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 arge as 0.5 km over nearly 40 percent of the asteroid.

5 surface properties and rotation state of the asteroid.

6 abundant in symptomatic than in asymptomatic asteroids.

7 itational escape velocity of kilometre-sized asteroids.

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

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

10 ons for the geological history of chondritic asteroids.

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

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

13 but the region is not uniformly filled with asteroids.

14 collisional evolution than typical main-belt asteroids.

15 d that fragments of these bodies survived as asteroids.

16 meteorites) do not seem to be abundant among asteroids.

17 d the four terrestrial planets, the Moon and asteroids.

18 simals, analogues of Solar System comets and asteroids.

19 roids but very similar to that of near-Earth asteroids.

20 range of topography on small satellites and asteroids.

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

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

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

24 ocess governing regolith generation on small asteroids.

25 contribute to regolith production on larger asteroids.

26 rus associated with tissues from symptomatic asteroids.

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

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

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

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

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

32 rt that a dark region on a small (550-metre) asteroid-25143 Itokawa-is significantly more space-weath

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

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

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

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

37 diogenites, which are thought to sample the asteroid 4 Vesta) and the angrites (from an unidentified

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

39 nd, like them, are probably derived from the asteroid 4 Vesta.

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

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

42 The second most massive asteroid--4 Vesta--has differentiated to a crust, mantle

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

44 Asteroid 433 Eros, the most closely studied small body,

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

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

47 The asteroid 617 Patroclus is the only known binary Trojan.

48 al and orbital dynamics of binary near-Earth asteroid 66391 (1999 KW4) suggest that it is excited as

49 gh-resolution radar images reveal near-Earth asteroid (66391) 1999 KW4 to be a binary system.

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

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

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

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

54 Many decades of asteroid and comet characterization have yielded formati

55 erplanetary dust particles (IDPs), which are asteroid and comet fragments of diameter approximately 1

56 core-mantle material from a single disrupted asteroid and have no known equivalents among the basalti

57 The combined asteroid and meteorite reflectance spectra identify the

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

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

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

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

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

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

64 ks that must be collisionally replenished by asteroids and comets, as the dust would otherwise be dep

65 reflecting the direct ('primary') impacts of asteroids and comets.

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

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

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

69 urface most closely resembles that of C-type asteroids and small outer Solar System bodies such as Ch

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

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

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

73 ow-gravity environment, simply landing on an asteroid appears to be much more challenging than we had

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

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

76 We predict that some asteroids are main-belt interlopers (such as (4) Vesta).

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

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

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

80 Asteroids are primitive Solar System bodies that evolve

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

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

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

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

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

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

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

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

89 Asteroids, because of the hazard they pose to Earth, are

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

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

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

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

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

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

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

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

98 Collisions in the asteroid belt frequently lead to catastrophic breakups,

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

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

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

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

103 The asteroid belt therefore preserves a record of both this

104 for identification of recent breakups in the asteroid belt using catalogs of osculating (i.e., instan

105 The accretion of bodies in the asteroid belt was halted nearly 4.6 billion years ago by

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

107 Hence, both meteorites (originating from the asteroid belt) and interplanetary dust particles (possib

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 nce for planet-sized objects in the earliest asteroid belt, as required by current numerical simulati

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

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

113 that were dynamically ejected from the main asteroid belt, possibly due to the orbital migration of

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

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

116 e usually assumed to have formed in the main asteroid belt, which is the source of most meteorites.

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

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

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

120 ype asteroids which are abundant in the main asteroid belt.

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

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

123 ration of material transported into the main asteroid belt.

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

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

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

127 n quite different from that of the main belt asteroids but very similar to that of near-Earth asteroi

128 alter the trajectory of an Earth-threatening asteroid by using gravity as a towline.

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

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

131 5 Myr ago, but its origin by comet shower or asteroid collision remains uncertain.

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

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

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

135 the unofficial species designation Nocardia asteroides complex antimicrobial susceptibility pattern

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

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

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

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

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

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

148 oups of fragments with similar orbits called asteroid families.

