ライフサイエンスコーパス: planet

1 star is perpendicular to the surface of the planet).

2 epresent the most abundant life forms on the planet.

3 or governs the long-term habitability of the planet.

4 photosphere along the chord transited by the planet.

5 y unknown in the evolutionary history of our planet.

6 fundamental role in maintaining life on our planet.

7 dvantage that those species now dominate the planet.

8 tern in the ecology and paleo-ecology of our planet.

9 ses, play a key role in the evolution of the planet.

10 omposition and maintaining a life-supporting planet.

11 the most widespread coastal ecosystem on the planet.

12 r one of the most important resources on the planet.

13 to increase food production for the growing planet.

14 ems, no single approach will safely feed the planet.

15 ing and sustainability on a highly urbanized planet.

16 ive and widespread coastal ecosystems on the planet.

17 ressure-temperature-composition range of the planet.

18 Agriculture dominates the planet.

19 hotspots are unevenly distributed across the planet.

20 ystems-level understanding of our remarkable planet.

21 studied and best understood organism on the planet.

22 shaping the environmental trajectory of the planet.

23 genetics of millions of other species on the planet.

24 chitin, the most abundant biopolymer on the planet.

25 act ranging from individual organisms to the planet.

26 ally reordering the structure of life on our planet.

27 o limit emissions and further warming of the planet.

28 oes not spread to surrounding regions of the planet.

29 a profound impact on the habitability of the planet.

30 is the diverse microbial life that spans the planet.

31 tlook is similar to that for the rest of the planet.

32 l fluctuations caused by the rotation of the planet.

33 tionship on a rapidly urbanizing, yet finite planet.

34 evolution and potential habitability of the planet.

35 re among the most vulnerable habitats on the planet.

36 y formation in surface environments of rocky planets.

37 to more hospitable volatile-rich Earth-sized planets.

38 ion environments of the exoplanets and outer planets.

39 importance to the evolution and dynamics of planets.

40 t stars induced by the influence of orbiting planets.

41 rest to the atmospheric chemistry of several planets.

42 entually seed the origins of life on nascent planets.

43 em but may be common for close-in extrasolar planets.

44 because of the challenges of observing small planets.

45 l laboratory to test models of jets in giant planets.

46 scale" abiogenesis probabilities on suitable planets.

47 erally smaller and less massive than gaseous planets.

48 dels of aeolian processes on the terrestrial planets.

49 ay result from gravitational perturbation by planets.

50 pheric ion escape rates for all of the seven planets.

51 d to investigate atmospheres and climates on planets.

52 The dwarf planet (1) Ceres, the largest object in the main asteroi

53 ost numerous photosynthetic organisms on our planet [1, 2].

54 eflected starlight makes this close-in giant planet a unique study case.

55 ecord the history of the magnetic field of a planet, a key constraint for understanding its evolution

56 This planet also has a sufficiently low luminosity to be cons

57 Microbial communities inhabit our entire planet and have a crucial role in biogeochemical process

58 history of arsenic adaptation of life on our planet and imply that dissemination of genes encoding di

59 served in the ultraviolet spectrum, when the planet and its escaping atmosphere transit the star, giv

60 approximately one in six individuals on the planet and, until recently, few resources have been devo

61 mportant because of their abundance in giant planets and because of the hopes of discovering high-ene

62 re and pressure, which may exist in ice-rich planets and exoplanets.

63 arfs are massive analogs of extrasolar giant planets and may host types of atmospheric circulation no

64 bserved in the ISM and in the ionospheres of planets and moons.

65 bsorption lines are seen in clear-atmosphere planets and the weakest features are associated with clo

66 components of the interiors of the giant icy planets and their satellites, which has motivated their

67 the molecule-dominated atmospheres of other planets and, given the level of ultraviolet irradiation

68 drogen bonding is fundamental to life on our planet, and nature utilizes H-bonding in nearly all biom

69 storms are some of the most powerful on the planet, and rain gauges in this region have recorded a r

70 ell membranes on early Earth and other rocky planets, and amphiphile-mineral interactions in diverse

71 planets to systems with multiple transiting planets, and identify a population of exoplanets with a

72 s transferred and the number of life-bearing planets are also likely to be higher because of the incr

73 temperatures of 7,300-10,000 kelvin), and no planets are known to transit the even hotter B-type star

74 rved orbital-period distribution, where many planets are not in resonances.

75 The atmospheres of orbiting Earth-sized planets are observationally accessible via transmission

76 ng ultracool dwarfs, of which the TRAPPIST-1 planets are the first transiting example.

