ライフサイエンスコーパス: asteroid

1 impact of a binary, presumably 'rubble pile' asteroid.

2 partial melts from a volatile-rich, oxidized asteroid.

3 variations across the surface of this large asteroid.

4 stitute the building blocks of a rubble-pile asteroid.

5 5) Bennu, demonstrating that it is an active asteroid.

6 es, as well as for the development of binary asteroids.

7 nnot be the main source of regolith on small asteroids.

8 of low-perihelion, carbonaceous, near-Earth asteroids.

9 ocess governing regolith generation on small asteroids.

10 contribute to regolith production on larger asteroids.

11 rus associated with tissues from symptomatic asteroids.

12 abundant in symptomatic than in asymptomatic asteroids.

13 itational escape velocity of kilometre-sized asteroids.

14 ent with delivery by comets or volatile-rich asteroids.

15 rs now make up the high-inclination Hungaria asteroids.

16 ons for the geological history of chondritic asteroids.

17 other planets (Venus, Mars, or Mercury) and asteroids.

18 le to dynamos in other bodies, such as large asteroids.

19 but the region is not uniformly filled with asteroids.

20 collisional evolution than typical main-belt asteroids.

21 d that fragments of these bodies survived as asteroids.

22 nning the range seen among similar main-belt asteroids.

23 dies in our solar system such as Mercury and asteroids.

24 Remote observations of the asteroid (1) Ceres from ground- and space-based telescop

25 Carbonaceous (C-type) asteroids(1) are relics of the early Solar System that h

26 Asteroid (101955) Bennu is a dark asteroid on an Earth-c

27 pacecraft recently arrived at the near-Earth asteroid (101955) Bennu, a primitive body that represent

28 During its approach to asteroid (101955) Bennu, NASA's Origins, Spectral Interp

29 depth of craters observed on boulders on the asteroid (101955) Bennu.

30 ges (0.44 to 0.89 micrometers) of near-Earth asteroid (101955) Bennu.

31 craft arrived at the near-Earth carbonaceous asteroid 162173 Ryugu in 2018.

32 The near-Earth carbonaceous asteroid 162173 Ryugu is thought to have been produced f

33 -rotation thermographic images of the C-type asteroid 162173 Ryugu, taken by the thermal infrared ima

34 The near-Earth asteroid 162173 Ryugu, the target of the Hayabusa2 sampl

35 The near-Earth asteroid (162173) Ryugu is thought to be a primitive car

36 For instance, the asteroids (162173) Ryugu and (101955) Bennu have an obla

37 Bennu is a low-albedo B-type asteroid(2) that has been linked to organic-rich hydrate

38 rvations and analysis that demonstrates that asteroid 2015 BZ509 is indeed a retrograde co-orbital as

39 Asteroid 2015 BZ509 was discovered in 2015, but with too

40 Here we report infrared spectra of the asteroid 24 Themis which show that ice and organic compo

41 ion of water ice and organic material on the asteroid 24 Themis, a detection that has been independen

42 (FeS) grains recovered from the regolith of asteroid 25143 Itokawa have lost sulfur during long-term

43 om Apollo lunar samples(6) and images of the asteroid (25143) Itokawa(7).

44 Thirty-five N. cyriacigeorgica, 30 N. asteroides, 26 N. farcinica, 12 N. otitidiscaviarum, and

45 The kilometre-sized main-belt asteroid 288P (300163) showed activity for several month

46 Here we report that the kilometre-sized asteroid (29075) 1950 DA is a rubble pile that is rotati

47 Asteroid (3200) Phaethon is an active near-Earth asteroi

48 The asteroid 4 Vesta was recently found to have two large im

49 teorites, whose parent body is the main-belt asteroid 4 Vesta.

50 of basaltic meteorites are derived from the asteroid 4 Vesta.

51 In contrast to the asteroid (4) Vesta, this strong compensation points to t

52 nducted a successful flyby of the near-Earth asteroid 4179 Toutatis at a closest distance of 770 +/-

53 uous increase in the spin rate of near-Earth asteroid (54509) 2000 PH5 can be attributed to the Yarko

54 otometric observations of a small near-Earth asteroid, (54509) 2000 PH5, acquired over 4 years.

