity ha

129 at Gusev Crater, Meridiani Planum, and Gale Crater implies locally sourced, globally similar basalti

130 InSight landed in a degraded impact crater in Elysium Planitia on a smooth sandy, granule- a

131 s, and highlight the possible role of impact cratering in modifying Earth's climate.

132 matter and indicate that geologic detectors (craters in peat bogs) and space-based detectors (satelli

133 apping of Mars suggest derivation from small craters in terrains of Amazonian to Hesperian age.

134 The post-Rheasilvia craters in the north-polar region on Vesta could be the

135 r CheMin X-ray diffraction results from Gale crater indicate that the crystallinity of Martian sedime

136 ize distributions proximal and distal to the crater indicate the ejected carbon was dispersed globall

137 Age estimates from the craters indicate a resurfacing age of [Formula: see text

138 Craters indicate that the time scale of these color chan

139 The density of impact craters indicates the surface dates from the formation o

140 These surfaces exhibit few fresh craters, indicating geologically recent wind erosion.

141 Crater interior plains, possibly lavas, share the chaoti

142 t simulations indicate that a 70 km-diameter crater into a continental glacier could release between

143 The density of the sedimentary rocks in Gale crater is 1680 +/- 180 kilograms per cubic meter.

144 Shackleton crater is nearly coincident with the Moon's south pole.

145 indicate that groundwater in the Chesapeake crater is remnant Early Cretaceous North Atlantic (ECNA)

146 The morphology of some impact craters is consistent with ice in the subsurface, which

147 The overall scarcity of recognizable large craters is incompatible with collisional models, even in

148 We find that the roughness in SIMS craters is limited to approximately 1.5 nm, which is muc

149 f impact origin of a 200 km suspected impact crater Kotuykanskaya near Popigai, Siberia, Russia.

150 on a sympatrically diverging species pair of crater lake cichlid fishes.

151 raphically isolated radiations of Nicaraguan crater lake cichlid fishes.

152 Neotropical crater lake cichlids are ideal models to study evolution

153 e past 25 000 years from Lake Challa, a deep crater lake in equatorial East Africa.

154 in a small (700 meters in diameter) isolated crater lake in Tanzania.

155 IL, Mingo, MO, Phoenix, AZ, San Gabriel, CA, Crater Lake National Park, OR, and Spokane, WA.

156 mean, 22 +/- 9.5 minutes) to a high-altitude crater lake.

157 Until recently, Uganda's crater lakes were considered schistosomiasis free due to

158 ites of acid mine drainage, and acid-sulfate crater lakes, may be ideal hunting grounds for finding m

159 e only comparable to those found in volcanic crater lakes.

160 l radiation events within and among isolated crater lakes.

161 ers, pitted plains, and inverted fluvial and crater landforms.

162 by the 1974 Mariner 10 flybys show extensive cratered landscapes degraded into vast knob fields, know

163 The oldest terrains of Mars are cratered landscapes, in which extensive valleys and basi

164 These terrains have a lower density of craters less than 100 km in diameter than does the Moon,

165 ms like a liquid yet it preserves a circular crater like a solid.

166 A unique three-dimensional, crater-like microstructure was also observed in authenti

167 For example, we show that catena-producing craters likely formed in the gravity regime, providing c

168 Several irregularly shaped craters located within Arabia Terra, Mars, represent a n

169 the upwelling hydrothermal system below the craters, magma intrusion pathways and inherited faults.

170 ) is similar to pyroclastic rocks from Gusev crater, Mars, and consistent with widespread distributio

171 d mudstone (Buckskin) at Marias Pass in Gale crater, Mars, by the Chemistry and Mineralogy X-ray diff

172 imentologic evidence of giant floods in Gale crater, Mars, during the Noachian Period.

173 ugh organic matter has been detected at Gale Crater, Mars, its concentrations are lower than expected

174 re water within lacustrine sediments of Gale Crater, Mars, using smectite interlayer compositions.

175 riosity rover at Yellowknife Bay within Gale crater, Mars.

176 jecta velocity field and knowledge of source crater material properties.

177 ts for Rhodamine B show that very consistent craters may be generated.

178 Fractured rocks of impact craters may be suitable hosts for deep microbial communi

179 oils and aeolian materials analyzed at Gusev Crater, Meridiani Planum, and Gale Crater implies locall

180 Crater morphology and simple-to-complex crater transitio

181 same energy scaling and reproduces the same crater morphology as that of asteroid impact craters.

182 the uppermost layered materials on the Gale crater mound.

