ライフサイエンスコーパス: planetary

1 rules during the first five million years of planetary accretion to explain their observed abundance.

2 Since planetary accretion, water has been exchanged between th

3 tion at depth and processes occurring during planetary accretion.

4 data to document the Arctic-wide decrease in planetary albedo and its amplifying effect on the warmin

5 ysis reveals a striking relationship between planetary albedo and sea ice cover, quantities inferred

6 We find that the Arctic planetary albedo has decreased from 0.52 to 0.48 between

7 Wind tunnel data collected under ambient and planetary-analogue conditions inform our models of aeoli

8 rather than impact craters such as those on planetary and asteroid surfaces.

9 significant mutual inclinations between the planetary and binary star orbital planes.

10 s used as chronometers and tracers in earth, planetary, and environmental sciences.

11 point the contributions of microorganisms to planetary, animal and human health.

12 The spectrum is indicative of a planetary atmosphere in which the abundance of heavy ele

13 ly 250 parts per million) indicates that the planetary atmosphere is predominantly clear down to an a

14 observe the composition and dynamics of the planetary atmosphere.

15 ronments such as the interstellar medium and planetary atmospheres (CN, SiN and C2H), and combustion

16 Aerosols are ubiquitous in planetary atmospheres in the Solar System.

17 cal species relevant to the understanding of planetary atmospheres other than that of Earth.

18 Because all planetary atmospheres possess ionospheres, we anticipate

19 Observations of sulfur compounds in planetary atmospheres when compared with model results s

20 to's atmosphere is unique among Solar System planetary atmospheres, as its radiative energy equilibri

21 conditions consistent with extraterrestrial planetary atmospheres, that ammonia forms clathrate hydr

22 e in the gas-phase systems of combustion and planetary atmospheres.

23 culations of propagation of stellar light in planetary atmospheres.

24 Planetary auroras reveal the complex interplay between a

25 tion the imaging of motion patterns inside a planetary ball mill from simulations and video recording

26 A planetary ball mill proved to be more suitable for the s

27 Processes inside planetary ball mills are complex and strongly depend on

28 Planetary ball mills are well known and used for particl

29 during the last few years the application of planetary ball mills has extended to mechanochemical app

30 delines to follow for modelling processes in planetary ball mills in terms of refinement, synthesis'

31 ons illustrate the effect of the geometry of planetary ball mills on the energy entry.

32 icant and hardly measurable for processes in planetary ball mills.

33 er hydrochlorides and potassium cyanate in a planetary ball-mill is described.

34 ned a major role as antifreeze in giving icy planetary bodies (e.g., Titan) a liquid subsurface ocean

35 re essential for scientific investigation of planetary bodies and are therefore ubiquitous on mission

36 plays an important role in the evolution of planetary bodies and atmospheres.

37 substantial process during crustal growth on planetary bodies and well documented to have occurred in

38 achyandesites on Earth, also formed on small planetary bodies approximately 4.56 billion years ago.

39 n whether the notable volatile depletions of planetary bodies are a consequence of accretion or inher

40 cognized that Earth and other differentiated planetary bodies are chemically fractionated compared to

41 pic compositions of the main constituents of planetary bodies can contribute to this debate.

42 Knowledge of the magnetization of planetary bodies constrains their origin and evolution,

43 tem, the molten metallic cores of many small planetary bodies convected vigorously and were capable o

44 e nature and extent of volatile-depletion of planetary bodies during the earliest stages of Solar Sys

45 itentes have been identified conclusively on planetary bodies other than Earth.

46 lutionary course of our Solar System and the planetary bodies within it.

47 ng of reduced carbon from Fe-rich basalts on planetary bodies would produce methane-bearing, CO-rich

48 a major contributor of volatile elements to planetary bodies, and could have played a key role in th

49 ces of the major elements of Earth and other planetary bodies, are a natural consequence of substanti

50 is critical for modeling collisions between planetary bodies, interpreting the significance of shock

51 r organisms which, when transported to other planetary bodies, pose a contamination risk.

52 Chemical evolution of planetary bodies, ranging from asteroids to the large ro

53 istory has implications for the formation of planetary bodies, the delivery of water to the inner Sol

54 At temperatures characteristic of icy planetary bodies, vapor deposits of methanol, water, and

55 and hydrosphere, and water on Mars and other planetary bodies.

56 lications for understanding the evolution of planetary bodies.

57 floodplains of the Moon and Venus, and other planetary bodies.

58 of shallow density anomalies on terrestrial planetary bodies.

