ライフサイエンスコーパス: planet

1 that TOI-849b is the remnant core of a giant planet.

2 govern variation in biodiversity across the planet.

3 rations, and the current habitability of the planet.

4 f the most abundant natural resources on our planet.

5 ributed unidirectional growth process on the planet.

6 habiting the largest ecological realm on the planet.

7 o make them a consequential component of the planet.

8 rve these unique communities in our changing planet.

9 into the thermal history and rheology of the planet.

10 the most rapidly changing ecosystems on the planet.

11 d are among the predominant organisms on the planet.

12 omogenized vegetation in savannas across the planet.

13 re samples from inaccessible portions of our planet.

14 ic factory that eventually fuels life on our planet.

15 ratio of diabetes is found risky across the planet.

16 ogeochemistry, food webs, and climate of our planet.

17 out the survival of coral reefs in a warming planet.

18 eases and infect all living organisms on the planet.

19 the global intertwined system of people and planet.

20 epresent the most abundant life forms on the planet.

21 chitin, the most abundant biopolymer on the planet.

22 act ranging from individual organisms to the planet.

23 the most widespread coastal ecosystem on the planet.

24 ally reordering the structure of life on our planet.

25 o limit emissions and further warming of the planet.

26 oes not spread to surrounding regions of the planet.

27 to diamond-forming processes at depth in the planet.

28 t is dissociated to hydrogen and escapes the planet.

29 crobes are the most diverse organisms on the planet.

30 ocean, the largest inhabitable space on the planet.

31 abiota-the largest animals and plants on the planet.

32 water could exist on the surface of a rocky planet.

33 -driven instabilities over vast areas of the planet.

34 marks a major expansion of humans across the planet.

35 inhabitant of aquatic ecosystems across the planet.

36 one of the most pressing problems facing our planet.

37 to retain the last intact ecosystems on the planet.

38 ognizable and common microbial smells on the planet.

39 the largest and least explored biome on the planet.

40 upper atmosphere and at the surface of other planets.

41 of the interior and atmospheres of Gas Giant planets.

42 ant materials in the interiors of water-rich planets.

43 s on Earth that offer clues to life on other planets.

44 forward and back contamination of exploring planets.

45 initial structure and long-term evolution of planets.

46 be the internal structure of Earth and other planets.

47 ental physical process in the fluid cores of planets.

48 the deep interior of large, rocky extrasolar planets.

49 vironments of the Earth and other magnetized planets.

50 lectrons near the Earth and other magnetized planets.

51 ssembly and ensuing evolution of terrestrial planets.

52 ion environments of the exoplanets and outer planets.

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

54 l cycle, and dynamo generation in water-rich planets.

55 Dawn mapping of dwarf planet (1) Ceres has identified similar deposits within

56 hases in the crust and mantle of terrestrial planets (1-10 M(E)).

57 opogenic noise and night lighting across our planet(1,2) is of increasing conservation concern(3-6).

58 rth to develop oceans and become a habitable planet(1-4).

59 h a composition similar to that of ice giant planets(14) demonstrated that massive planets might also

60 ultivariate logistic regression model in the PlaNet-2 data to predict baseline risk of major bleeding

61 his heterogeneity of treatment effect in the PlaNet-2 trial, to investigate whether all preterm neona

62 The Platelets for Neonatal Thrombocytopenia (PlaNeT-2) trial reported an unexpected overall benefit o

63 some of the best-preserved ecosystems on the planet(3) and to intact ecological gradients-from mangro

64 at have been argued to be opened by embedded planets(4-7): these flows bear a striking resemblance to

65 er atmosphere, which cooled and darkened the planet-a scenario known as an impact winter.

66 heories, and that it puts constraints on the planet accretion and migration rates.

67 Today, the planet again faces the challenge of how to provide peopl

68 Whether or not planets already exist in the disk of IRS 63, it is clear

69 bundant oxygen-generating phototrophs on our planet and are therefore important to life.

70 fe, being the defining characteristic of our planet and even our body.

71 ed from aeolian transport to move across the planet and find suitable habitats to thrive and evolve.

72 is the most extensive magmatic system on our planet and is the site of 75 per cent of Earth's volcani

73 ni mission, the spacecraft dived between the planet and its innermost ring, at altitudes of 2600 to 3

74 had a critical role in the evolution of our planet and the development of life and sustainability of

75 to determine the gravitational field of the planet and the mass of its rings.