77 bow shock 60,000-100,000 km upstream of our planet, as long as the solar wind fast magnetosonic Mach

78 igin, formation and thermal evolution of our planet, as well as the composition of its interior.

79 tmospheric radiative energy balance on other planets, as on Jupiter.

80 arth-mass and super-Earth-mass free-floating planets, as predicted by planet-formation theories.

81 erall mass of the Solar System's terrestrial planets, as well as the absence of planets with a < 0.4

82 free hydrogen-dominated atmospheres for each planet at >/=10sigma levels; TRAPPIST-1 b and c are ther

83 Our maps reveal a dynamically active planet at pressures less than 2 to 3 bar.

84 he potential contribution of comets to inner-planet atmospheres are long-standing problems.

85 technique for discovering and characterizing planets beyond our solar system relies upon measurement

86 The state and evolution of planets, brown dwarfs and neutron star crusts is determi

87 role in the transport of microbes across the planet but it is often neglected as a microbial habitat.

88 statement is true, as far as we know, on our planet, but it is not clear whether it must hold through

89 of life cycle events in organisms across the planet, but the magnitude of change often varies among t

90 cal composition and thermal structure of our planet, but their origin has long been debated.

91 polar hot-spots have been observed on other planets, but detection of post-equinox cooling is so far

92 action to curb biodiversity loss across the planet by 2020-an urgent imperative.

93 interior, preserves the young surface of our planet by catalysing mantle convection, lubricating plat

94 ofuel would have on the number of people the planet can feed.

95 Unbound planets can also be formed through gravitational collaps

96 tmospheric biosignature gases from habitable planets can be detected with our current capabilities?

97 e Quarter 1-17 Data Release 24 (Q1-Q17 DR24) planet candidate catalog from NASA's Kepler mission, spe

98 The surface elemental composition of dwarf planet Ceres constrains its regolith ice content, aqueou

99 The surface of dwarf planet Ceres contains hydroxyl-rich materials.

100 The dwarf planet Ceres is known to host phyllosilicate minerals at

101 raming Camera images, of a landform on dwarf planet Ceres that we argue represents a viscous cryovolc

102 sorption feature at 3.4 micrometers on dwarf planet Ceres.

103 on on coverage and optical properties of the planet clouds contained in the measured phase curve.

104 The transiting configuration of these planets, combined with the Jupiter-like size of their ho

105 of abiogenesis is enhanced on the TRAPPIST-1 planets compared with the solar system.

106 s and the largest explosive eruptions on our planet consist of calcalkaline rhyolites.

107 Infrared radiation emitted from a planet contains information about the chemical compositi

108 rns of upwelling timing and intensity as the planet continues to warm.

109 f clay minerals and early metabolites in our planet could have been facilitated by sunlight photochem

110 We find that terrestrial planets could lose a total atmospheric mass comparable t

111 scape routes that, in turn, pushed them onto planet-crossing orbits.

112 et irradiation and ablation experienced by a planet depends strongly on the temperature of its host s

113 oximately 25% of primary productivity on the planet despite being used by only 3% of species.

114 oid may orbit stably in the same region as a planet, despite revolving around the Sun in the sense op

115 tion confined to the planetary dayside, or a planet devoid of atmosphere with low-viscosity magma flo

116 oring the entire population of free-floating planets down to Mars-mass objects, because the microlens

117 bined transmission spectrum of the two inner planets during their simultaneous transits on 4 May 2016

118 to the physical aspects of evolution on our planet Earth are also discussed.

119 ng blocks of life by meteorites or comets to planet Earth are discussed in this Perspective.

120 eutral energy schemes to be able to preserve Planet Earth for future generations to come and still pr

121 970's, the Gaia hypothesis suggests that our planet earth has a self-regulating ability to maintain a

122 On planet Earth, water is everywhere: the majority of the s

123 ight into the chemical energy that fuels the planet Earth.

124 s suggesting that orbital migration of giant planets ejects a large fraction of the original planetes

125 n the possible biological damage suffered by planets exposed to X-ray and extreme ultraviolet (XUV) r

126 Deep inside planets, extreme density, pressure, and temperature stro

127 sensing techniques used to characterize such planets for potential habitability and life rely solely

128 The six inner planets form a near-resonant chain, such that their orbi

129 cular precursors of biorelevant molecules as planets form in their interstellar nurseries.

