ライフサイエンスコーパス: star

1 st, or a regression tree-based pipeline, rtp-star.

2 lack hole or an unexpectedly massive neutron star.

3 hs and correlated with the overexpression of Star.

4 erfacial mixing of materials of a progenitor star.

5 olution of hypothetical planet(s) around the star.

6 g magnetized collisionless winds from G-type stars.

7 mptomatic sea stars than in asymptomatic sea stars.

8 ly bound systems of thousands to millions of stars.

9 h is as expected if mergers produce magnetic stars.

10 is less clear for low- and intermediate-mass stars.

11 s of thousands of classical Cepheid variable stars.

12 and die more catastrophically than low-mass stars.

13 vironments for the formation of supermassive stars.

14 e(1,2) and as such mark the death of massive stars.

15 temporal light intensity patterns of distant stars.

16 high mass infall rates to form supermassive stars.

17 cs of the interstellar medium around massive stars.

18 nt and collectively define how galaxies form stars.

19 appears younger and bluer than other coeval stars.

20 ously large radii, or that orbit less active stars.

21 kroaches, crickets, moths, crayfish, and sea stars.

22 days, respectively, for planets around field stars.

23 matic sea stars compared to asymptomatic sea stars.

24 resent the final state of evolution for most stars(1-3).

25 e found in the spectra of ancient metal-poor stars(15-20).

26 ose-orbiting planets will be engulfed by the star(2), but more distant planets can survive this phase

27 gned with the orbital plane of its companion star(2).

28 of pulsators, including low-mass solar-type stars(2), red giants(3), high-mass stars(4) and white dw

29 The purpose of the STAR 2019 Working Group was to build on findings from th

30 )), a cluster of young, massive stars (the S stars(3)) and various gaseous features(4,5).

31 creation of atypical stars (such as magnetic stars(3), blue stragglers(4) and rapid rotators(5)), the

32 ss than their counterparts orbiting Sun-like stars(3-6).

33 about 35 to 210 astronomical units from the star(4), and with clumps exhibiting non-Keplerian motion

34 olar-type stars(2), red giants(3), high-mass stars(4) and white dwarfs(5).

35 matter such as that in the cores of neutron stars(6).

36 manifestations of magnetic 'activity' on the star(8,9).

37 llar core that will then form a supermassive star(9,10).

38 external photoevaporation by nearby massive stars(9).

39 g the structure and evolution of white dwarf stars(9).

40 igh diversity of densoviruses present in sea stars across the West Coast of the United States and glo

41 e variance in in vitro functional data among star alleles with unknown function.

42 = 0.001 [95% CI 31.14, 93.38 meters]; North Star Ambulatory Assessment, p < 0.001 [95% CI 2.702, 6.6

43 bed in terms of a system containing the host star and a protoplanetary disk(1-3), of which the intern

44 ) always disintegrate into a single escaping star and a stable bound binary(3,4), but the chaotic nat

45 We find that the motion of the B star and an accompanying Halpha emission line require th

46 hat mouse tumors exhibited downregulation of Star and Cyp11b1 and upregulation of Ezh2, similar to AC

47 e conversions allowing high molecular weight star and dendritic block copolymers to be prepared in a

48 et, which did not emerge from the progenitor star and instead deposited all of its energy in a therma

49 timicrobial genotypes and non-overlapping NG-STAR and NG-MAST sequence types.

50 eshkov mixing breaks spherical symmetry of a star and provides conditions for synthesis of heavy mass

51 My that is predominantly produced in massive stars and ejected in supernova explosions.

52 imulations of the coalescence of two massive stars and follow the evolution of the merged product.

53 is consistent with observed phenomena in AGB stars and PNe.

54 d lithium abundance with measurements in old stars and with expectations from Big Bang nucleosynthesi

55 ents that enables echinoderm Asteroidea (sea stars) and Holothuroidea (sea cucumbers) to efficiently

56 or Reporting of Diagnostic Accuracy Studies (STARD), and risk of bias was evaluated by adherence to t

57 ed the genome of the cultivated variety "Big Star*" and assessed the genetic diversity among 97 sweet

58 to the core-collapse explosion of a massive star, and probe supernova nucleosynthesis.

59 als, nuclear fission, the merging of neutron stars, and the expansion of the early Universe.

60 The use of star anise oil from a natural source as a dienophile in

61 ltant Fe(2)GeS(4) NPs exhibit an interesting star anise-like morphology with stacks of nanoplates tha

62 f compact binaries with at least one neutron star are promising standard sirens for an independent me

63 Nuclides synthesized in massive stars are ejected into space via stellar winds and super

64 Mergers of neutron stars are known to be associated with short gamma-ray bu

65 neutron-star mergers, and shows that neutron stars are made of neutron-rich matter(13).