59 the formation, evolution and habitability of planetary bodies.

60 re states during the formation of primordial planetary bodies.

61 available for study on Earth of a number of planetary bodies.

62 to the thermodynamic conditions found on icy planetary bodies.

63 and isotopic signatures compared with other planetary bodies; any successful model for the origin of

64 The asteroid Vesta is the smallest known planetary body that has experienced large-scale igneous

65 their source, for the first time across any planetary body, creating a novel way to probe planetary

66 onsistent with those of chondrites and other planetary body.

67 The planetary boundaries framework defines a safe operating

68 One of the planetary boundaries is determined by "chemical pollutio

69 Other chemical pollution-related planetary boundaries likely exist, but are currently unk

70 ve climate policies that comply with the two planetary boundaries related to climate change: (1) stay

71 Rockstrom et al. proposed a set of planetary boundaries that delimit a "safe operating spac

72 Rockstrom et al. proposed a set of planetary boundaries that delimitate a "safe operating s

73 Many of the planetary boundaries that have so far been identified ar

74 The "planetary boundaries" concept, and its extension through

75 cosystem services, environmental footprints, planetary boundaries, human-nature nexuses, and telecoup

76 use these have impacts reaching or exceeding planetary boundaries.

77 e of change relates to the recently proposed planetary boundary ("safe limit").

78 cal ecosystems--beyond its recently proposed planetary boundary across 58.1% of the world's land surf

79 The planetary boundary framework constitutes an opportunity

80 Here, we revise and update the planetary boundary framework, with a focus on the underp

81 ion planetary boundary, but rather that many planetary boundary issues governed by chemical pollution

82 tion at surface, surface air temperature and planetary boundary layer (PBL) height.

83 oceanic features in forcing the atmospheric planetary boundary layer (PBL).

84 nts and water vapour accumulate in a shallow planetary boundary layer (PBL).

85 We combined height of the planetary boundary layer and wind speed, which affect co

86 eased canopy and air temperatures within the planetary boundary layer compared to Koshihikari.

87 evated semi-enclosed air basin with a unique planetary boundary layer dynamic.

88 Results show that decreases in planetary boundary layer height (PBLH) resulting from th

89 Planetary boundary layer modelling is used to estimate t

90 Unlike in the planetary boundary layer, few observations of NPF in the

91 For the planetary boundary layer, global simulations indicate th

92 most plausible alternative, at least in the planetary boundary layer.

93 ays after contact of the air masses with the planetary boundary layer; this is related to the time ne

94 A chemical poses an unknown planetary boundary threat if it simultaneously fulfills

95 neously met for chemical pollution to pose a planetary boundary threat.

96 tly available to identify chemicals that are planetary boundary threats is prioritization against pro

97 e that there is no single chemical pollution planetary boundary, but rather that many planetary bound

98 Transits of a third planetary candidate are also found: a 1.7-Earth radius s

99 of CO(2) from the atmosphere is an important planetary carbon dioxide removal mechanism.

100 cycling rate of local moisture, regulated by planetary circulation patterns associated with the El Ni

101 rise that extends for approximately half the planetary circumference at mid-latitudes.

102 Modeling studies of terrestrial extrasolar planetary climates are now including the effects of ocea

103 ne that formed Imbrium, should have survived planetary collisions and contributed to the heavy impact

104 voking Kozai-Lidov oscillations, an external planetary companion drives a planet onto an orbit having

105 the CoRoT satellite that is known to host a planetary companion.

106 We present the results of a search for planetary companions orbiting near hot Jupiter planet ca

107 e context of their relevance under plausible planetary conditions.

108 e mass distribution, chemical abundances and planetary configuration of the Solar System today, but t

109 open questions for the origins of life in a planetary context.

110 nverse of the heat-pipe/mantle-plume mode of planetary cooling.

111 as quark-gluon plasmas, electrons in solids, planetary cores and charged macromolecules.

112 or instead of MgO in rocky mantles and rocky planetary cores under highly oxidized conditions.

113 is commonly found in astrophysics (e.g., in planetary cores) as well as in high energy density physi

114 the hydrothermal alteration of olivine-rich planetary crust.

115 ate vertical fluxes and increase porosity in planetary crust.

116 chronology of the formation and evolution of planetary crusts.

117 here with heat recirculation confined to the planetary dayside, or a planet devoid of atmosphere with

118 span a wide range of terrestrial, marine and planetary depositional systems, we show that the advecti

119 However, processes of planetary differentiation may also modify the isotopic c

120 the timing of core formation and other early planetary differentiation processes.

