ライフサイエンスコーパス: solar system

1 id of water because they formed in the inner Solar System.

2 the surface dates from the formation of the Solar System.

3 ic radar observations of a small body in the solar system.

4 an ancient (per)chlorate presence across our solar system.

5 largest volcanic complex on Mars and in the Solar System.

6 in planetesimals that accreted in the outer Solar System.

7 al collapse that led to the formation of the solar system.

8 icle aggregation during the formation of the Solar System.

9 es are abundant on rocky bodies of the inner solar system.

10 ate its magnetic field, the strongest in the solar system.

11 ago and on the origin of water in the inner Solar System.

12 not previously definitively observed in the Solar System.

13 cording early delivery of water to the inner Solar System.

14 e, by analogy with other large basins in the Solar System.

15 gradually losing volume, over the age of the Solar System.

16 l-rich molecular cloud material in the inner Solar System.

17 oon and the bombardment history of the early Solar System.

18 ized cometesimals in the early stages of the Solar System.

19 out its formation and evolution in the early solar system.

20 agreement with the observed structure of the Solar System.

21 the search for life on other planets in our solar system.

22 s in the interstellar medium or in the outer solar system.

23 eologic processes that occurred in the early Solar System.

24 of the large nitrogen isotopic range in the solar system.

25 e ubiquitous in planetary atmospheres in the Solar System.

26 ities far greater than those observed in our Solar System.

27 t are inconsistent with the structure of the Solar System.

28 arable to the mass of large asteroids in the Solar System.

29 preserve material from the formation of the solar system.

30 he first steps of formation of solids in our Solar System.

31 similar to the ratios in rocky bodies in the Solar System.

32 tic activity among these bodies in the early Solar System.

33 hich occurs on airless bodies throughout the solar system.

34 iled characterization of planets outside the Solar System.

35 of finding habitable environments beyond the solar system.

36 surprisingly so, as they are missing in our solar system.

37 s a potentially important constituent in the solar system.

38 nts to a dramatic early history of the inner Solar System.

39 usively around the four giant planets in the Solar System.

40 odies is a ubiquitous process throughout the solar system.

41 chaotic planetary system reminiscent of the solar system.

42 other dynamically stable populations in the Solar System.

43 tudy volatile element depletion in the early solar system.

44 unusual processes that occurred in the early solar system.

45 grains in the cold, outer edge of the early Solar System.

46 adiation event during accretion in the early solar system.

47 knowledge of smaller meteoroids in the outer solar system.

48 nd that are smaller than those we see in the Solar System.

49 likely in planetary bodies in and beyond our solar system.

50 iscent of the orderly arrangement within the solar system.

51 lar oxygen isotopic composition of the inner solar system.

52 ive remnants of planetesimals from the early Solar System.

53 150 million years after the formation of the solar system.

54 ast than any adjacent pair of planets in the solar system.

55 d have also been discovered elsewhere in the Solar System.

56 are consistent with meteoritic values in the Solar System.

57 0 million years (Myr) after the birth of the Solar System.

58 eme environments on Earth and throughout the Solar System.

59 ogical and geochemical systems and the early Solar System.

60 l to the use of comets in studying the early solar system.

61 ation of carbonaceous asteroids in the early Solar System.

62 nt a phase of magmatic activity early in the Solar System.

63 dances inform our understanding of the early Solar System.

64 35% from ~0.95-1.2 AU to 0.95-1.31 AU in our solar system.

65 high priority task in the exploration of the Solar System.

66 Kuiper Belt is a distant region of the outer Solar System.

67 ugu is among the darkest known bodies in the Solar System.

68 action of the plutonium present in the early Solar System.

69 t of a gentle, low-speed merger in the early Solar System.

70 netic fields present during evolution of the Solar System.

71 80 million years before the formation of the Solar System.

72 tems on Earth, and possibly elsewhere in the solar system.

73 cretion processes that operated in the early Solar System.

74 agnetic recordings from the formation of the Solar System.

75 se some of the largest known channels in the Solar System.

76 rganic-rich asteroids that reside within the Solar System.

77 well as in magnetized plasmas throughout the solar system.

78 y to addressing numerous questions about our solar system.

79 nation compared with other reservoirs in the solar system.

80 s of atmospheric circulation not seen in the solar system.