66 n of 1.8 solar radii(7), and the two neutron stars are predicted to coalesce in [Formula: see text] m

67 Young stars are surrounded by a circumstellar disk of gas and

68 Black hole binary systems with companion stars are typically found via their x-ray emission, gene

69 sses of the pulsar and the companion neutron star, as measured by a dedicated pulsar timing campaign,

70 y are members of known associations of young stars, as confirmed by modelling of their pulsation spec

71 ore frequent than gas giants around low-mass stars, as predicted by the core accretion theory of plan

72 in limpets and sea urchins, followed by sea stars, ascidians, and sea cucumbers.

73 Lastly, we focus the study on sea star-associated densovirus (SSaDV), the first sea star d

74 experimentally in the zygote of the radiate star Asterias forbesi.

75 ed poecilogony vs. crypticism in the brittle star Astrotoma agassizii across the Southern Ocean.

76 g-shaped ultraviolet ('blue') nebula and the star at its centre, TYC 2597-735-1.

77 ing at someone, and then when they catch you staring at them, you immediately turn away.

78 Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 2

79 s and protostellar disks surrounding forming stars because these environments have higher relative de

80 on to light mass elements synthesized in the star before its explosion.

81 lycophylogeny, our data position the brittle star between invertebrates and vertebrates and confirm t

82 s form a minority of the total population of star-black-hole binaries(5,6).

83 teractions dominate the evolution of massive stars, but their role is less clear for low- and interme

84 ng some cnidarians, ctenophores, and brittle stars, but those use luminescent substrates (luciferins)

85 ften attributed to the tidal disruption of a star by the central black hole(1,2).

86 seismology probes the internal structures of stars by using their natural pulsation frequencies(1).

87 masses of the planets orbiting the brightest stars can be determined by ground-based spectroscopic ob

88 w metagenomic-derived viral genomes from sea stars collected from Antarctica, California, Washington,

89 and a minority cold stellar phase comprising stars, compact objects, and low-temperature gas.

90 sed on its representation in symptomatic sea stars compared to asymptomatic sea stars.

91 versity and ubiquity of these viruses in sea stars confound the original hypothesis that one densovir

92 te and siderophore metabolic pathways in the star coral, Montastraea cavernosa, while there was highe

93 rging of main-sequence and pre-main-sequence stars could produce such strong fields(4,5), and the pre

94 , a Sierpinski triangular prism, and a cubic star, could be readily obtained through dynamic complexa

95 matter phases theorized to exist in neutron star crusts, where the right- and left-handed helical el

96 associated densovirus (SSaDV), the first sea star densovirus discovered, by documenting its biogeogra

97 SSWS.IMPORTANCE The primary interest in sea star densoviruses, specifically SSaDV, has been their as

98 not by a mutant lacking the highly-conserved STAR domain (18 amino-acids, including the LEWD motif).

99 rint time in study I (compared to LR) and in star drill time in study II (no topper) were observed.

100 e (40-m sprint time, long jump distance, and star drill time) in youth male athletes age 10-19, in tw

101 introduction of sea urchin AGS into the sea star embryo induces asymmetric cell divisions, suggestin

102 Pulsars are rotating neutron stars emitting lighthouse-like beams.

103 ravitational waves (GWs) from binary neutron stars encode unique information about ultra-dense matter

104 If the neutron-star equation of state is sufficiently stiff (that is, t

105 ctive field theory, to constrain the neutron-star equation of state.

106 ed with the collision of two extreme-density stars establishes the origin of r-process elements in ne

107 ) mobility (the Timed Up and Go test and the Star Excursion Balance test), and (4) perceptions of the

108 ergy into the interstellar medium by massive stars ('feedback') are the main uncertainties in modern

109 "becoming pale with sinking to the floor and staring for approximately 1 minute with confusion therea

110 It is important to determine if massive stars form via disc accretion, like their low-mass count

111 a link between astronomical observations of star formation and cosmochemical studies of Solar System

112 The physics of star formation and the deposition of mass, momentum and

113 r age of 2.98 billion years, indicating that star formation commenced in these galaxies at a mean red

114 le (about 10 million years), with integrated star formation efficiencies of only 2 to 3 per cent.

115 not negligible and could affect the rate of star formation in the central regions of the Galaxy.

116 rius A* at its current level of activity nor star formation in the inner Galaxy seems to be a viable

117 A simple model of star formation in the spiral arms reproduces the observe

118 tify the evolutionary timeline and find that star formation is regulated by efficient stellar feedbac

119 ossibly formed during an episode of enhanced star formation ~7 Ga ago.

120 servoir of material available to fuel future star formation, but direct constraints on its mass and p

121 hase outflow is probably driven by bursts of star formation, consistent with theory(11,12).