121 Accurate (182)Hf-(182)W chronology of early planetary differentiation relies on highly precise and a

122 ed to studies of igneous processes including planetary differentiation.

123 of gas can naturally be produced by a proto-planetary disc surrounding a low-mass star, which was sc

124 tic centre, and that tidal debris from proto-planetary discs can flag low-mass stars, which are other

125 m the dynamical evolution of idealized proto-planetary disks under perturbations from massive distant

126 al properties of mantle materials, governing planetary dynamics and evolution.

127 Theory famously predicts that planetary dynamo systems naturally settle into the so-ca

128 state is the natural expression of turbulent planetary dynamo systems.

129 Most analog models of planetary dynamos, however, use moderate Pr fluids, and

130 impact of the three greenhouse gases on the planetary energy budget, with a best estimate (in petagr

131 toward the synthesis of ribonucleotides in a planetary environment.

132 lability of meteoritic organic materials for planetary environments than previously assumed and that

133 ly of significance in various combustion and planetary environments.

134 Understanding the role of biology in planetary evolution remains an outstanding challenge to

135 e exploration missions (i.e., Venus &Jupiter planetary exploration, and heliophysics missions) and ea

136 tudy of a wide range of phenomena, including planetary formation and asteroid impact sites, the forma

137 e in some of the most enigmatic processes of planetary formation by mediating the rapid accretion of

138 ry disk, would constrain a critical phase of planetary formation by unveiling the unknown planetesima

139 During planetary formation, we explore scenarios leading to fur

140 y of systems from intercellular transport to planetary formation.

141 nd characteristic spectral features from the planetary geological surface and subsurface which are de

142 are powerful indicators of a wide variety of planetary geophysical processes, and for Mars they revea

143 several overarching themes that emerge from planetary health and suggest advances in the way we trai

144 e attributed to the SPNA as one of the major planetary heat sinks.

145 s the contribution of continental growth and planetary hydrogen loss to the secular evolution of hydr

146 ns during haze episodes would have expedited planetary hydrogen loss, with a single episode of haze d

147 reassessment because chemical reactivity of planetary ices is underestimated.

148 pretative tools with which to retrieve vital planetary information.

149 The evolution of the planetary interior during plate tectonics is controlled

150 e study of the evolution and dynamics of the planetary interiors as well as to the fundamental unders

151 d determining its origin and distribution in planetary interiors has important implications for under

152 ctive generation of magnetic fields in fluid planetary interiors is known as the dynamo process.

153 Degassing of planetary interiors through surface volcanism plays an i

154 ties and compressibility of, e.g., fluids in planetary interiors, and is a prerequisite for the prepa

155 anding Warm Dense Matter (WDM), the state of planetary interiors, is a new frontier in scientific res

156 nce of which can profoundly change models of planetary interiors, where high pressure reigns.

157 rtant role in magma transport in terrestrial planetary interiors.

158 es for our understanding of dense matter and planetary interiors.

159 (2) and potential implications for Earth and planetary interiors.

160 eratures and pressures reflect the nature of planetary interiors.

161 nstrumental suites on robotic spacecraft and planetary landers; this necessitates robust and reliable

162 ge terrestrial planets with implications for planetary magnetic-field generation in silicate magma la

163 These waves are important not only in planetary magnetospheres, heliospheres and astrophysical

164 regions and blurring the distinction between planetary mantles and cores.

165 h a millisecond pulsar, a white dwarf, and a planetary-mass object in an orbit of several decades), s

166 A handful of free-floating planetary-mass objects have been discovered by infrared

167 tailed follow-up observations to measure the planetary masses or to study their atmospheres.

168 ied by the observed transit times permit the planetary masses to be measured, which is key to determi

169 provide precise, but complex, constraints on planetary masses, densities, and orbits, even for planet

170 havior of carbon dioxide (CO2), an important planetary material found in Venus, Earth, and Mars, is v

171 identifying multi-stage events from complex planetary materials is highly challenging at the length

172 t have low abundances in most geological and planetary materials.

173 substantial mixing through processes such as planetary migration and the subsequent dynamical process

174 t Jupiters') can largely be accounted for by planetary migration associated with viscous evolution of

175 ation of the transition line is relevant for planetary models.

176 rrectly infers the phase space structure for planetary motion, avoids overfitting in a biological sig

177 n associated with viscous evolution of proto-planetary nebulae.

