ライフサイエンスコーパス: Neptune

1 mes in the Nephrotic Syndrome Study Network (NEPTUNE).

2 outwards because of tidal interactions with Neptune.

3 rge number of bodies orbiting the Sun beyond Neptune.

4 CH4, water, and ammonia, such as Uranus and Neptune.

5 s may be important as they are at Uranus and Neptune.

6 conditions as in the interiors of Uranus and Neptune.

7 ner Solar System to excitation by Uranus and Neptune.

8 compared to conventional parameters alone in NEPTUNE.

9 sk, possibly around the orbits of Uranus and Neptune.

10 rough a spin-orbit precession resonance with Neptune.

11 ost exoplanets with masses exceeding that of Neptune.

12 iper Belt but Triton being later captured by Neptune.

13 and in GCR measured by Voyager 2, then near Neptune.

14 epler planets, 92% of which are smaller than Neptune.

15 sion to their Ice Giant siblings, Uranus and Neptune.

16 d orbits and sizes between that of Earth and Neptune.

17 er-Earth," whereas the other is more akin to Neptune.

18 representative of the interior of Uranus and Neptune.

19 ocks upstream of Jupiter, Saturn, Uranus and Neptune.

20 he Sun before being captured in orbit around Neptune.

21 elt analogous region out beyond the orbit of Neptune.

22 similar in morphology to those of Uranus and Neptune.

23 ting of solid bodies orbiting the Sun beyond Neptune.

24 retrograde orbit at 14 planetary radii from Neptune.

25 of 30 to 50 km, were presumably captured by Neptune.

26 res and temperatures of super-Earths and sub-Neptunes.

27 torage and evolution in super-Earths and sub-Neptunes.

28 ing rocky super-Earths and gas-enveloped sub-Neptunes.

29 ospheres: Earth, Jupiter, Saturn, Uranus and Neptune(1).

30 rths" (1.0 to 1.5 R((+))) from gas-rich "sub-Neptunes" (2.0 to 3.0 R((+))).

31 rome Rare Disease Clinical Research Network (NEPTUNE); (2) FSGS clinical trial (FSGS-CT); and (3) Kid

32 fference in the environmental impact between Neptune 3 and canister systems, evaluating all individua

33 The Neptune 3 drainage system is developed as an alternative

34 In both high and low volume procedures, Neptune 3 has a lower environmental impact compared to c

35 Results from this LCA demonstrate that the Neptune 3 system is environmentally beneficial compared

36 loss in the evolution of close-orbiting sub-Neptunes(5-8,15,16).

37 at of Earth (with radius R Earth symbol) and Neptune (about 4R Earth symbol) are now known to be comm

38 yager 2 spacecraft imaged six small moons of Neptune, all with orbits well interior to that of the la

39 In high volume scenarios (5 + Liters) Neptune also has a lower impact in stratospheric ozone d

40 dual stages of the product life cycle of the Neptune and canisters.

41 eatures had high prognostic accuracy in both NEPTUNE and CureGN, and higher prognostic accuracy for b

42 eptune-sized Kepler-4b is similar to that of Neptune and GJ 436b, even though the irradiation level i

43 MIF was observed for Si isotopes on both Neptune and Neptune plus MC-ICPMS instruments in this st

44 ase in the nebula from which Saturn, Uranus, Neptune and their major moons formed.

45 e plastic flow of the internal icy layers in Neptune and Uranus may be significantly faster than prev

46 iar geophysical properties of the ice giants Neptune and Uranus, there has been a growing interest in

47 objects, KBOs) that lie beyond the orbit of Neptune and which are believed to have formed contempora

48 planetary systems (including systems of 'hot Neptunes' and 'super-Earths') whose angular momentum vec

49 e interiors of the ice giant planets Uranus, Neptune, and sub-Neptune exoplanets.

50 Exoplanets smaller than Neptune are common around red dwarf stars (M dwarfs), wi

51 Close-in transiting sub-Neptunes are abundant in our Galaxy(1).

52 Sub-Neptunes are common among the discovered exoplanets.

53 Sub-Neptunes are expected to be the most diverse family of t

54 Super-Earths and sub-Neptunes are the most common planet types in our galaxy.

55 h and Neptune (hereafter referred to as 'sub-Neptunes') are found in close-in orbits around more than

56 rior of ice giant planets, such as Uranus or Neptune, are evaluated from equilibrium ab initio molecu

57 ity waves can result in orbital evolution of Neptune as well as changes in the structure of the Kuipe

58 or an emerging taxonomy of volatile-rich sub-Neptunes as a function of their equilibrium temperature

59 The Kuiper belt extends from the orbit of Neptune at 30 au to an abrupt outer edge about 50 au fro

60 iper belt-the region of space extending from Neptune (at 30 astronomical units) to well over 100 AU a