130 organic molecules (COMs) accompany star and planet formation and may eventually seed the origins of

131 ris disks' were thought to be by-products of planet formation because they often exhibited morphologi

132 ed a critical role in the earliest stages of planet formation by mediating the accumulation of dust i

133 A key stage in planet formation is the evolution of a gaseous and magne

134 Gas-giant planet formation likely involved the growth of large sol

135 terrestrial planets has been a challenge for planet formation models.

136 tion dates to processes that occurred during planet formation remains an unanswered question.

137 On the basis of these data and our new planet formation simulations that include a realistic mo

138 e most of the mass is concentrated and where planet formation takes place.

139 Planet formation theories predict that some planets may

140 tent with the core accretion model for giant planet formation.

141 when developing models of disk evolution and planet formation.

142 esults, however, do not match predictions of planet-formation theories and surveys of young clusters.

143 -mass free-floating planets, as predicted by planet-formation theories.

144 ar System and has served as a cornerstone of planet-formation theory.

145 This architecture suggests that the planets formed farther from the star and migrated inward

146 his scenario, the Solar System's terrestrial planets formed from gas-starved mass-depleted debris tha

147 main nitrogen reservoir from which the giant planets formed.

148 ugars and amides are ubiquitous in star- and planet-forming regions, but their formation mechanisms h

149 he C-H-O system is one of the most important planet-forming systems, but its high-pressure chemistry

150 characterization of thousands of extrasolar planets from the Kepler mission, the Hubble Space Telesc

151 l for inferring processes on Earth and other planets from water isotopic measurements.

152 the beta Pictoris system, in which the known planet generates an observable warp in the disk.

153 nclude that the Imbrium impactor was a proto-planet (half the diameter of Vesta), once part of a popu

154 A temperate planet has been discovered orbiting Proxima Centauri, th

155 Our planet has been through phases of snowball (all frozen),

156 Building the terrestrial planets has been a challenge for planet formation models

157 nic compounds on Earth and other terrestrial planets has been discussed for a long time without reach

158 also destroy the habitability of water-rich planets has remained unclear.

159 The nature of these planets has yet to be determined, as their masses remain

160 Moreover, the seven planets have equilibrium temperatures low enough to make

161 PLANET I was a randomised, double-blind, parallel-group

162 Using the Gemini Planet Imager, we discovered a planet orbiting the ~20-m

163 the discovery via imaging of a young Jovian planet in a triple-star system and characterize its atmo

164 The age of Jupiter, the largest planet in our Solar System, is still unknown.

165 a major threat to the sustainability of the planet in terms of reactive nitrogen pollution.

166 Dedicated space-based monitoring of the planet in the infrared revealed a modulation of the ther

167 gest that the nearest transiting Earth-sized planet in the liquid-water, habitable zone of an M dwarf

168 have affected the habitability of Earth-like planets in our Galaxy.

169 ted in the past century from observations of planets in our own Solar System and has served as a corn

170 -magnetosphere coupling which is unusual for planets in our solar system but may be common for close-

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

172 a), once part of a population of large proto-planets in the asteroid belt.

173 isks show evidence for the presence of young planets in the form of disk asymmetries or infrared sour

174 report transit timing variations of the four planets in the Kepler-223 system, model these variations

175 urface renewal may also occur on other dwarf planets in the Kuiper belt, which may help to explain th

176 lishing the current orbits of the four giant planets in the Solar System by disrupting a theoretical

177 life was initiated by panspermia on multiple planets in the TRAPPIST-1 system.

178 e most common intracellular infection on the planet, infects 40% of insects as well as nematodes, iso

179 uld have driven any preexisting short-period planets into the Sun.

180 Our planet is an increasingly urbanized landscape, with over

181 The semimajor axis of the planet is closer relative to that of its hierarchical tr

182 The dwarf planet is dominated by numerous craters, but other featu

183 valence of tailed DNA bacteriophages on this planet is enabled by highly efficient self-assembly of h

184 ttest known transiting planet, WASP-33b; the planet is itself as hot as a red dwarf star of type M (r

185 We infer from this that the planet is surrounded and trailed by a large exospheric c

186 Characterizing rocky planets is particularly difficult, because they are gene

187 the most enigmatic physical phenomena of the planet, is constantly changing on various time scales, f

188 the Sun in the sense opposite to that of the planet itself.

189 deed a retrograde co-orbital asteroid of the planet Jupiter.

190 period of about 1.48 days) transiting giant planet, KELT-9b.