178 e and cost-effective measures to avoid these planetary nitrogen burdens and the necessity to remediat

179 variability in iron isotopic composition in planetary objects cannot be due to core formation.

180 We expect all airless planetary objects to be immersed in similar tenuous clou

181 at the stellar spin axis and the axis of the planetary orbit coincide, the minimum spectroscopic mass

182 d aid in experimental detection of these CPP planetary orbit complexes.

183 Yet the secular evolution of the planetary orbits beyond 50 million years ago remains hig

184 e degree of coplanarity and proximity of the planetary orbits imply energy dissipation near the end o

185 for misalignment-driven mechanisms to modify planetary orbits, and that these conditions are present

186 guaranteed: dynamical interactions may tilt planetary orbits, or stars may be misaligned with the pr

187 cts to realign the stellar spin axis and the planetary orbits, the fraction of planetary systems (inc

188 and the evolution of Earth's atmosphere via planetary outgassing.

189 re haze development played a pivotal role in planetary oxidation, hastening the contingent biological

190 gest that most fluid compounds, e.g., strong planetary oxides, reach a common state on the universal

191 iety of non-trivial structures attributed to planetary perturbations and used to constrain the proper

192 terizing the gravitational effects of mutual planetary perturbations for hundreds of planets.

193 With planetary perturbers, the inner orbit's angular momentum

194 of great interest for fundamental research, planetary physics, and energy applications.

195 bservational constraint is available for the planetary population surrounding ultracool dwarfs, of wh

196 The proportion of planetary primary production by diatoms in the modern oc

197 g to subsequent fractionation by nebular and planetary processes.

198 sition of Earth's mantle control fundamental planetary properties, including the vigor of mantle conv

199 , a knowledge-based and effective policy for planetary protection is essential.

200 ntrolled cleanrooms to ensure the demands of planetary protection.

201 radiation and may play an important role in planetary radiative forcing and climate.

202 We find that the difference between the planetary radius measured at optical and infrared wavele

203 However, the role that planetary redox evolution has played in controlling the

204 edge of these ancient microbial mediators in planetary redox evolution.

205 heir dust streams are regular occurrences in planetary rings, altering them in ways that remain detec

206 topic fractionation during volatilization in planetary rocks, but is hardly fractionated during terre

207 e dominated by the controlling influences of planetary rotation and magnetic fields through the Corio

208 Although planetary rotation is considered to be important for par

209 the Earth's system are intricately linked to planetary scale processes, and precise characterization

210 The plausibility of a planetary-scale 'tipping point' highlights the need to i

211 China but highlight the fundamental role of planetary-scale atmospheric dynamics in the sensitivity

212 n react in the same way and is approaching a planetary-scale critical transition as a result of human

213 rbance [2-4], underpinning key regional- and planetary-scale functions [5, 6].

214 l theory, despite being different from other planetary-scale habitats.

215 or the generation of persistent longitudinal planetary-scale high-amplitude patterns of the atmospher

216 shadowing, and three of the six known giant planetary-scale storms have developed in it.

217 tion is dominated by beat patterns caused by planetary-scale wave pairs and by a small number of brig

218 ara seas, enhances the upward propagation of planetary-scale waves with wavenumbers of 1 and 2, subse

219 cadal changes and the overriding controls on planetary scales.

220 exceptional windows into impact processes at planetary scales.

221 f astrophysical systems from cosmological to planetary scales.

222 y ranging from inertially confined fusion to planetary science and medicine.

223 , and implications for general chemistry and planetary science are also discussed.

224 s, and a prominent goal in geomorphology and planetary science is to determine formation processes fr

225 eceiving much attention in the materials and planetary science literature.

226 ich is of fundamental importance in physics, planetary science, and astrophysics.

227 Because of applications to planetary science, inertial confinement fusion and funda

228 in the dense liquid, due to its relevance to planetary science.

229 n, environmental monitoring, geophysics, and planetary science.

230 rent interest for warm dense matter physics, planetary sciences, and inertial fusion energy research.

231 on-hydrogen system is of great importance to planetary sciences, as hydrocarbons comprise a significa

232 roblems across many disciplines in earth and planetary sciences, including paleoclimatology, sediment

233 rity, we integrate the physical insight from planetary sciences, the liquid marble model from fluid m

234 iour of confined fluids relevant to geo- and planetary sciences.

235 ical processes involving negative ions among planetary scientists.

236 hape provides a new tool for terrestrial and planetary sedimentology.