61 However, the icy debris beyond the orbit of Neptune, called the Kuiper Belt, contains only one known

62 Similar to its family member, EKLF, Neptune can bind CACCC-box and GC-rich DNA elements.

63 ditions inside ice giants such as Uranus and Neptune can result in peculiar chemistry and structural

64 led in the Nephrotic Syndrome Study Network (NEPTUNE) cohort and from our own institutions, for circu

65 The cooler condition of the interior of Neptune compared to Uranus means that the former is much

66 ed radius-mass relationship suggest that sub-Neptunes contain a discernible amount of either hydrogen

67 We show that Neptune cooperates with the hematopoietic transcription

68 SI) kidney biopsies from participants in the NEPTUNE/CureGN prospective observational cohort studies

69 In the NEPTUNE dataset, tubular features were quantified at the

70 The discovery of exoplanets in the hot-Neptune desert(6), a region close to the host stars with

71 s found in and near the typically barren hot-Neptune 'desert'(1,2) (a region in mass-radius space tha

72 descriptors were quantified by applying the NEPTUNE Digital Pathology Scoring System to NEPTUNE kidn

73 ) from the Nephrotic Syndrome Study Network (NEPTUNE) Digital Pathology Scoring System.

74 sizes and masses between those of Earth and Neptune, dominate the exoplanet population.

75 f giant planets--Jupiter, Saturn, Uranus and Neptune--during their formation.

76 r Minimal Change Disease collected across 29 NEPTUNE enrolling centers along with 459 whole slide ima

77 a fundamentally different mineralogy for sub-Neptune exoplanets compared with rocky planets.

78 Many sub-Neptune exoplanets have been believed to be composed of

79 cliff") and the atmosphere chemistry of sub-Neptune exoplanets.

80 e ice giant planets Uranus, Neptune, and sub-Neptune exoplanets.

81 neptune expression is induced in response to components

82 ure condition in the interiors of Uranus and Neptune, forming a H(2)O-dominated fluid in the upper ma

83 ssible precursor of the super-Earths and sub-Neptunes frequently found around main-sequence stars.

84 Dead leaves of the Neptune grass, Posidonia oceanica (L.) Delile, in the Me

85 ication, and human carcinogenic toxicity the Neptune has a lower impact only in the very large volume

86 Neptune has five narrow ring arcs, spanning about 40 deg

87 Determining why Uranus and Neptune have different field morphologies is not only cr

88 ft discovered that the ice giants Uranus and Neptune have nondipolar magnetic fields, defying expecta

89 Water-rich sub-Neptunes have been believed to form farther from the sta

90 mosphere-interior boundary, the cores of sub-Neptunes have been modeled with molten silicates and met

91 a vast swarm of small bodies orbiting beyond Neptune, have been a major process affecting this popula

92 ets with radii between that of the Earth and Neptune (hereafter referred to as 'sub-Neptunes') are fo

93 o reach water-rich compositions for some sub-Neptunes, implying an evolutionary relationship between

94 re likely captured by a migrating, eccentric Neptune in a dynamically excited planetesimal population

95 anets intermediate in size between Earth and Neptune in our Solar System, yet these objects are found

96 f two Sun-like stars by planets smaller than Neptune in the billion-year-old open cluster NGC6811.

97 i-planet systems containing super-Earths and Neptunes in orbits of a few days to a few months.

98 In the region beyond Neptune, in contrast, no collisionally created families

99 NEPTUNE included 166 patients with incident FSGS enrolle

100 e-temperature brown dwarfs resembles that of Neptune, indicating the presence of zonal temperature an

101 roximately 10(3)-kilometre-sized bodies) and Neptune is a far more likely explanation for Triton's ca

102 NEPTUNE is a multicenter US/Canada cohort study; FSGS-CT

103 These studies demonstrate that Neptune is a positive regulator of primitive erythropoie

104 group with larger radii (referred to as 'sub-Neptunes') is distinguished by having hydrogen-dominated

105 The Nephrotic Syndrome Study Network (NEPTUNE) is poised to address these challenges.

106 of small bodies in undisturbed orbits beyond Neptune, is composed of primitive objects preserving inf

107 rings, these moons are probably younger than Neptune itself; they formed shortly after the capture of

108 -bearing molecules in the habitable zone sub-Neptune K2-18 b.

109 NEPTUNE Digital Pathology Scoring System to NEPTUNE kidney biopsies.

110 The NEPTUNE Knowledge Network, comprising combined, multisca

111 Similar populations and dynamics at both Neptune Lagrangian regions indicate that the Trojans wer

112 outer planets, some of their moons, as well Neptune-like exo-planets.

113 Recent discoveries of water-rich Neptune-like exoplanets require a more detailed understa

114 of icy moons, giant planets and Uranus- and Neptune-like exoplanets(1-3).

