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 pogenic aerosols are hypothesized to enhance planetary albedo and offset some of the warming due to t

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

6 The change in planetary albedo due to aerosol-cloud interactions durin

7 igible, we find direct evidence of increased planetary albedo primarily through increased drop concen

8 surface conditions will modify the change in planetary albedo when sea ice melts.

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

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

11 ustainable and is having negative impacts on planetary and human health.

12 ion documents need revision to consider both planetary and public health.

13 electron spectrometers that can be used for planetary and space science missions to environments of

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

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

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

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

18 observe the composition and dynamics of the planetary atmosphere.

19 nce, but equally on constituent parts of the planetary atmosphere.

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

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

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

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

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

25 latitudinal) winds dominate the bulk flow of planetary atmospheres.

26 Planetary auroras reveal the complex interplay between a

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

28 dant form of volcanism on Earth and on other planetary bodies and satellites.

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

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

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

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

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

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

35 u evidence of impacts on boulders on airless planetary bodies has come from Apollo lunar samples(6) a

36 nerals are widespread on Earth and likely in planetary bodies in and beyond our solar system.

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

38 gnetic data(9), and especially in studies of planetary bodies that no longer have a dynamo(10), such

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

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

41 one of the most fundamental constituents in planetary bodies, being an essential building block of m

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

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

44 re states during the formation of primordial planetary bodies.

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

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

47 the formation, evolution and habitability of planetary bodies.

48 to the thermodynamic conditions found on icy planetary bodies.

49 nditions for different evolutionary paths of planetary bodies.

50 es, which in turn are primitive fragments of planetary bodies.

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

52 differentiation of a carbonaceous chondritic planetary body, bridging a previously persistent gap in

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

54 ation at static pressures >20 GPa in a large planetary body, like diamonds formed deep within Earth's

55 onsistent with those of chondrites and other planetary body.

56 , five food-related per capita environmental planetary boundaries (carbon emissions, water, land, nit

57 n B12, vitamin E, and saturated fats and the planetary boundaries for carbon emissions and nitrogen a

58 The planetary boundaries framework defines a safe operating

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

60 recommendations or transgress environmental planetary boundaries or both.

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

62 Sustainability within planetary boundaries requires concerted action by indivi

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

64 l pollution has been mentioned as one of the planetary boundaries within which humanity can safely op

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

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

67 eatening to push the Earth system beyond its planetary boundaries, risking catastrophic and irreversi

68 joy sufficient well-being and avoid crossing planetary boundaries.

69 use these have impacts reaching or exceeding planetary boundaries.

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

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

72 The planetary boundary framework constitutes an opportunity

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

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

75 Simulation of the planetary boundary layer (PBL) is key for forecasting ai

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

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

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

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

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

81 Planetary boundary layer modelling is used to estimate t

82 bution of the HDO/H(2)O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilomet

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

84 For the planetary boundary layer, global simulations indicate th

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

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

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

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

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

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

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

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

93 ng metal-silicate partitioning (analogous to planetary core formation) over a large range of oxygen f

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

95 ty and length scale-are poorly quantified in planetary cores owing to the strong dependence of these

96 Although modelling the conditions of larger planetary cores remains out of reach, the fact that the

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

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

99 to large uncertainties in the properties of planetary cores.

100 gm involves the growth of a relatively mafic planetary crust over the first 1 to 2 billion years of E

101 ate vertical fluxes and increase porosity in planetary crust.

102 chronology of the formation and evolution of planetary crusts.

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

104 ition of this disk is unlike all other known planetary debris around white dwarfs(7), but resembles p

105 As the effect of planetary differentiation on the behavior of N isotopes

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

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

108 ed to studies of igneous processes including planetary differentiation.

109 t document incipient melting at the onset of planetary differentiation.

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

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

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

113 iversity that rivals the complexity of other planetary ecosystems.

114 -on collision (giant impact) between a large planetary embryo and the proto-Jupiter could have shatte

115 The acquisition of nebular gases requires planetary embryos to grow to sufficiently large mass bef

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

117 doreductase, is of central importance in the planetary energy cycle.