55 Here we report that asteroid, a gene identified in an ethylnitrosourea mutag

56 een in the existence of separate families of asteroids--a family consists of many asteroids with simi

57 lithic clast that was accreted to the parent asteroid after metamorphism.

58 mmon ancestor of echinoids, holothurians and asteroids, although it is not clear if the occurrence of

59 s), have blurred the line between comets and asteroids, although so far neither ice nor organic mater

60 Many decades of asteroid and comet characterization have yielded formati

61 The combined asteroid and meteorite reflectance spectra identify the

62 roid (3200) Phaethon is an active near-Earth asteroid and the parent body of the Geminid Meteor Showe

63 o incomplete differentiation of their parent asteroid and to previously unrecognized diversity of ear

64 for the production and destruction of small asteroids and a contributor to dust in the Sun's zodiaca

65 Random bombardment by comets, asteroids and associated fragments form and alter the lu

66 ectral properties of Ceres relative to other asteroids and carbonaceous meteorites, indicate that the

67 None of the approximately 750,000 known asteroids and comets in the Solar System is thought to h

68 roxy for the early Earth, contains relics of asteroids and comets that have pummeled terrestrial plan

69 ve outer Solar System objects related to icy asteroids and comets underwent a phase of magmatic activ

70 he petrogenetic continuum between comets and asteroids and elevates the astrophysical importance of s

71 s-long puzzle of the difference in colour of asteroids and meteorites.

72 riginate from disrupted rocky bodies such as asteroids and minor planets.

73 Central in this research is the accretion of asteroids and planets from a gas-rich circumstellar disk

74 The composition of asteroids and their connection to meteorites provide ins

75 rocesses can lead to the formation of binary asteroids and to the release of dust, both directly and,

76 e rejuvenation of the surfaces of near-Earth asteroids, and may explain the observed lack of low-peri

77 ch destruction occurs is greater for smaller asteroids, and their temperatures during perihelion pass

78 when samples returned by missions to C-class asteroids are interpreted.

79 ound-based observations have shown that some asteroids are loose collections of rubble rather than so

80 eventually break up, we find that low-albedo asteroids are more likely to be destroyed farther from t

81 These Q-type asteroids are not currently found among asteroids showin

82 Most inner main-belt asteroids are primitive rock and metal bodies in orbit a

83 Asteroids are primitive Solar System bodies that evolve

84 Active asteroids are those that show evidence of ongoing mass l

85 teorites and their asteroidal parent bodies, asteroids are typically characterized only by their ligh

86 ystem bodies, including the Earth, Moon, and asteroids, are depleted in volatile elements relative to

87 d meteorite reflectance spectra identify the asteroid as F class, now firmly linked to dark carbon-ri

88 Ultrasound-Derived Coronary Atheroma Burden (ASTEROID) assessed whether rosuvastatin could regress co

89 is thought to be caused by the impact of an asteroid at Chicxulub, present-day Mexico.

90 the rocky terrestrial planets including the asteroids at 0.39 to 4.2 astronomical units (AU) from th

91 a fragments from that event struck main-belt asteroids at velocities exceeding 10 kilometers per seco

92 Using an asteroid-avoidance game that allows us to study learning

93 trophic disruption of the parent body of the asteroid Baptistina, which we infer was a approximately

94 r than 35 kilometers, supporting the view of asteroids being born big.

95 Most near-Earth objects came from the asteroid belt and drifted via non-gravitational thermal

96 representation of the kind of bodies in the asteroid belt approximately 500 Myr ago.

97 nce of such forces, most objects in the main asteroid belt are expected to be geologically inert.

98 kedly increase estimates for the mass in the asteroid belt before depletion caused by the orbital mig

99 ended and now largely extinct portion of the asteroid belt between 1.7 and 2.1 astronomical units fro

100 arther out in the solar system, not only the asteroid belt but even in the comet accretion region, su

101 growth is stunted, and nothing large in the asteroid belt can accumulate.

102 has been dynamically decoupled from the main asteroid belt for 1.75 +/- 0.75 million years.