81 of water and organic compounds in the early solar system.

82 a large short-period comet within the inner Solar System.

83 on the TRAPPIST-1 planets compared with the solar system.

84 discovered thousands of planets outside the Solar System(1), most of which orbit stars that will eve

85 s of (92,94)Mo and (96,98)Ru isotopes in the Solar System(1,3,14) and for the signatures of early Uni

86 .6 Ma to ~3 +/- 2 Ga before the start of the Solar System ~4.6 Ga ago.

87 similar to that of rocky bodies in the inner Solar System(5).

88 t of a meteorite, likely formed in the early solar system about 4.5 Gya.

89 mparing numerical simulations with the early Solar System abundance ratios of actinides produced excl

90 bulk of the material that formed the Sun and Solar System accreted within the CAI-forming epoch, whic

91 evidence for organic synthesis in the early solar system activated by an anomalous nitrogen-containi

92 The timing of water accretion to the inner solar system also has implications for how and when life

93 y lose their H(2); this process has no known Solar System analog.

94 sols are common among the atmospheres of our solar system and beyond.

95 inertial motion about the barycenter of the solar system and closely linked to an increase of solar

96 tury from observations of planets in our own Solar System and has served as a cornerstone of planet-f

97 on with low temperature ices relevant to the solar system and interstellar medium.

98 implications for the origins of water in the solar system and other astrophysical environments.

99 n, another radionuclide present in the early solar system and produced in the same events.

100 for planetary surfaces throughout the inner Solar System and provides evidence of the dynamic nature

101 one of the oldest hydrogen reservoirs in the solar system and show that Vesta contains the same hydro

102 est that collisions were common in the young Solar system and that a similar event may have also occu

103 of interplanetary dust throughout the inner solar system and the associated impacts on Mars's atmosp

104 e relative homogeneity of Mg isotopes in the solar system and the lack of Mg isotope fractionation by

105 ve determined the evolutionary course of our Solar System and the planetary bodies within it.

106 surfaces of small rocky bodies in the inner solar system and their spatial and size distributions gi

107 This configuration is similar to that of our Solar System, and contrasts with the isolated hot Jupite

108 s perhaps the most important molecule in the solar system, and determining its origin and distributio

109 Thus, Jupiter is the oldest planet of the Solar System, and its solid core formed well before the

110 es on the terrestrial planets throughout the solar system, and on at least Earth and Mars impacts hav

111 , the study of isotopic heterogeneity in the Solar System, and other studies.

112 predicted chaotic dynamical behaviour of the Solar System, and provides a constraint for refining num

113 y bodies, the delivery of water to the inner Solar System, and the formation of prebiotic molecules.

114 n our understanding of dust evolution in the solar system, and transport from the middle atmosphere t

115 onized astronomy, offering new insights into solar system architecture and planet demographics.

116 bundances of (92)Nb and (146)Sm in the early solar system are determined from meteoritic analysis, an

117 Solar System, their abundances in the early Solar System are known because their daughter products w

118 archetypal examples of planets, those of our solar system are merely possible outcomes of planetary s

119 rates that most of the gross features of the solar system are one outcome in a continuum of possibili

120 flares--the most powerful explosions in the solar system--are also efficient particle accelerators,

121 the same star-formation processes in our own solar system as those that we can observe now through te

122 uded a spike in the bolide flux to the inner solar system at ca. 3.85-3.95 Ga (the Late Heavy Bombard

123 t with volatile-rich material from the outer Solar System being delivered to Earth during late accret

124 incorporated into the "building material" of solar systems, biorelevant molecules such as glycerol co

125 ondritic meteorites, and their signatures on solar system bodies have been sought for decades.

126 Asteroids are primitive Solar System bodies that evolve both collisionally and t

127 In particular, CO2 ice is present in several solar system bodies, as well as in interstellar and circ

128 plain the origin of nucleobases in the inner Solar System bodies, including meteorites and extra-terr

129 Inner solar system bodies, including the Earth, Moon, and aste

130 processes controlling the evolution of small solar system bodies.

131 features, unlike those on previously visited Solar System bodies.

132 is 76 AU, far greater than that of any other Solar System body.