76 oviruses exist in aquatic systems around the planet and they infect certain eukaryotic green algae th

77 rigation water needs will change in a warmer planet and where freshwater will be locally available to

78 As seismic activity is also present on other planets and moons in our solar system the mechanism eluc

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

80 y or transit-duration measurements for small planets and within a factor of a few of systems that exh

81 of the most diverse groups of animals on our planet, and exhibit an equally wide array of fascinating

82 are the most abundant large carnivore on the planet, and their ubiquity has led to concern regarding

83 ons in the Earth's magnetosphere, magnetized planets, and laboratory plasmas, play an important role

84 insulating and metallic layers in giant gas planets, and reconciles existing discrepancies between e

85 ral occurrence on Earth and extraterrestrial planets, and their significant applications in sustainab

86 e very low and low influence portions of the planet are comprised of cold (e.g., boreal forests, mont

87 s to demonstrate that many intermediate-size planets are "water worlds."

88 The planets are interior to, but close to the inner edge of,

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

90 Theoretical models predict that these planets are more vulnerable to atmospheric loss than the

91 The surfaces of rocky planets are mostly covered by basaltic crust, but Earth

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

93 We report the discovery of a giant planet around the very-low-mass star GJ 3512, as determi

94 omical units and 154 days, respectively, for planets around field stars.

95 Detection of newly formed planets around such a star is challenged by the presence

96 motivating the search for smaller transiting planets around white dwarfs.

97 n provided a close-up study of the gas giant planet, as well as its rings, moons, and magnetosphere.

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

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

100 ally driven environmental changes affect our planet at an unprecedented rate.

101 physiography, tectonics, and climate of our planet at the dawn of life.

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

103 The transiting planet, AU Mic b, has an orbital period of 8.46 days, an

104 Just because we have knocked our planet away from a stable state, doesn't mean we have to

105 hat volcanic degassing is most efficient for planets between 2 and 4 Earth masses.

106 hest preference for geoengineering cools the planet beyond what is socially optimal at the expense of

107 Identification of habitable planets beyond our solar system is a key goal of current

108 he evolution of the disk-such as movement of planet-building material from volatile-rich regions to t

109 c cooling in upwardly moving air like on our planet, but from a circulation-induced enrichment of gas

110 able of sustaining health and protecting the planet, but it did not assess dietary affordability.

111 y the largest reservoir of carbon (C) in the planet, but its C abundance has been poorly constrained

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

113 it the longest terrestrial migrations on the planet, but, over the course of a year, gray wolves move

114 Unbound planets can also be formed through gravitational collaps

115 r the WD 1856+534 system indicate that giant planets can be scattered into tight orbits without being

116 e differentiation events for the terrestrial planets can be traced with the short-lived (146)Sm-(142)

117 If planets can form within the warped disk, disk tearing co

118 hite dwarfs, but it is unclear whether these planets can survive the journey.

119 be engulfed by the star(2), but more distant planets can survive this phase and remain in orbit aroun

120 The planet candidate is roughly the same size as Jupiter and

121 f or stellar companions) and low mass of the planet candidate make common-envelope evolution less lik

122 dic dimming of the white dwarf caused by the planet candidate passing in front of the star in its orb

123 Here we report the observation of a giant planet candidate transiting the white dwarf WD 1856+534

124 Our observations of a planet co-existing with a debris disk offer the opportun

125 ts once-abundant water to space, leaving the planet cold and dry.

126 ss loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial

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

128 mportant given that most biodiversity on the planet consists of ectotherms whose body temperature dep

129 The planet could have been a gas giant before undergoing ext

130 xt of the global-scale biome crisis that our planet currently faces.

131 e most charismatic animals and plants of the planet, data show that marine species are better at trac

132 r megafauna species globally from the Living Planet Database and available literature, and distributi

133 r 2000 vertebrate species part of the Living Planet Database.

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

135 ear to have been a persistent feature of our planet despite singular changes in its terrestrial biota

136 ts of top-of-canopy height with thousands of Planet Dove satellite images into a random forest machin

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

138 gst the most rapidly changing regions of the planet during the second half of the Twentieth Century.

139 On tidally-locked planets, dust cools the day-side and warms the night-sid

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

141 lic hydrogen and on convective mixing as the planet evolves(11,12).

142 On a planet experiencing global environmental change, the gov

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

144 n Arabia can provide important lessons for a planet facing catastrophic global warming and environmen

145 onomies (for financial networks) or even the planet (for ecosystems).

146 to test the predictions of current models of planet formation and evolution.

147 umstellar disk of gas and dust, within which planet formation can occur.

148 Planet formation is generally described in terms of a sy

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

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

151 This implies that planet formation may already be underway in even younger

152 uctures are often interpreted as evidence of planet formation(1-3), with planetary-mass bodies carvin

153 redicted to occur during the early stages of planet formation(8-12).