103 The asteroids in the main asteroid belt have been discovered to be more compositio

104 t implies that the observed diversity of the asteroid belt is not a direct reflection of the intrinsi

105 The main asteroid belt lies between the orbits of Mars and Jupite

106 large differentiated rocky body in the main asteroid belt that accreted within the first few million

107 et (1) Ceres, the largest object in the main asteroid belt with a mean diameter of about 950 kilometr

108 bution matching those derived from the inner asteroid belt, ancient martian impact basins, and planet

109 cts into dry bodies, ranging out to the main asteroid belt, and icy bodies beyond the belt.

110 ple resembles chondritic meteorites from the asteroid belt, composed mostly of inner solar nebula mat

111 In the asteroid belt, direct evidence of the effects of large c

112 on the surface of the largest object in the asteroid belt, the dwarf planet (1) Ceres, which is thou

113 The main asteroid belt, which inhabits a relatively narrow annulu

114 oid was disrupted by a collision in the Main Asteroid Belt, which spawned fragments into Earth crossi

115 f a population of large proto-planets in the asteroid belt.

116 ystem, including a small Mars and a low-mass asteroid belt.

117 ration of material transported into the main asteroid belt.

118 of the icy bodies may have migrated into the asteroid belt.

119 roke up 160(-20)+30Myr ago in the inner main asteroid belt.

120 s originating in a third reservoir: the main asteroid belt.

121 the Nightingale crater region on near-Earth asteroid Bennu with a distinct infrared absorption aroun

122 It is different from the known asteroid binaries in its combination of wide separation,

123 r-Earth objects and suggests that low-albedo asteroids break up more easily as a result of thermal ef

124 t the core microbiota member Bifidobacterium asteroides, but that exhibited different host ranges at

125 ut are consistent with dynamical ejection of asteroids by the sweeping of gravitational resonances du

126 In a subset of the asteroids called main-belt comets, the sublimation of ex

127 ironment, a natural satellite, or unexpected asteroid characteristics would have had consequences for

128 Telescopic measurements of asteroids' colours rarely match laboratory reflectance s

129 ts that fragments of a large, disintegrating asteroid/comet struck North America, South America, Euro

130 Asteroids, comets and moons are leftovers of planet form

131 Unlike asteroids, comets preserve a nearly pristine record of t

132 rites suggests that amino acids delivered by asteroids, comets, and their fragments would have biased

133 the unofficial species designation Nocardia asteroides complex antimicrobial susceptibility pattern

134 nd expression of this process will vary with asteroid composition and location, influencing how diffe

135 issues that was inoculated into asymptomatic asteroids consistently resulted in SSWD signs whereas an

136 Sunshine et al. reported that certain asteroids contain 30 +/- 10 volume percent calcium- and

137 Impacts of comets or volatile-rich asteroids could have provided both dark and bright depos

138 e report a quantitative comparison of actual asteroid detections and a near-Earth-object model (which

139 Here we report that asteroids displaying unweathered spectra (so-called 'Q-t

140 show, through numerical simulations of large asteroid disruptions, that oblate spheroids, some of whi

141 that the observed distribution of main belt asteroids does not fill uniformly even those regions tha

142 e proposed new species Nocardia wallacei (N. asteroides drug pattern IV) and N. blacklockiae (N. tran

143 th DNA-DNA hybridization, indicated that "N. asteroides drug pattern IV," "N. transvalensis new taxon

144 hybridization results confirm that Nocardia asteroides drug pattern type VI, which has long been rec

145 han 3 meters, reveals new discoveries on the asteroid, e.g., a giant basin at the big end, a sharply

146 both bright and dark (high- and low-albedo) asteroids eventually break up, we find that low-albedo a

147 omenon that is of fundamental importance for asteroid evolution and sulfur delivery to the Earth.

148 ds is associated with more than 100 distinct asteroid families, meaning that these asteroids originat

149 rs ago, in agreement with estimates of Vesta asteroid family age based on dynamical and collisional c

150 We discovered a 4-billion-year-old asteroid family extending across the entire inner part o

151 raints, supporting the notion that the Vesta asteroid family was formed during this event.