183 was recently found to have two large impact craters near its south pole, exposing subsurface materia

184 mission signature 90 seconds after the Lunar Crater Observation and Sensing Satellite (LCROSS) Centau

185 The Lunar CRater Observation and Sensing Satellite (LCROSS) missio

186 The Lunar Crater Observation and Sensing Satellite (LCROSS) missio

187 On 9 October 2009, the Lunar Crater Observation and Sensing Satellite (LCROSS) sent a

188 The Lunar Crater Observation and Sensing Satellite (LCROSS) struck

189 report an analysis of the size and depth of craters observed on boulders on the asteroid (101955) Be

190 lar interest is a bright pit on the floor of crater Occator that exhibits probable sublimation of wat

191 Here, we present a study of the largest crater of Europe, the Devonian Siljan structure, showing

192 x explosive episodes from the New South-East Crater of Mt.

193 4 lines of evidence that the 0.79-Ma impact crater of the Australasian tektites lies buried beneath

194 terminal' bombardment that culminated in the cratering of the Moon.

195 e initial detection of RSL candidates in two craters of Mawrth Vallis.

196 ice may be presented in permanently shadowed craters of the Moon.

197 thography to pattern surfaces with nanoscale craters of various aspect ratios and pitches, we show th

198 co - located about 500 km from the Chicxulub crater - offer a unique opportunity to determine an exti

199 The almost complete absence of terrestrial craters older than 650 million years may indicate a mass

200 , including that in the K-T Chicxulub impact crater on Earth.

201 eralogy of certain basaltic rocks from Gusev crater on Mars and of martian basaltic meteorites.

202 The landforms of northern Gale crater on Mars expose thick sequences of sedimentary roc

203 of Endeavour Crater, a large ancient impact crater on Mars.

204 obvious indication of asteroid impacts, but craters on Earth are quickly obscured or destroyed by su

205 hy similar to that observed at similar-sized craters on Earth.

206 around 70 and four Chicxulub-sized or larger craters on the Earth and Moon, respectively, between 1.7

207 We report counts of impact craters on the MFF units that have implications for our

208 Sedimentary rocks at Yellowknife Bay (Gale crater) on Mars include mudstone sampled by the Curiosit

209 SS) sent a kinetic impactor to strike Cabeus crater, on a mission to search for water ice and other v

210 e in Oxo, a 10-kilometer, geologically fresh crater, on five occasions over a period of 1 month.

211 analysis of zircaloy sample while creating a crater only 10 mum in diameter.

212 roids that produced many young lunar basins (craters over 300 kilometres in diameter) has frequently

213 The accumulation of impact craters over time is of fundamental use in evaluating th

214 Impact crater populations on Pluto and Charon are not consisten

215 The characteristics of pre- and postmare crater populations support the hypothesis that there wer

216 The most-densely cratered portion of the highlands reached a state of sat

217 thin an exhumed alluvial fan complex in Gale Crater, presents some of the most compelling evidence ye

218 We also observe a secondary cratering process that we estimate churns the top two ce

219 roughness variations cannot be explained by cratering processes only.

220 e pairs to quantify the contemporary rate of crater production on the Moon, to reveal previously unkn

221 tions still remain about the present rate of crater production, the effect of early-stage jetting dur

222 e processes, viz., LA sampling (via ablation crater profiles [ACP]) and aerosol washout/transfer/ICPM

223 onsequences for the meteorite production and cratering rate during several millions of years followin

224 the process of crater formation and the past cratering rate, questions still remain about the present

225 The terrestrial impact crater record is commonly assumed to be biased, with ero

226 The terrestrial crater record shows similar results, suggesting that the

227 tructure on Earth, extending the terrestrial cratering record back >200 million years.

228 Results show that Vesta's cratering record has a strong north-south dichotomy.

229 ative surface ages from space weathering and cratering records.

230 We present spectra of the Nightingale crater region on near-Earth asteroid Bennu with a distin

231 , a result that reflects the preservation of crater relief in highly fractured crust.

232 well under the ten-million-year upper-limit crater retention age for Sputnik Planum.

233 involved in convection and advection, with a crater retention age no greater than ~10 million years.

234 ater SFD has been used to estimate a surface crater retention age of approximately 1.6 +/- 0.3 Gyr.

235 ruption alone can explain the relatively old crater-retention ages of the equatorial features of Ryug

236 nce Laboratory Mast Camera (Mastcam) in Gale crater reveal isolated outcrops of cemented pebbles (2 t

237 Absolute model ages from impact craters reveal that extrusion of the dome has occurred r

238 ly wet climate that supplied moisture to the crater rim and transported sediment via streams into the

239 e expected antiquity of rocks comprising the crater rim.

240 veins cut sedimentary rocks adjacent to the crater rim.

241 action beneath a sedimentary cap rock at the crater rim.

242 frost containing methane is observed coating crater rims and walls as well as mountain tops, providin

243 include widespread, wind-eroded landscapes, crater rims eroded down by several hundred meters, pitte

244 emplacement mechanism and source of Occator crater's bright faculae.