118 changes in the climate system can alter the planetary energy fluxes.

119 year between 1991 and 2016, equivalent to a planetary energy imbalance of 0.80 +/- 0.49 W watts per

120 toward the synthesis of ribonucleotides in a planetary environment.

121 ly of significance in various combustion and planetary environments.

122 ~ 10(4) to ~ 10(9) Hz after passage through planetary environments.

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

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

125 ated ME analysis of soil samples relevant to planetary exploration.

126 ure search and selection of landing sites in planetary exploration.

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

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

129 um) in tracking the late accretion stages of planetary formation has long been recognized.

130 tes(2,3) and are essential for understanding planetary formation processes.

131 During planetary formation, we explore scenarios leading to fur

132 in ureilite meteorites is a timely topic in planetary geology as recent studies have proposed their

133 rent diets are detrimental to both human and planetary health and shifting towards more balanced, pre

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

135 iverse natural environments are dependent on planetary health, which should be a priority also among

136 d food system, as that will also help ensure planetary health.

137 rganisms that are of pressing importance for planetary health.

138 Earth's mantle convection, which facilitates planetary heat loss, is manifested at the surface as pre

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

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

141 pretative tools with which to retrieve vital planetary information.

142 kton diversity and ecology in the ocean as a planetary, interconnected ecosystem.

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

144 nriched by water or other volatiles from the planetary interior.

145 Retention of nebular gases by planetary interiors also constrains the dynamics of outg

146 Superdense plasmas widely exist in planetary interiors and astrophysical objects such as br

147 Volcanic degassing of planetary interiors has important implications for their

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

149 Evidence for the capture of nebular gases by planetary interiors would place important constraints on

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

151 mixture at the high-pressure environment of planetary interiors, in particular, for non-crystalline

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

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

154 tanding the seismic and dynamic structure of planetary interiors.

155 y processes provide a route to understanding planetary interiors.

156 rtant role in magma transport in terrestrial planetary interiors.

157 al species and the primary energy source for planetary magnetic fields.

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

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

160 neration of chorus waves in other magnetized planetary magnetospheres.

161 osition of atmospheres while factors such as planetary mass, thermal state, and age mainly affect the

162 an [Formula: see text] per cent of the total planetary mass.

163 d as evidence of planet formation(1-3), with planetary-mass bodies carving rings and gaps in the disk

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

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

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

167 ue against any major contribution of EC like planetary materials in Earth's accretion.

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

169 n carbonaceous chondrites and differentiated planetary materials, suggesting the existence, perhaps e

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

171 chnology that could be implemented on future planetary missions.

172 Using a novel ecosystem-planetary model, we find that pre-photosynthetic methane

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

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

175 giant branch (AGB) star into a nonspherical planetary nebula (PN) could be due to binary interaction

176 at a wavelength of 149.1 micrometres in the planetary nebula NGC 7027.

177 eometries with morphological similarities to planetary nebulae (PNe).

178 In particular, the conditions in planetary nebulae were shown to be suitable for producin

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

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

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

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

183 Planetary orbit, specifically the condition of perpetual

184 Our Stability of Planetary Orbital Configurations Klassifier (SPOCK) pred

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

186 discrete field theory from a set of data of planetary orbits similar to what Kepler inherited from T

187 e serving algorithm correctly predicts other planetary orbits, including parabolic and hyperbolic esc

188 rometer (FIPS), which detected heavy ions of planetary origin that were recently ionized, and "picked

189 The next step to understand planetary origins in our Solar System requires a mission

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

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

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

193 led C-P-O-Fe cycles that can lead to runaway planetary oxygenation as rising atmospheric pO(2) sweeps

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 It does however exacerbate certain planetary pressures, largely by stimulating additional b

197 iofuel policy, however, it can alleviate all planetary pressures.

198 ry world, since it can ameliorate many other planetary pressures.