152 ming populations, and thus to be relevant to asteroid formation and meteorite petrogenesis.

153 model used to explain this assumes that most asteroids formed in situ from a primordial disk that exp

154 SSaDV was detected in museum specimens of asteroids from 1942, suggesting that it has been present

155 nce that, like the terrestrial planets, some asteroids generated crust and underwent large-scale diff

156 We found that the asteroid has been continuously increasing its rotation r

157 The physical behaviour of such 'rubble-pile' asteroids has been traditionally described using only gr

158 Airbursts/impacts by a fragmented comet or asteroid have been proposed at the Younger Dryas onset (

159 So far, no measurements of water ice on asteroids have been made, but its presence has been infe

160 Thus, these asteroids have higher concentrations of CAI material, ap

161 Asteroids hitting Earth typically vaporize a mass of tar

162 ification of silicone lenses associated with asteroid hyalosis accounted for the most cases (3/4) of

163 f lens is not appropriate in the presence of asteroid hyalosis.

164 The Chicxulub asteroid impact (Mexico) and the eruption of the massive

165 dinosaur habitability in the wake of various asteroid impact and Deccan volcanism scenarios.

166 roles of Deccan volcanism and the Chicxulub asteroid impact as kill mechanisms for this event.

167 These results support the asteroid impact as the main driver of the non-avian dino

168 An asteroid impact at the end of the Cretaceous caused mass

169 tions, such as those that occurred after the asteroid impact at the end of the Cretaceous period appr

170 oduces the same crater morphology as that of asteroid impact craters.

171 atastrophe in the wake of the end-Cretaceous asteroid impact had drastic effects that rippled through

172 An asteroid impact in the Yucatan Peninsula set off a seque

173 Asteroid impact models generate a prolonged cold winter

174 ite after a rare 4-kiloton of TNT-equivalent asteroid impact over the foothills of the Sierra Nevada

175 phenomena, including planetary formation and asteroid impact sites, the formation of interstellar dus

176 The asteroid impact that formed the 66 Ma Chicxulub crater h

177 , continental uplift and erosion, volcanism, asteroid impact) play a moderating role.

178 s, such as those predicted to result from an asteroid impact, on ten Campanian and seven Maastrichtia

179 canism mitigated the most extreme effects of asteroid impact, potentially reducing the extinction sev

180 OA could feasibly have been produced by the asteroid impact.

181 ass extinction coinciding with the Chicxulub asteroid impact.

182 archaic birds coinciding with the Chicxulub asteroid impact.

183 de risks that are well characterized such as asteroid impacts and supervolcanic eruptions, as well as

184 ources - supernovae, gamma-ray bursts, large asteroid impacts, and passing-by stars.

185 t craters are the most obvious indication of asteroid impacts, but craters on Earth are quickly obscu

186 stones formed from molten rock ejected from asteroid impacts.

187 characteristics, formation, and evolution of asteroids in general.

188 stem hydrothermal alteration of carbonaceous asteroids in the early Solar System.

189 The asteroids in the main asteroid belt have been discovered

190 xygen fugacities of Earth, Mars, and typical asteroids in the Solar System, suggesting that at least

191 is sometimes comparable to the mass of large asteroids in the Solar System.

192 t postulates the formation of differentiated asteroids in the terrestrial planet region, with survivi

193 rom the comet-like activity of several small asteroids, including two members of the Themis dynamical

194 Sulfur depletion on asteroids is a long-standing, yet unresolved phenomenon

195 A quarter of known asteroids is associated with more than 100 distinct aste

196 culture growth and identification of this N. asteroides isolate affected both initial therapeutic dec

197 s of soil samples from both the Moon and the asteroid Itokawa determined that nanophase metallic part

198 infrared observations have shown that small asteroids (kilometre-sized or smaller) are covered by a

199 For asteroids larger than about ten kilometres in diameter,

200 ed spectral differences between it and other asteroids make 24 Themis unique so far, and our identifi

201 sing candidate disease agent responsible for asteroid mass mortality.