154 as predicted by the core accretion theory of planet formation.

155 hanged our view of the processes involved in planet formation.

156 uld place important constraints on models of planet formation.

157 Asteroids, comets and moons are leftovers of planet formation.

158 ust-grain growth, which is a prerequisite of planet formation.

159 Planet-formation models indicate that most heavy element

160 in the disk of IRS 63, it is clear that the planet-formation process begins in the initial protostel

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

162 ar phases, earlier than predicted by current planet-formation theories(11).

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

164 element enrichment, thus challenges standard planet-formation theory.

165 und in snowfields across cold regions of the planet, forming highly visible red and green patches bel

166 ynamic nature of the Solar System during the planet-forming era.

167 Planets found in and near the typically barren hot-Neptu

168 s research is the accretion of asteroids and planets from a gas-rich circumstellar disk and the final

169 dense plasmasphere, which corotates with the planet, from the hot ring current/plasma sheet outside.

170 mples brought to light the importance during planet growth of highly energetic collisions that lead t

171 e that fit the probe's data suggest that the planet has a diluted core, with a total heavy-element ma

172 The planet has a minimum mass of 0.46 Jupiter masses, very h

173 e presence of more massive bodies(6), yet no planet has so far been detected at a white dwarf.

174 o improve sea level forecasting on a warming planet have focused on determining the temperature, sea

175 So far, no intact planets have been detected in close orbits around white

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

177 The two planets have orbital periods of 9.3 and 21.8 days.

178 egion in mass-radius space that contains few planets) have proved to be particularly valuable in this

179 Big data analyses could benefit the planet if tightly coupled with ongoing sustainability ef

180 Any planet in the 2- to 4-R((+)) range requires a gas envelo

181 m changes and the future habitability of our planet in the Anthropocene epoch.

182 s to the most abundant fish community on the planet in the mesopelagic.

183 0,000 for spectroscopically detectable giant planets in close orbits around white dwarfs.

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

185 median semi-major axis and orbital period of planets in phase space overdensities are 0.087 astronomi

186 are more than [Formula: see text] inhabited planets in the galaxy with a probability exceeding 95%.

187 tween pCO(2) and incident flux on Earth-like planets in the HZ.

188 icities between the inner and outer pairs of planets in the Kepler-431 system of three approximately

189 Planets in the mass range of 10-15 M((+)), if half-ice a

190 Even for the planets in the Solar System, difficulties in observation

191 tions, indicating the presence of additional planets in the system.

192 These planets include HD149026b(3), which is thought to have a

193 As human influences change the planet including the composition of oceans and the atmos

194 almost every environmental niche across the planet, including from air, soil, fresh water, and the o

195 decline of more than 50% since 1970 (Living Planet Index(2)).

196 f taxonomic-geographic systems in the Living Planet Index, 16 systems contain clusters of extreme dec

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

198 important insights into the dynamics of our planet interior.

199 Awareness that our planet is a self-supporting biosphere with sunlight as i

200 ing and temperature regulating an Earth-like planet is also analysed, with a significant advantage de

201 The climate on our planet is changing and the range distributions of organi

202 e of Mars is the interface through which the planet is continuously losing its reservoir of atmospher

203 e compounding effects of climate change, the planet is facing challenges that necessitate significant

204 , we show that while ~40% of the terrestrial planet is intact, only 9.7% of Earth's terrestrial prote

205 The orbit of the planet is most probably the result of gravitational inte

206 Our planet is teeming with an astounding diversity of plants

207 the equilibrium temperature of the 21.8-day planet is ~350 kelvin.

208 ant products of melting the mantles of rocky planets is unclear.

209 es drift poleward in atmospheres of rotating planets like Earth?

210 ion, with two peaks corresponding to smaller planets (likely rocky) and larger intermediate-size plan

211 formation of the aquatic environment of our planet, making it suitable for the emergence of life.

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

213 The key building blocks of the planets may be represented by chondrules, the main const

214 giant planets(14) demonstrated that massive planets might also find their way into tight orbits arou

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

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

217 vide a mechanism for forming wide-separation planets on oblique orbits.

218 f the inner structure and thermal history of planets on their observable features, such as luminosity

219 r a thick atmosphere has survived on a small planet, one approach is to search for signatures of atmo

220 Most known terrestrial planets orbit small stars with radii less than 60 per ce

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

222 A giant planet orbiting a hot white dwarf with a semi-major axis

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

224 theoretical predictions that hot terrestrial planets orbiting small stars may not retain substantial

225 While only the masses of the planets orbiting the brightest stars can be determined b

226 Astronomers have discovered thousands of planets outside the Solar System(1), most of which orbit

227 portunities for detailed characterization of planets outside the Solar System.