133 coupling which is unusual for planets in our solar system but may be common for close-in extrasolar p

134 rent orbits of the four giant planets in the Solar System by disrupting a theoretical initial resonan

135 could instead be readily produced within the Solar System by heavy solar-wind ions exchanging electro

136 Relative to younger objects in the Solar System, CAIs contain positive r-process anomalies

137 s range in the earliest formed solids in our Solar System, calcium-aluminum-rich inclusions (CAIs), a

138 The observable Solar System can be divided into three distinct regions:

139 The gas and ice giants in our solar system can be seen as a natural laboratory for the

140 e isotopic signature extending from an inner Solar System composition toward a (26)Mg*-depleted and (

141 e uniform, and yet distinct from the average Solar System composition.

142 has not been possible to define a primordial solar system composition.

143 Dynamical models can produce inner Solar System configurations that closely resemble our So

144 are most beautiful and dynamic places in the solar system, consisting of ice particles in a constant

145 hat they formed in a different region of the solar system, contrary to predictions of recent dynamica

146 s are much more highly irradiated than their solar system counterparts.

147 f planets, which are very common yet have no solar system counterparts.

148 s are the first solids to have formed in the Solar System, defining the epoch of its birth on an abso

149 Even for the planets in the Solar System, difficulties in observation lead to large

150 nd magnetic flux that travel out through the solar system, driving extreme space weather.

151 ovides evidence of the dynamic nature of the Solar System during the planet-forming era.

152 of extreme environments from which the early solar system emerged and evolved.

153 grains formed in the innermost region of the solar system ended up much farther out in the solar syst

154 portant role in prebiotic reactions in early solar system environments.

155 ce of short-lived radionuclides in the early solar system, especially (60)Fe, (26)Al, and (41)Ca, req

156 tem configurations that closely resemble our Solar System, especially when the orbital effects of lar

157 tely defining the absolute timeline of early Solar System events.

158 l is representative of the earliest stage of solar system evolution in which a chiral molecule has be

159 re of a wide variety of processes, including solar system evolution, geological formational temperatu

160 Water throughout the solar system exhibits deuterium-to-hydrogen enrichments,

161 Nitrogen isotopic distributions in the solar system extend across an enormous range, from -400

162 rves the average isotopic composition of the solar system for elements heavier than lithium, we concl

163 tiation within the first 30 million years of Solar System formation and implies the formation of a co

164 roperties determine comet evolution and even solar system formation because comets are considered rem

165 Solar system formation may have been "triggered" by ioni

166 Current Solar System formation models do not predict conditions

167 anetary bodies during the earliest stages of Solar System formation remain poorly understood.

168 e (T Tauri) phase of star formation, placing Solar System formation within an astronomical context.

169 an approximately 200 Myr into the history of Solar System formation would not have resulted in a redu

170 ntact protoplanet from the earliest epoch of solar system formation, based on analyses of howardite-e

171 much debated, with distinct implications for solar system formation, dynamics, and geology.

172 ximately 1 My and approximately 3-4 My after Solar System formation.

173 h differentiation within the first 100 My of solar system formation.

174 star formation and cosmochemical studies of Solar System formation.

175 imitive objects preserving information about Solar System formation.

176 ly found in the interstellar medium prior to solar system formation.

177 likely occurred within less than 10 My after Solar System formation.

178 es until at least approximately 3-4 My after Solar System formation.

179 iate until about 4 to 11 million years after solar system formation.

180 1 million years ago, 3.8 million years after solar system formation.

181 Most rocky bodies in the Solar System formed at oxygen fugacities approximately f

182 e to hydrogen, it is estimated that when the Solar System formed, the circumstellar disk must have ha

183 , more than about 60 million years after the Solar System formed.

184 ound stars that lived their lives before the solar system formed.

185 hat neutral interstellar atoms flow into the solar system from a different direction than found previ

186 ell documented to have occurred in the early Solar System from the recognition of numerous basaltic m

187 es hit the surfaces of airless bodies in the Solar System, generating charged and neutral gas clouds,

188 No known objects in the Solar System have such extreme dimensions.

189 reated during the first ~50 million years of solar system history, indicating that portions of the ma

190 formed within the first 30 million years of solar system history-indicates that the mantle may have

191 in records of the first few million years of solar system history.

192 formed within the first 60 million years of solar system history.