191 ermine that the mass of the Mars-sized inner planet, Kepler-138 b, is 0.066(+0.059)(-0.037) Earth mas

192 ange of mass-loss rates that could leave the planet largely stripped of its envelope during the main-

193 A correlation between giant-planet mass and atmospheric heavy elemental abundance wa

194 rge surface gravity and cool insolation, the planet may have retained its atmosphere despite the grea

195 Planet formation theories predict that some planets may be ejected from their parent systems as resu

196 in a triple system demonstrates that massive planets may be found on long and possibly unstable orbit

197 de co-orbital asteroids of Jupiter and other planets may be more common than previously expected.

198 We show that planets may survive and become misaligned from their hos

199 me scale for formation of the gas giants and planet migration.

200 l damage caused by Sgr A* to surface life on planets not properly screened by an atmosphere was proba

201 Of the thousands of extrasolar planets now known, only six have been found that transit

202 r, resulting in a reorientation of the dwarf planet of around 60 degrees with respect to the rotation

203 Thus, Jupiter is the oldest planet of the Solar System, and its solid core formed we

204 of Jupiter-mass free-floating or wide-orbit planets of 0.25 planets per main-sequence star.

205 We conclude that the outer planets of the TRAPPIST-1 system are capable of retainin

206 sional numerical experiments of a water-rich planet orbiting a double star.

207 ng the Gemini Planet Imager, we discovered a planet orbiting the ~20-million-year-old star 51 Eridani

208 The discovery of planets orbiting double stars at close distances has spa

209 a in the recently discovered system of seven planets orbiting the ultracool dwarf star TRAPPIST-1 and

210 itherto undetected population of terrestrial planets orbiting them--ranging from metal-rich Mercury-s

211 , such as those inferred for some extrasolar planets, our results also indicate that for environments

212 f multi-planet systems of sub-Neptunes, more planet pairs are observed near resonances than would gen

213 sible via transmission spectroscopy when the planets pass in front of these stars.

214 free-floating or wide-orbit planets of 0.25 planets per main-sequence star.

215 ximity to resonance enables the detection of planets perturbing each other.

216 Most creatures on this planet possess an ability to anticipate upcoming events

217 e jovian magnetosphere from bow shock to the planet, providing magnetic field, charged particle, and

218 mpletely sterilise an Earth-like planet with planet radii in the range 0.5-1.5R plus sign in circle a

219 The inner two planets receive four times and two times the irradiation

220 Here we apply this model to the terrestrial planet region and find that it can reproduce the basic s

221 raise fundamental questions about how small planets remain active many billions of years after forma

222 lation of unbound or wide-orbit Jupiter-mass planets (reported to be almost twice as common as main-s

223 an limb (that is, the observed 'edge' of the planet) represents a unique window into the complex atmo

224 es of the forcing frequencies related to the planet's as well as to the binary's orbital periods are

225 s absorbed by the atoms and molecules in the planet's atmosphere, causing the planet to seem bigger;

226 endent, and modulates the composition of the planet's atmosphere.

227 mporally, with profound implications for the planet's biodiversity and human economies.

228 -triple isotopes can be used to decipher the planet's climate history.

229 he atmosphere has a noticeable impact on the planet's climate.

230 Preserving global public goods, such as the planet's ecosystem, depends on large-scale cooperation,

231 s depleted in the protoplanetary disk at the planet's formation location, but it is unclear whether t

232 on, which has important implications for our planet's geochemical evolution and physical history.

233 mordial reservoirs that have survived in the planet's interior.

234 Still, 75% the planet's land surface is experiencing measurable human p

235 lized economy exert a major influence on the planet's land use and resources through their product de

236 between clock gene expression and one of the planet's largest daily migrations of biomass.

237 Drylands represent the planet's largest terrestrial biome and evidence suggests

238 bsurface ocean generates stresses within the planet's lithosphere, resulting in a global network of e

239 via photolysis following the collapse of the planet's magnetic field, the widespread serpentinization

240 te this, Earth's polar regions have been our planet's most environmentally constant surface regions f

241 The impact of human activities on our planet's natural systems has been intensifying rapidly i

242 sing the planet to seem bigger; plotting the planet's observed size as a function of the wavelength o

243 The planet's remaining large and ecologically important trac

244 , a phenomenon that is currently eroding the planet's richest repositories of biodiversity.

245 17, the Cassini spacecraft passed inside the planet's rings, allowing in situ measurements of the ion

246 arth's mantle, water has been present on our planet's surface for most of geological time.