202 This high-porosity asteroid may link cosmic fluffy dust to dense celestial

203 in celestial mechanics has revealed that an asteroid may orbit stably in the same region as a planet

204 ns match those of Earth's mantle, so EC-like asteroids might have contributed these volatile elements

205 present in the telescopic spectra of several asteroids; modeling indicates that these contain approxi

206 resolved spectroscopic observations of this asteroid, mostly covering the northern hemisphere and th

207 onstrain the formation history of Ryugu: the asteroid must be a rubble pile formed from impact fragme

208 All isolates of N. cyriacigeorgica, N. asteroides, N. abscessus, and N. otitidiscaviarum were s

209 tant to imipenem, but N. cyriacigeorgica, N. asteroides, N. farcinica, and N. abscessus were only mod

210 n is reflected) asteroids, the characterized asteroids near the Sun typically have high albedos.

211 ndica is a rare pathogen related to Nocardia asteroides, Nocardia neocaledoniensis, and Nocardia cais

212 2015 BZ509 is indeed a retrograde co-orbital asteroid of the planet Jupiter.

213 Retrograde co-orbital asteroids of Jupiter and other planets may be more commo

214 The determination of which asteroids of the remaining population are members of und

215 Asteroid (101955) Bennu is a dark asteroid on an Earth-crossing orbit that is thought to h

216 dence of magmatic activity in a carbonaceous asteroid on the verge of differentiating and demonstrate

217 ignited after the impact of a 10-km-diameter asteroid on the Yucatan Peninsula 66 million y ago.

218 It has been proposed that fragments of an asteroid or comet impacted Earth, deposited silica- and

219 erial has been detected on the surface of an asteroid or directly proven to be an asteroidal constitu

220 ies they studied are indeed older than known asteroids or formed before the injection of (26)Al into

221 the clast possibly originated from D/P type asteroids or trans-Neptunian Objects.

222 as determined by observations of near-Earth asteroids, or from the Moon's incomplete impact chronolo

223 stinct asteroid families, meaning that these asteroids originate as impact fragments from the family

224 This suggests that primitive chondritic asteroids, originating from a similar source region, wer

225 ces in the discovery and characterization of asteroids over the past decade have revealed an unantici

226 ausible mechanism for their synthesis in the asteroid parent bodies, and strongly supports an extrate

227 We find a pattern of excess depletion of asteroids, particularly just outward of the Kirkwood gap

228 r the affected splice junction replicate the asteroid phenotype.

229 h orbital resonances with the giant planets; asteroids placed in these locations will follow chaotic

230 lly explain fast rotation rates in the small-asteroid population.

231 the depletion of the primordial main belt of asteroids predict 10-15 craters >400 km should have form

232 belt whose members include most of the dark asteroids previously unlinked to families.

233 Asteroids provide fundamental clues to the formation and

234 ains, is the most likely dominant short-term asteroid resurfacing process.

235 Hayabusa2 spacecraft investigated the small asteroid Ryugu, which has a rubble-pile structure.

236 spacecraft Hayabusa2(5), indicating that the asteroid's boulders and their surroundings have similar

237 We simulated the asteroid's close Earth approaches from 2001 to 2005, sho

238 has played an important role in shaping the asteroid's geology.

239 An asteroid's history is determined in large part by its st

240 l dehydration due to internal heating of the asteroid's parent body.

241 observations of Bennu to understand how the asteroid's properties compare to pre-encounter expectati

242 sest distance of 770 +/- 120 meters from the asteroid's surface.

243 the future of meteorite research, including asteroid sample return missions.

244 lations to derive the impact strength at the asteroid scale(4,5).

245 tion of ophiuroid brittle stars as sister to asteroid sea stars (the Asterozoa hypothesis).

246 Less reddened asteroids seem to cross most deeply into the terrestrial

247 ity pattern type VI and distinct from the N. asteroides sensu stricto strain ATCC 19247(T).