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

200 g to subsequent fractionation by nebular and planetary processes.

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

202 ically recovered from Mars spacecraft during planetary protection bioburden screenings.

203 r Mars exploration in terms of rover safety, planetary protection during rover operations, and the cu

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

205 ntrolled cleanrooms to ensure the demands of planetary protection.

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

207 vative of this quantity must be equal to the planetary radiative imbalance.

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

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

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

211 thermal evolution, volatile compositions and planetary redox states(1-7).

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

213 Although planetary rotation is considered to be important for par

214 the strong dependence of these properties on planetary rotation, buoyancy driving and magnetic fields

215 rely determined by the flow velocity and the planetary rotation.

216 re and 100 km in the ocean, smaller than the planetary scale and the typical extent of ocean basins,

217 ratosphere by enhanced upward propagation of planetary-scale atmospheric waves.

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

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

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

221 A planetary-scale understanding of the ocean ecosystem, pa

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

223 the positive STWCPSST anomaly and subsequent planetary-scale wave propagation act to increase the Arc

224 Other planetary-scale waves and large-scale turbulence act in

225 f astrophysical systems from cosmological to planetary scales.

226 occur in several astrophysical scenarios and planetary science [Drake R (2005) Plasma Phys Controlled

227 ities across scientific disciplines, such as planetary science and astronomy, each of which are grapp

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

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

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

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

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

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

234 material on Mars is a major issue in modern planetary science.

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

236 ems, material sciences, medicinal chemistry, planetary sciences, and biochemistry.

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

238 f technical disciplines, including earth and planetary sciences, environmental monitoring, bioremedia

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

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

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

242 ical processes involving negative ions among planetary scientists.

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

244 a measure of rock oxidation that influences planetary structure and evolution.

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

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

247 y consistent with gradual oxygenation of the planetary surface after the evolution of oxygenic photos

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

249 the most prominent criteria associated with planetary surface habitability.

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

251 missions have searched for molecular life on planetary surfaces beyond Earth.

252 returned samples underpins age estimates for planetary surfaces throughout the inner Solar System and

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

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

255 de information about the geologic history of planetary surfaces.

256 llenging to quantify how the architecture of planetary sysems is affected by these environmental proc

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

258 simulations to demonstrate that the GJ 3512 planetary system challenges generally accepted formation

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

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

261 ences (with p values of 10(-5) to 10(-2)) in planetary system properties between phase space overdens

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

263 y) determine the properties of the resulting planetary system(4).

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

265 characterizing the components of this nearby planetary system.

266 preserved material from the beginning of our planetary system.

267 een two large planetesimals in an extrasolar planetary system.

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

269 As most planetary systems are expected to experience outbursts c

270 However, (proto)planetary systems are predicted(5,6) and observed(7,8) t

271 12) and demonstrate that the architecture of planetary systems exhibits a strong dependence on local

272 ause these are the environments in which new planetary systems form, some of the chemical species mad

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

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

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

276 ilar events should be very rare in quiescent planetary systems of the age of Fomalhaut, suggesting th

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

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

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

280 s in the Solar System is typical among other planetary systems.

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

282 o habitable exoplanets and exomoons in other planetary systems.

283 dominant mechanism of the formation of such planetary systems.

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

285 is a key factor setting the architectures of planetary systems.

286 smaller bodies, implying that they may host planetary systems.

287 expectations for Antarctic amplification of planetary temperature changes.

288 s, and the importance of better constraining planetary temperature profiles.

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

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

291 Plastic pollution is a planetary threat, affecting nearly every marine and fres

292 s regarding the longevity of such sources on planetary timescales-and whether any survive today-remai

293 and vapor loss of lighter Si isotopes during planetary volatilization were also influential in establ

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

295 , we suggest that airborne dust can postpone planetary water loss at the inner edge of the habitable

296 spheric polar vortex by enhancing the upward planetary wave propagation, and thereby affecting both s

297 The episodes generate planetary waves and higher-frequency wave trains that tr

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.