115 e of tidally driven inflation(4) acting on a Neptune-like internal structure, which can naturally exp

116 pproximately 740 K) transiting planet with a Neptune-like mass of roughly 30.5 M((+)) and Jupiter-lik

117 as massive as Jupiter, to intermediate-mass Neptune-like objects with large cores and moderate hydro

118 far too small to deplete the atmosphere of a Neptune-like planet in the lifetime of the parent star,

119 n that hot rocky planets might have begun as Neptune-like, but subsequently lost all of their atmosph

120 ind a mass of 7.1 +/- 0.7 M((+)) for the sub-Neptune LP 791-18c and a mass of [Formula: see text] for

121 n MgO rock in the deep interiors of Earth to Neptune mass planets.

122 Here we report that in the ultraviolet the Neptune-mass exoplanet GJ 436b (also known as Gliese 436

123 We find that the eccentric orbit of the Neptune-mass exoplanet GJ 436b is nearly perpendicular t

124 detailed atmospheric study of the transiting Neptune-mass exoplanet HAT-P-26b.

125 sed radial velocity observations to detect a Neptune-mass exoplanet orbiting LHS 3154, a star that is

126 Surveys have shown that super-Earth and Neptune-mass exoplanets are more frequent than gas giant

127 accretion simulations, we show that close-in Neptune-mass planets are only formed if the dust mass of

128 of the Sun) host star, and is one of the few Neptune-mass planets that is amenable to detailed charac

129 The NEPTUNE Match report is communicated using established p

130 NEPTUNE Match represents the first application of precis

131 we describe the design and implementation of NEPTUNE Match, which bridges a basic science discovery p

132 The small eccentricity of Neptune may be a direct consequence of apsidal wave inte

133 ugh column chemistry using a Thermo Finnigan Neptune MC-ICPMS and a Nu Sapphire CRC-MC-ICPMS in CRC m

134 e influence of sample introduction system on Neptune MC-ICPMS lead isotopic ratio measurements was te

135 ion of C ((29)Si(+)) and H3 ((30)Si(+)) on a Neptune MC-ICPMS.

136 masses using medium resolution on the Thermo Neptune MC-ICPMS.

137 the hundreds of multi-planet systems of sub-Neptunes, more planet pairs are observed near resonances

138 a class of abundant exoplanets smaller than Neptune on close, <100-day orbits(1-4).

139 The field planets are usually the size of Neptune or smaller.

140 Terrestrial and sub-Neptune planets are expected to form in the inner (less

141 Sub-Neptune planets, with sizes and masses between those of

142 observed for Si isotopes on both Neptune and Neptune plus MC-ICPMS instruments in this study.

143 e of apsidal wave interaction with the trans-Neptune population of debris called the Kuiper belt.

144 In large sub-Neptunes, pressure at the atmosphere-magma boundary can

145 The gravitational interaction with the sub-Neptune prevents the complete circularization of LP 791-

146 anetary mass-metallicity relation in the sub-Neptune regime.

147 the properties of lower-mass exoplanets (sub-Neptune) remain largely unconstrained because of the cha

148 Study pathologists scored 12 descriptors in NEPTUNE renal biopsies from 242 patients with minimal ch

149 al magnetic fields of the planets Uranus and Neptune represent important observables for constraining

150 uggest that geophysical models of Uranus and Neptune require reassessment because chemical reactivity

151 d Saturn's obliquity to increase through the Neptune resonance.

152 et GJ 436b-which has been labelled as a 'hot Neptune'-reveals itself by the dimming of light as it cr

153 5 au and were subsequently pushed outward by Neptune's 1:2 mean motion resonance during its final pha

154 ar, for a belt eroded out to the vicinity of Neptune's 2:1 resonance at about 48 astronomical units,

155 raviolet and GCR are likely to be modulating Neptune's atmosphere in combination.

156 GCR is further supported by the response of Neptune's atmosphere to an intermittent 1.5- to 1.9-year

157 Long-duration observations of Neptune's brightness at two visible wavelengths provide

158 A similar coincident variability in Neptune's brightness suggests nucleation onto GCR ions.

159 et TOI-849b, which has a radius smaller than Neptune's but an anomalously large mass of [Formula: see

160 A fusion protein comprised of Neptune's DBD and the Drosophila engrailed repressor dom

161 :1 resonance at about 48 astronomical units, Neptune's eccentricity can damp to its current value ove

162 h a perihelion distance of 70 au, far beyond Neptune's gravitational influence.

163 We also observe Naiad, Neptune's innermost moon, which was last seen in 1989, a

164 Despite these common features, Neptune's irregular satellite system, hitherto thought t

165 ontrolled by precipitation of electrons from Neptune's magnetosphere as previously proposed, Triton c

166 The discovery of Uranus' and Neptune's non-dipolar, non-axisymmetric magnetic fields

167 s) are an ancient reservoir of comets beyond Neptune's orbit.