248 Asteroid shapes and hydration levels can serve as tracer

249 Models predict that numerous asteroids should be found on orbits that closely approac

250 Observations of comets and asteroids show that the solar nebula that spawned our pl

251 We find that this asteroid shower is the most likely source (>90 per cent

252 type asteroids are not currently found among asteroids showing no evidence of recent close planetary

253 ause thermal fragmentation is independent of asteroid size, this process can also contribute to regol

254 terplanetary dust particles and on lunar and asteroid soil regolith grains.

255 h's current supply of water was delivered by asteroids, some time after the collision that produced t

256 Populations of at least 20 asteroid species on the Northeast Pacific Coast have rec

257 The detection of asteroid spin-up supports the YORP effect as an explanat

258 miliar phenomena of raining and catastrophic asteroid strikes.

259 ace weathering' process that rapidly reddens asteroid surfaces in less than 10(6) years.

260 es that can produce both fresh and weathered asteroid surfaces resolves the decades-long puzzle of th

261 mpact craters such as those on planetary and asteroid surfaces.

262 mal breakdown and assess its significance on asteroid surfaces.

263 Planned upgrades to contemporary asteroid survey instruments and improved data processing

264 We conclude that water ice is more common on asteroids than was previously thought and may be widespr

265 ceous chondrites are meteoritic fragments of asteroids that avoided the geological reprocessing of la

266 es of the sizes and impact velocities of the asteroids that created global spherule layers.

267 88P is part of a young family of at least 11 asteroids that formed from a precursor about 10 kilometr

268 The barrage of comets and asteroids that produced many young lunar basins (craters

269 red, consistent with comets or organic-rich asteroids that reside within the Solar System.

270 istory; this is especially true for Nocardia asteroides, the type species of the genus and previously

271 Chondritic meteorites are fragments of asteroids, the building blocks of planets, that retain a

272 per cent of incident radiation is reflected) asteroids, the characterized asteroids near the Sun typi

273 'Unweathered' asteroids (those having spectra matching the most common

274 evolution of planetary bodies, ranging from asteroids to the large rocky planets, is thought to begi

275 ified over the imaged area of the near-Earth asteroid Toutatis.

276 ASTEROID treated 507 coronary disease patients with rosu

277 the anomalous distribution of spin rates for asteroids under 10 kilometers in diameter and as a binar

278 body would likely be classified as a V-type asteroid, V-type precursors for basaltic meteorites unre

279 The surface of the asteroid Vesta has prominent near-infrared absorption ba

280 The asteroid Vesta is the smallest known planetary body that

281 Likewise, an extrapolation from the asteroid Vesta would require at least 6-7 such basins.

282 ated the origin of unusual pitted terrain on asteroid Vesta, revealed in images from the Dawn spacecr

283 during occultation by the Dawn spacecraft at asteroid Vesta.

284 ation was sufficient to produce Vesta-family asteroids (Vestoids) and HED meteorites.

285 At the ultrastructural level, mutant asteroid/vglut3 hair cells show a decrease in the number

286 bulo-ocular and acoustic startle reflexes in asteroid/vglut3 mutants was attributable to a defect in

287 of hair cells and labeling is not present in asteroid/vglut3 mutants.

288 tic acousticolateralis neurons are absent in asteroid/vglut3 mutants.

289 with sizes similar to those of the main belt asteroids, VSPA becomes inefficient beyond approximately

290 On 6 October 2008, a small asteroid was discovered with a flat reflectance spectrum

291 A 200-km large asteroid was disrupted by a collision in the Main Astero

292 Nocardia asteroides was isolated after prolonged culture from the

293 perienced an extensive outbreak of sea-star (asteroid) wasting disease (SSWD).

294 Scaling from the observed Hungaria asteroids, we find that E-belt projectiles made about te

295 disintegration) of a substantial fraction of asteroids when they achieve perihelion distances of a fe

296 unambiguously identified on the surfaces of asteroids, whereas they have been detected on cometary n

297 ed human spaceflight to another planet or an asteroid will introduce unique challenges of mitigating

298 f P/2010 A2, a previously unknown inner-belt asteroid with a peculiar, comet-like morphology.

299 lies of asteroids--a family consists of many asteroids with similar orbits and, frequently, similar s

300 presence of water ice on the surface of some asteroids, with sublimation a potential reason for the d