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

229 the high eccentricity is most likely due to planet-planet interactions.

230 ons rather than internal migration(13,14) or planet-planet scattering(15,16).

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

232 important question about the composition of planets ranging from 2 to 4 Earth radii (R((+))) still r

233 The interiors of giant planets remain poorly understood.

234 (likely rocky) and larger intermediate-size planets, respectively.

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

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

237 e considered for a full understanding of the planet's atmospheric convection and composition.

238 may result from anthropogenic impacts to the planet's climate and oceans, and informed the creation o

239 as been used to obtain information about the planet's composition and internal structure.

240 Most of the planet's diversity is concentrated in the tropics, which

241 Karsts occupy approximately 20% of the planet's dry ice-free land and are of great socioeconomi

242 ped and developing societies have had on our planet's environment during the past century, and the pr

243 ts are accreted during the early stages of a planet's formation to create a relatively compact core(5

244 the magnetosphere, which is connected to the planet's interior, to determine the wind speed.

245 ygen may have multiple valence states in our planet's interior.

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

247 n the cavity beneath the Ross Ice Shelf, the planet's largest ice shelf by area.

248 uch, information can be shared in one of the planet's most challenging environments for visual commun

249 of eDNA from sponges (phylum Porifera), the planet's most effective water-filterers.

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

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

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

253 n sea level, the hydrological cycle, and the planet's radiation imbalance.

254 clear and pressing need to better manage our planet's resources.

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

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

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

258 due to the orbital evolution of hypothetical planet(s) around the star.

259 riod-ratio range, as well as to a large five-planet sample with qualitatively different configuration

260 binary could fit within the diameter of the planet Saturn.

261 419-B440; Dahl TW, Stevenson DJ (2010) Earth Planet Sci Lett 295:177-186].

262 study the atmosphere and surface of Saturn's planet-sized moon Titan, and orbited Saturn for the next

263 icroplastics in this sensitive region of the planet, specifically studies on temporal trends and pote

264 ane-cycling ecosystems on a globally reduced planet such as the late Hadean/early Archean Earth.

265 For gas giant planets such as Jupiter, the motion of clouds can be com

266 tory of Earth and possibly other terrestrial planets such as Mars, where weathering-formed opal occur

267 onic) occurring in the interior of ice giant planets, such as Uranus or Neptune, are evaluated from e

268 Our model, trained on ~100,000 three-planet systems sampled at discrete resonances, generaliz

269 al understanding of resonant dynamics in two-planet systems with machine-learning techniques to train

270 stabilities may be more efficient in forming planets than previously thought.

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

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

273 convection in the outer layers of gas giant planets that spontaneously generates giant polar cyclone

274 has been interpreted as the debris of rocky planets that were scattered inwards and tidally disrupte

275 Across the planet the biogeographic distribution of human cultural

276 change may impact the largest habitat on the planet, the deep pelagic realm.

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

278 ces nearly half of the primary energy on the planet through photosynthesis or chemosynthesis.

279 e among the most vulnerable countries on the planet to climate variability and climate change.

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

281 31 system of three approximately Earth-sized planets to both be below 0.05.

282 Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune

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

284 Here we report observations of a planet transiting AU Mic.

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

286 ant limitations on our understanding of this planet type.

287 comparable to those present inside icy giant planets (Uranus, Neptune), shock-compressed polyethylene

288 54 Ma), during which time the planet was warmer and wetter than any period in the Ceno

289 ange spreads warm, dry conditions across the planet, water requirements are increasingly likely to dr

290 As the knickpoints are spread across the planet, we suggest that these Martian knickpoints were f

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

292 expected to be delivered to the surfaces of planets where they can potentially play key roles in the

293 ecent lifestyle changes occurring around the planet, whole populations are seeing a major shift in th

294 enerated flood waters of this magnitude on a planet whose present-day average temperature is - 60 deg

295 ring the red giant phase, any close-orbiting planets will be engulfed by the star(2), but more distan

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

297 In response to a warming planet with earlier springs, migratory animals are adjus

298 up of deeper atmospheric layers of icy giant planets, with H(2)O and H(2)S being major constituents.

299 large grains by either hidden, still-forming planets within the disk(2) or (magneto-)hydrodynamic ins

300 s on Earth and potentially other terrestrial planets, yet direct evidence remains elusive.