237 Large planetary seedlings, comets, microscale pharmaceuticals,

238 The low-degree gravity field, combined with planetary spin parameters, yields the moment of inertia

239 past two decades offer a new perspective on planetary structure.

240 undant form of condensed matter in our solar planetary structure.

241 lanetary body, creating a novel way to probe planetary surface characteristics.

242 the most prominent criteria associated with planetary surface habitability.

243 ns terrestrial life and consists of the thin planetary surface layer between unaltered rock and the a

244 ives of environmental conditions and ancient planetary surface processes that led to their formation.

245 ersal palaeohydraulic reconstruction tool on planetary surfaces and allow for quantitative identifica

246 nderstanding the ways in which floods modify planetary surfaces, the hydrology of early Mars and abru

247 formation in heterogeneous thin films or on planetary surfaces-have been characterized experimentall

248 ds and comets that have pummeled terrestrial planetary surfaces.

249 live in urban areas, a critical question for planetary sustainability is how the size of cities affec

250 ons to be made between material from another planetary system and from our own.

251 The most common class of planetary system detectable today consists of one or mor

252 solar system are merely possible outcomes of planetary system formation and evolution, and conceivabl

253 ar disk with a radius of 90 AU, from which a planetary system is expected to form.

254 0.05 solar masses, which is enough to form a planetary system like our own.

255 ould be the end state of a secularly chaotic planetary system reminiscent of the solar system.

256 show that the solar nebula that spawned our planetary system was rich in water and organic molecules

257 moons with Kepler (HEK) project, we report a planetary system with two confirmed planets and one cand

258 preserved material from the beginning of our planetary system.

259 nes of its planets traces the history of the planetary system.

260 characterizing the components of this nearby planetary system.

261 is and the planetary orbits, the fraction of planetary systems (including systems of 'hot Neptunes' a

262 hose that take place during the formation of planetary systems and galaxies.

263 sent yet another new and unexpected class of planetary systems and provide an opportunity to test the

264 We suggest that extrasolar planetary systems are also organized to a large extent b

265 As most planetary systems are expected to experience outbursts c

266 rst exoplanets, it has been known that other planetary systems can look quite unlike our own.

267 With more detections, such binary-star planetary systems could constrain models of planet forma

268 e differences between hot Jupiters and other planetary systems denote a distinctly different formatio

269 ormation that can account for the variety of planetary systems discovered so far.

270 t the typical characteristics of planets and planetary systems for planets with sizes as small as, an

271 The statistics of extrasolar planetary systems indicate that the default mode of plan

272 The key feature of these planetary systems is an isolated, Earth-sized planet wit

273 The existence of water in extrasolar planetary systems is of great interest because it constr

274 Accounting for detection efficiency, such planetary systems occur with a frequency similar to the

275 dwarfs, suggests that rocky debris from the planetary systems of white-dwarf progenitors occasionall

276 tside it, despite models of the formation of planetary systems suggesting that orbital migration of g

277 tary masses, densities, and orbits, even for planetary systems with faint host stars.

278 ts on the formation and orbital evolution of planetary systems with low-mass planets.

279 mportant ingredients in the formation of all planetary systems, including our own.

280 sently, we have limited knowledge about such planetary systems, mostly about their sizes and orbital

281 dd an important constraint on simulations of planetary systems, since they must be able to reproduce

282 riance in the probability of life arising in planetary systems.

283 a key ingredient regulating the structure of planetary systems.

284 terstellar ices are available to all nascent planetary systems.

285 on is exploring the diversity of planets and planetary systems.

286 es that close binary stars can host complete planetary systems.

287 ttle into disks that eventually give rise to planetary systems.

288 o habitable exoplanets and exomoons in other planetary systems.

289 hat such compounds might also exist in other planetary systems.

290 lling whether the Solar System is typical of planetary systems.

291 dominant mechanism of the formation of such planetary systems.

292 expectations for Antarctic amplification of planetary temperature changes.

293 global topography is more subdued, allowing planetary temperatures to vary depending on the global d

294 ases will produce absorption features in the planetary thermal spectrum.

295 ons of the Rossiter-McLaughlin effect during planetary transits have revealed that a considerable fra

296 of ~150,000 stars, searching for evidence of planetary transits.

297 on to the atmosphere, it could drive further planetary warming.

298 her show that resonance conditions for these planetary waves were, in many cases, present before the

299 highly magnified quasistationary midlatitude planetary waves with zonal wave numbers m = 6, 7, and 8.

300 tant role of the QRA mechanism in amplifying planetary waves, favoring recent NH weather extremes.