168 n region of gravitational equilibrium within Neptune's orbit.

169 product of a merging binary near the end of Neptune's orbital migration.

170 Triton is Neptune's principal satellite and is by far the largest

171 same wavelengths in the spectra of Pluto and Neptune's satellite Triton are due to CH4 on their surfa

172 ethylene may be required to explain the hot Neptune's small CH(4)-to-CO ratio, which is at least 10(

173 Neptune shapes the dynamics of most Kuiper belt objects,

174 se present inside icy giant planets (Uranus, Neptune), shock-compressed polyethylene retains a polyme

175 piters (with slightly larger orbits) and hot Neptune-size candidates do exhibit signatures of additio

176 Characterizing rocky or sub-Neptune-size exoplanets with JWST is an intricate task,

177 rum of the approximately 750 K, low-density, Neptune-sized exoplanet WASP-107b using a combination of

178 The density of the Neptune-sized Kepler-4b is similar to that of Neptune an

179 Earth masses, almost twice that of any other Neptune-sized planet known so far, and a density of 9.7

180 Neptune-sized planets exhibit a wide range of compositio

181 ions, we demonstrate sensitivity to warm sub-Neptune-sized planets throughout much of the habitable z

182 on close to the host stars with a deficit of Neptune-sized planets, provides insights into the format

183 ar absorption in the atmospheres of smaller (Neptune-sized) planets during transits have revealed onl

184 lt is subject to resonant perturbations from Neptune, so that the transport of angular momentum by de

185 abling unprecedented characterization of sub-Neptunes, starting with the first detections of carbon-b

186 cts in the Nephrotic Syndrome Study Network (NEPTUNE), stratified by APOL1 risk genotype.

187 The NEPTUNES study evaluated combination nivolumab and ipili

188 Small planets between the sizes of Earth and Neptune substantially outnumber Jupiter-sized planets.

189 anets intermediate in size between Earth and Neptune ('super-Earths') are among the most common plane

190 er support for the hypothesis that the inner Neptune system has been shaped by numerous impacts.

191 o end-point results, it is observed that the Neptune system is beneficial for resources in each scena

192 GJ 1214b is an archetype sub-Neptune that has been observed extensively using transmi

193 a temperate exo-Earth in a system with a sub-Neptune that retained its gas or volatile envelope.

194 oir of icy bodies at and beyond the orbit of Neptune-the Kuiper belt-has opened a new frontier in ast

195 rocky core, befitting the appellation ''mini-Neptunes.'' The gas giant planets occur preferentially a

196 e in two cold reservoirs beyond the orbit of Neptune: the Kuiper Belt (equilibrium temperatures of ap

197 disk of icy bodies that orbit the Sun beyond Neptune; the largest known members are Pluto and its com

198 embers, refs 6, 7), Uranus (six, ref. 8) and Neptune (three, ref. 9).

199 eport the detection of 2008 LC18, which is a Neptune Trojan in the trailing (L5) Lagrangian region of

200 This discovery demonstrates that the Neptune Trojan population occupies a thick disk, which i

201 We estimate that the leading and trailing Neptune Trojan regions have similarly sized populations

202 e report the discovery of a high-inclination Neptune Trojan, 2005 TN(53).

203 The Neptune Trojans appear to have a population that is seve

204 Our color measurements show that Neptune Trojans have statistically indistinguishable sli

205 ort the discovery of five irregular moons of Neptune, two with prograde and three with retrograde orb

206 f critical importance for devising models of Neptune, Uranus, and white dwarf stars, as well as of ex

207 The warm Neptune WASP-107b stands out among exoplanets with an un

208 atmospheres of Jupiter, Saturn, Uranus, and Neptune were modeled as shallow layers of turbulent flui

209 e bodies in the universe, such as Saturn and Neptune, where nonmolecular ice is thought to be the mos

210 ere, we identified a novel Xenopus KLF gene, neptune, which is highly expressed in the ventral blood

211 servations and atmospheric inferences of sub-Neptunes, which in turn provide key insights into their

212 es of models for the interiors of Uranus and Neptune with the Concentric MacLaurin Spheroid method.

213 Similarly, for sub-Neptunes with H(2)O-rich interiors, increasing atmospher

214 The six planets are found to be sub-Neptunes with radii ranging from 1.94R((+)) to 2.85R((+)

215 ficant tidal heating due to its orbit around Neptune, with subsequent resurfacing and a relatively fl

216 ing rocky gas dwarfs, water worlds, and mini-Neptunes, with a wide range of atmospheric, surface, and

217 jects orbiting primarily between Jupiter and Neptune--with an equivalent radius of 124 +/- 9 kilometr