193 ary disk is consistent with formation of our Solar System in an active star-forming region of the gal

194 ets harbor the most pristine material in our solar system in the form of ice, dust, silicates, and re

195 sozoic owing to the chaotic diffusion of the solar system in the past.

196 The so far unique role of our Solar System in the universe regarding its capacity for

197 n reproduce the basic structure of the inner solar system, including a small Mars and a low-mass aste

198 ected from all the magnetized planets in our Solar System, including Earth.

199 ay provide a unique window into the earliest Solar System, including the origin of short-lived radioi

200 entification of habitable planets beyond our solar system is a key goal of current and future space m

201 umented in long runout landslides across our solar system is commonly associated with the existence o

202 for evidence of extraterrestrial life in our Solar System is currently guided by our understanding of

203 the timing of its accretion within the inner solar system is important for understanding the dynamics

204 The solar system is littered, however, with distorted polyhe

205 short-lived radioisotopes were added to the Solar System is necessary to assess their validity as ch

206 ly 750,000 known asteroids and comets in the Solar System is thought to have originated outside it, d

207 clear whether this oxidation of rocks in the Solar System is typical among other planetary systems.

208 there has been no way of telling whether the Solar System is typical of planetary systems.

209 When viewed in this context, the Solar System is unusual.

210 he age of Jupiter, the largest planet in our Solar System, is still unknown.

211 rotoplanetary disks, which can evolve toward solar systems like our own.

212 powerful persistently active volcano in the Solar System, Loki Patera.

213 ically derived from gases in the early inner solar system (< approximately 2 AU), and that bulk inner

214 neutron-capture events that contaminated the solar system material at ~100 million years and ~30 mill

215 Through the laboratory study of ancient solar system materials such as meteorites and comet dust

216 odern and ancient Earth, Mars, and the early solar system (meteorites).

217 considered the most primitive bodies in the solar system, N2 has not been detected.

218 olar system ended up much farther out in the solar system, not only the asteroid belt but even in the

219 The outer Solar System object (486958) Arrokoth (provisional desig

220 The 'snowline' conventionally divides Solar System objects into dry bodies, ranging out to the

221 g and demonstrates that some primitive outer Solar System objects related to icy asteroids and comets

222 and circumstellar regions, making a stop in solar system objects that could have delivered organic s

223 es for unsampled units on the Moon and other Solar System objects.

224 ble gases differ in the Sun from other inner solar system objects.

225 100 million years after the formation of the Solar System, OIB and MORB mantle sources must have diff

226 us formed shortly after the formation of the solar system or that the current activity was triggered

227 approximately 1.5 My after the start of the Solar System or the transport of precursors from the con

228 r out of cometesimals accreting in the early solar system or, alternatively, out of comparable-sized

229 y of our lineage (on Earth, elsewhere in the solar system, or on an extrasolar planet) would provide

230 s that is inconsistent with recent models of solar system orbital architecture that require an early,

231 ions of these effects to physical chemistry, solar system origin models, terrestrial atmospheric and

232 e comet nuclei during migration to the inner solar system, perhaps explaining this lack of a substant

233 lude that Pluto's atmosphere is unique among Solar System planetary atmospheres, as its radiative ene

234 Including solar system planets yields a relation: rho = 2:32 + 3:1

235 short-lived r-process isotopes in the early Solar System point to their origin in neutron-star merge

236 ite groups requires isolation from the outer Solar System, possibly by the opening of disk gaps from

237 ain, and the chaotic dynamical nature of the Solar System predicted by theoretical models has yet to

238 In the nascent solar system, primitive organic matter was a major contr

239 The isotopic composition of our Solar System reflects the blending of materials derived

240 vering and characterizing planets beyond our solar system relies upon measurement of weak Doppler shi

241 ion of volatile-rich material from the outer Solar System represents a crucial prerequisite for Earth

242 step to understand planetary origins in our Solar System requires a mission to their Ice Giant sibli

243 Bulk inner Solar System reservoirs record positively correlated var

244 g the brief visit by the object to the inner Solar System reveal it to be asteroidal, with no hint of

245 of albedos is among the largest observed on Solar System rocky bodies.

246 (< approximately 2 AU), and that bulk inner solar system S-isotope composition was chondritic (consi

247 igins of the (33)S anomalies, or of the bulk solar system S-isotope composition.