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

150 Here we report the discovery of a very young asteroid family around the object 1270 Datura.

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

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

153 Trojan population consists of two swarms of asteroids following the same orbit as Jupiter and locate

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

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

156 articular straight-line distance through the asteroid from the centre of the large crater suggests de

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

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

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

160 ades of speculation, the existence of binary asteroids has been observationally confirmed, with examp

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

162 1 Ceres, the largest and most massive asteroid, has in contrast been presumed to be homogeneou

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

164 Several dozen large asteroids have been disrupted by impacts over the past s

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

166 res in reflected sunlight indicate that some asteroids have experienced sufficient thermal evolution

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

168 Asteroids hitting Earth typically vaporize a mass of tar

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

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

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

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

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

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

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

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

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

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

179 ass extinction coinciding with the Chicxulub asteroid impact.

180 archaic birds coinciding with the Chicxulub asteroid impact.

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

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

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

184 stones formed from molten rock ejected from asteroid impacts.

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

186 The slow but persistent collisions between asteroids in our Solar System generate a tenuous cloud o

187 The asteroids in the main asteroid belt have been discovered

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

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

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

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

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

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

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

195 For asteroids larger than about ten kilometres in diameter,

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

197 sing candidate disease agent responsible for asteroid mass mortality.

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

199 eroids suggests that the surfaces of small S asteroids may have developing stages of space weathering

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

201 and the outer several tens of metres of the asteroid must be composed of relatively non-cohesive mat

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

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

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

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

206 2015 BZ509 is indeed a retrograde co-orbital asteroid of the planet Jupiter.

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

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

209 The dynamical and physical properties of asteroids offer one of the few constraints on the format

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

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

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

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

214 y recent frequent or huge collisions between asteroids or other 'planetesimals' whose orbits are bein

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

216 catalogs of osculating (i.e., instantaneous) asteroid orbits.

217 ely 10(8) yr has been deduced from main belt asteroid orbits.

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

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

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

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

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

223 r the affected splice junction replicate the asteroid phenotype.

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

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

226 d Mercury and from the size distributions of asteroid populations.

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

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

229 Asteroids provide fundamental clues to the formation and

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

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

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

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

234 w mission from Japan that has made the first asteroid sample return attempt, this goal is now within

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

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

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

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

239 Trojan asteroids share a planet's semimajor axis but lead or fo

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

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

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

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

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

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

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

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

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

249 miliar phenomena of raining and catastrophic asteroid strikes.

250 Processes operating on such asteroids strongly influenced the final composition of t

251 A recent survey of small, near-Earth asteroids suggests that the surfaces of small S asteroid

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

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

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

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

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

257 llisional disruption of the >150-km-diameter asteroid that created the Veritas family 8.3 +/- 0.5 Myr

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

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

260 88P is part of a young family of at least 11 asteroids that formed from a precursor about 10 kilometr

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

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

263 oximately 3.8 billion years ago were made by asteroids that were dynamically ejected from the main as

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

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

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

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

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

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

270 ASTEROID treated 507 coronary disease patients with rosu

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

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

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

274 The asteroid Vesta is the smallest known planetary body that

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

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

277 during occultation by the Dawn spacecraft at asteroid Vesta.

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

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

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

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

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

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

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

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

286 Nocardia asteroides was isolated after prolonged culture from the

287 Ultrasound-Derived Coronary Atheroma Burden [ASTEROID]) was performed at 53 community and tertiary ca

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

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

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

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

292 come optically altered, to become the S-type asteroids which are abundant in the main asteroid belt.

293 ly origin of the disk is a tidally disrupted asteroid, which has been destabilized from its initial o

294 pace-weathered materials accumulate on small asteroids, which are likely to be the parent bodies of L

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

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

297 H, L, and LL) chondrites, there must be many asteroids with ordinary-chondrite compositions in near-E

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

299 The spacecraft hovers near the asteroid, with its thrusters angled outwards so that the

300 through the disruptive collision of a parent asteroid, with the new primary resulting from accretion

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