247 mes of water that could be removed from each planet's surface via the burial and metamorphism of hydr

248 e Southern Ocean, which encompass 10% of the planet's surface, are excluded from assessments of progr

249 l forests account for only a fraction of the planet's terrestrial surface, they exchange more carbon

250 small integers (resonances), often in a many-planet series (chain).

251 an important role for most organisms on this planet, serving either as a source of energy or informat

252 e dominant materials accreted to terrestrial planets should therefore be higher than those seen in ca

253 Here we show with three-dimensional aqua-planet simulations that CO2-induced forcing as readily d

254 rgifera, the most damaging maize pest on the planet, specifically accumulates the root-derived benzox

255 cerol could have been dispensed to habitable planets such as early Earth by comets and meteorites.

256 Water-rich planets such as Earth are expected to become eventually

257 The composition of terrestrial planets suggests that typical planetesimals contain enou

258 Surveys have revealed many multi-planet systems containing super-Earths and Neptunes in o

259 In the hundreds of multi-planet systems of sub-Neptunes, more planet pairs are ob

260 nteractions represent only one snapshot of a planet that is continuously changing, in part due to hum

261 Saturn's A- and B-rings cast a shadow on the planet that reduced ionization in the upper atmosphere,

262 agments of asteroids, the building blocks of planets, that retain a record of primordial processes.

263 that 11 orbits remain possible for the third planet, the most likely resulting in irradiation signifi

264 In the case of the gas-giant planets, these aurorae include highly polarized radio em

265 Humans have colonized the planet through a series of range expansions, which deepl

266 th archaic hominins and dispersed across the planet through host interbreeding and gene flow.

267 impacts provide a mechanism for resurfacing planets through mixing near-surface rocks with deeper ma

268 the nightside brightness temperature of the planet to 1,380 +/- 400 kelvin and the temperature of th

269 We measure the mass of the planet to be 6.6 times that of Earth, consistent with a

270 ules in the planet's atmosphere, causing the planet to seem bigger; plotting the planet's observed si

271 them--ranging from metal-rich Mercury-sized planets to more hospitable volatile-rich Earth-sized pla

272 lly comparing systems with single transiting planets to systems with multiple transiting planets, and

273 t the effects of increasing CO2 on a warming planet, together accounting for uptake of approximately

274 ents that gave rise to the first life on our planet took place in the Earth's deep past, seemingly fo

275 spin of a star and the orbital planes of its planets traces the history of the planetary system.

276 ime interval, known as the Hadean, the young planet transformed from an uninhabited world to the one

277 Seven Earth-sized planets transit the very low-mass star TRAPPIST-1, which

278 servations of three short-period Earth-sized planets transiting an ultracool dwarf star only 12 parse

279 al question of whether the seven Earth-sized planets transiting the recently discovered ultracool dwa

280 pin-orbit alignment can be measured when the planet transits its star, but such ground-based spectros

281 tropics, with the most diverse biome on the planet treated as a single type in models.

282 to the cores of Mercury-sized to Earth-sized planets, using a dynamically laser-heated diamond-anvil

283 re Tharsis formed, when the spin axis of the planet was controlled by the difference in elevation bet

284 of TiO in the atmosphere of the hot-Jupiter planet WASP-19b.

285 in, which hosts the hottest known transiting planet, WASP-33b; the planet is itself as hot as a red d

286 Recently, three Earth-sized planets were detected that transit (that is, pass in fro

287 igration creates tightly packed systems with planets whose orbital periods may be expressed as ratios

288 ts of an ecologically functional and diverse planet will need to integrate ecological and social scie

289 rvations that reveal the presence of a small planet with a minimum mass of about 1.3 Earth masses orb

290 Here we report observations of LHS 1140b, a planet with a radius of 1.4 Earth radii transiting a sma

291 lanetary systems is an isolated, Earth-sized planet with a roughly 1-d orbital period.

292 Here we report observations of GJ 1132b, a planet with a size of 1.2 Earth radii that is transiting

293 ents that completely sterilise an Earth-like planet with planet radii in the range 0.5-1.5R plus sign

294 position has induced a reorientation of the planet with respect to its spin axis (true polar wander,

295 rrestrial planets, as well as the absence of planets with a < 0.4 AU.

296 propose that impact ejecta exchange between planets with parallel chemistries and chemical evolution

297 Our observations reveal that at least seven planets with sizes and masses similar to those of Earth

298 olific producers of calcium carbonate on the planet, with a production of approximately 10(26) coccol

299 in the reference climate, implying that the planet would be subject to substantial loss of water to

300 ry some of the largest sediment loads on the planet, yet coarse gravel in these rivers vanishes withi