248 ing within the first 10 million years of the Solar System's approximately 4.5 billion-year history, s

249 The inner solar system's biggest and most recent known collision w

250 Astronomical calculations reveal the Solar System's dynamical evolution, including its chaoti

251 ecause they preserve a record of some of the Solar System's earliest ( approximately 4.5 Gy) chemical

252 This finding implies that, if the solar system's formation was typical, abundant interstel

253 haotic resonance transition at ~50 Ma in the Solar System's fundamental frequencies.

254 d by most scenarios for the formation of the solar system's innermost planet.

255 active earlier in its history.Mars hosts the solar system's largest volcanoes, but their formation ra

256 Mars hosts the solar system's largest volcanoes.

257 by rapid groundwater evacuation scoured the Solar System's most voluminous channels, the southern ci

258 Like our Moon, the majority of the solar system's satellites are locked in a 1:1 spin-orbit

259 In this scenario, the Solar System's terrestrial planets formed from gas-starv

260 ion, can explain the low overall mass of the Solar System's terrestrial planets, as well as the absen

261 and its viability as the sole source for the solar system's water.

262 gma oceans were once ubiquitous in the early solar system, setting up the initial conditions for diff

263 g stars (analogues of the Kuiper Belt in our Solar System) show a variety of non-trivial structures a

264 largest cosmic catastrophes occurred in our solar system since the accretion of the planets.

265 ich inclusions, (CAIs)] represent the oldest Solar System solids and provide information regarding th

266 aluminium-rich inclusions (CAIs), the oldest Solar System solids.

267 on years after the formation of the earliest solar system solids.

268 The solar system (SS) moves through the interstellar medium

269 on the Moon and other airless bodies in our solar system such as Mercury and asteroids.

270 Currently, ocean worlds in the outer Solar System, such as the icy moons Europa and Enceladus

271 of Earth, Mars, and typical asteroids in the Solar System, suggesting that at least some rocky exopla

272 The presence of 'Oumuamua in the Solar System suggests that previous estimates of the num

273 C-type) asteroids(1) are relics of the early Solar System that have preserved primitive materials sin

274 so present on other planets and moons in our solar system the mechanism elucidated here may be releva

275 suggest that, shortly after the birth of the Solar System, the molten metallic cores of many small pl

276 In the solar system, the planets' compositions vary with orbita

277 In the inner solar system, the planets' orbits evolve chaotically, dr

278 0 million years-are no longer present in the Solar System, their abundances in the early Solar System

279 ly coplanar and circular orbits found in our Solar System; their orbits may be eccentric or inclined

280 equires the (92)Nb/(92)Mo ratio in the early solar system to be at least 50% lower than the current n

281 gous to where the rocky planets orbit in the Solar System, to retaining at most a meagre amount of co

282 bundances and planetary configuration of the Solar System today, but there has been no way of telling

283 Just as secular chaos is reorganizing the solar system today, so it has likely helped organize it

284 of more than a thousand planets outside our Solar System, together with the significant push to achi

285 ch an event occurs sufficiently close to our solar system, traces of the supernova debris could be de

286 of exotic interstellar material to the inner solar system via impact.

287 e nuclei inferred to be present in the early solar system via meteoritic analyses, there are several

288 In the cold outer solar system, volcanism can occur on solid bodies with a

289 quires a nearby supernova shortly before our solar system was formed, suggesting that the Sun was for

290 This suggests that material from the outer Solar System was incorporated into Ceres, either during

291 al are expected to survive only in the outer Solar System, we infer that, similarly to cometary bodie

292 essentially all rocky materials in the inner solar system were enriched in (17)O and (18)O, relative

293 cal and chemical conditions during the early solar system when comets formed.

294 sess models of the formation dynamics of the solar system, when combined with measurements of the bul

295 te meteorites, which originated in the outer Solar System where water was more abundant.

296 the condensation of the first solids in the Solar System, whereas others claim a date later than 50

297 gainst an influx of water ice from the outer solar system, which has been invoked to explain the nons

298 satellite of Saturn, is the only one in the solar system with a dense atmosphere.

299 ation belts, unlike all other planets in the solar system with internal magnetic fields.

300 on is one of the most common elements in the solar system, with a fractional abundance of 10(-4) rela

301 bolic and hyperbolic escaping orbits, of the solar system without learning or knowing Newton's laws o