245 romatic hydrocarbons (PAHs) in the Chicxulub crater sediments and at two deep ocean sites indicate a

246 In addition, the cumulative crater SFD has been used to estimate a surface crater re

247 sample stage designs often lead to variable crater shapes.

248 that have been dismissed as degraded impact craters should be reconsidered as possible volcanic cons

249 presentation of radiation maps of the Bravo crater site.

250 As crater size increases, central peaks transition to peak

251 We characterized PIRL crater size using agar films containing Rhodamine.

252 o result from imprecise determination of the crater size when ablating the glass SRM.

253 degrees C from samples of Hesperian-era Gale crater smectite to determine this isotope ratio.

254 Arrokoth has a lightly cratered, smooth surface with complex geological feature

255 Here we report global crater statistics of Mercury's most heavily cratered ter

256 gh-resolution topography, image analysis and crater statistics, we have dated 35 different surfaces i

257 re of endogenic activity, rather than impact craters such as those on planetary and asteroid surfaces

258 r the brines, based on the chemistry of Gale crater, suggested that the oxidation of reduced sulfur s

259 by the Dawn spacecraft that reveal a heavily cratered surface, a heterogeneous crater distribution, a

260 The ancient cratered terrain of the southern highlands of Mars is th

261 The most heavily cratered terrains on Mercury have been estimated to be a

262 crater statistics of Mercury's most heavily cratered terrains on the entire surface.

263 Vesta's northern heavily cratered terrains retain much of their earliest history.

264 Pluto also has ancient cratered terrains up to ~4 billion years old that are ex

265 water ice, producing haze clouds inside the crater that appear and disappear with a diurnal rhythm.

266 re is no preserved evidence of the transient crater that would reveal the basin's maximum volume, but

267 ad reflectance zones associated with the new craters that we interpret as evidence of a surface-bound

268 n mudstone material, based on data from Gale Crater, that was inoculated and cultured over several mo

269 Under stagnant conditions near the crater, the extent of SO2 oxidation was substantially hi

270 reference sample to check the sample erosion crater, the sample stage movement and memory effects.

271 material ablated from submicrometer diameter craters, the effective lateral resolution is currently l

272 res, and partially or completely bury impact craters, the sizes of which indicate plains thicknesses

273 pattern can be tuned from random creases and craters to aligned creases, craters and lines, and the s

274 stinctive reimpact patterns allow sesquinary craters to be traced back to their source, for the first

275 Crater morphology and simple-to-complex crater transition diameters indicate that the crust of C

276 s farside landing on the floor of Von Karman crater (VK) inside the South Pole-Aitken (SPA).

277 considered to be derived from young, lightly cratered volcanic regions, such as the Tharsis plateau.

278 Degradation of the crater wall and rim probably supplied these sediments, w

279 al phases are possibly sourced from the Gale crater wall/rim/central peak.

280 were etched using He LTP, and the resulting crater walls were depth profiled using time-of-flight se

281 ssociated with craters, appear in ejecta and crater walls, and their pyroxene absorption strengths ar

282 cal observations suggests that the Chicxulub crater was formed by a steeply-inclined (45-60 degrees t

283 ter in lacustrine mudstone sediments at Gale crater was revealed by the Mars Science Laboratory Curio

284 recent aqueous activity in some mid-latitude craters was much more frequent than previously anticipat

285 g a smooth region associated with the Kerwan crater, we determined absolute model ages (AMAs) of 550

286 t Mars instrument suite on Curiosity at Gale crater, we report detection of background levels of atmo

287 Here, impact diamonds from the Popigai crater were characterized with a range of techniques.

288 The deposits in Gale crater were then exhumed, probably by wind-driven erosio

289 Doughnut-shaped craters were formed by single pulse irradiation on the S

290 cks on the rim of the Noachian age Endeavour crater, where orbital spectral reflectance signatures in

291 terrain is associated with numerous martian craters, where pits are thought to form through degassin

292 an ancient, unusually well-preserved simple crater whose interior walls are fresher than its floor a

293 The impact produced an artificial crater with a diameter >10 meters, which has a semicircu

294 ngwoodite grains, we infer an initial impact crater with ~90 km diameter, with a factor of 2 uncertai

295 trast, Bi(5)(+2) primary ions created impact craters with a depth of 1.8 nm in tetraglyme films and w

296 ions, Bi(1)(+) and C(60)(+2), created impact craters with depths of 0.3 and 1.0 nm, respectively, in

297 e quantified by using a method to date lunar craters with diameters greater than 10 kilometers and yo

298 with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta.

299 ew impact craters and found 33 per cent more craters (with diameters of at least ten metres) than pre

300 pressions found in and around several impact craters, with a distinct morphology not observed on othe