122 llar to pre-main sequence (T Tauri) phase of star formation, placing Solar System formation within an

123 e galaxies and are believed to trace intense star-formation events and the hierarchical build-up of s

124 Our current knowledge of cosmic star-formation history during the first two billion year

125 thousand times more massive, with a specific star-formation rate (the star-formation rate divided by

126 ve, with a specific star-formation rate (the star-formation rate divided by the mass) a hundred times

127 of them are extreme starburst galaxies with star-formation rates exceeding 1,000 solar masses per ye

128 itude higher than extreme starbursts(5)) and star-formation rates of 200 solar masses per year, these

129 e true abundance of massive galaxies and the star-formation-rate density in the early Universe.

130 to higher-metallicity, massive elliptical or star-forming galaxies, suggesting that perhaps the repea

131 detailed properties of disks in the earliest star-forming phases been observed(6,7).

132 ing FRB source(6), FRB 180916.J0158+65, to a star-forming region in a nearby (redshift 0.0337 +/- 0.0

133 RB 121102) has been localized to the largest star-forming region of a dwarf galaxy at a cosmological

134 RB 121102) has been localized to the largest star-forming region of a dwarf galaxy at a cosmological

135 imaged ionizing photon escape from a compact star-forming region through a narrow channel in an optic

136 med in interstellar ices before subliming in star-forming regions like SgrB2(N), thus providing a cri

137 e organosulfur chemistry can be initiated in star-forming regions via the elementary gas-phase reacti

138 e structure comprises the majority of nearby star-forming regions, has an aspect ratio of about 1:20

139 a likely source of organosulfur molecules in star-forming regions.

140 RN for endomesoderm specification in the sea star from zygote through gastrulation that corresponds t

141 tration of Drimys angustifolia AFPs into the star fruit allowed an initial cryoprotection, indicating

142 Moreover, with this treatment the star fruit firmness was maintained on thawing after 60 d

143 n of AFPs can increase the quality of frozen star fruit.

144 However, only star fruits that were vacuum infiltrated with AFPs retai

145 High-mass stars fuse elements much faster, fuse heavier nuclei, an

146 ng and annotation for gene fusion calls from STAR-Fusion and Arriba by merging, filtering, and priori

147 Overall, STAR-Fusion, Arriba, and STAR-SEQR are the most accurate

148 Gould Belt(1-4), an expanding ring of young stars, gas and dust, tilted about 20 degrees to the Gala

149 rth exoplanets orbiting the nearby red dwarf star GJ 887.

150 hs, 22 out of 27 (81.5%) patients undergoing STAR-guided ablation were free from AF/atrial tachycardi

151 STAR-guided AFD ablation through sequential mapping with

152 solation, leaving 27 patients that underwent STAR-guided AFD ablation.

153 erage, studies complied with only 35% of the STARD-guideline items.

154 and gaps) in disks around pre-main-sequence stars have been detected in abundance towards class II p

155 intermediate mass-the so-called delta Scuti stars-have rich pulsation spectra for which systematic m

156 e rise to the exclusive self-assembly of the star hexagon [Cd(18)L(1)(6)L(3)(3)] through complementar

157 on influenced the self-assembly pathway, the star hexagon was truncated into two triangular fragments

158 The accretion of hydrogen onto a white dwarf star ignites a classical nova eruption(1,2)-a thermonucl

159 the planet candidate passing in front of the star in its orbit.

160 euvel and Tauris argue that if the red giant star in the system 2MASS J05215658+4359220 has a mass of

161 s is further supported by a lack of magnetic stars in close binaries(8,9), which is as expected if me

162 -moving stellar groups around exoplanet host stars in the astrometric data from the Gaia satellite(11

163 hard ultraviolet radiation emitted by young stars in the first galaxies.

164 MC(17), detection of highly ionized gas near stars in the LMC(18,19) and predictions of cosmological

165 The space motions of some of these stars indicate that they are members of known associatio

166 ntly predicted from a bioluminescent brittle star, indicating that RLuc-like luciferases may have evo

167 l wind from an asymptotic giant branch (AGB) star into a nonspherical planetary nebula (PN) could be

168 that the radius of a 1.4-solar mass neutron star is [Formula: see text] km at 90% confidence and the

169 ection of newly formed planets around such a star is challenged by the presence of spots, plage, flar

170 and the predicted fraction of merged massive stars is also about ten per cent(6,7).

171 X-ray emission from young solar-type stars is thousands of times brighter than that of today'

172 NIa)-thermonuclear explosions of white dwarf stars-is an open question in astrophysics.

173 A class of neutron stars known as magnetars is a leading candidate source o

174 in an 11-hour orbit around the small nearby star LHS 3844.

175 Herein, a general amphiphilic star-like block copolymer nanoreactor strategy for in si

176 Third, we describe the star-like expansion of Q-M848 (within Q-M3) starting at

177 Here, we model such NONs as star-like motifs to analytically derive the critical val

178 lling into question our understanding of how stars lose angular momentum and spin down as they age(12

179 ensed in outflows of asymptotic giant branch stars <4.9 Ga ago that possibly formed during an episode

180 y coherent emission from FRBs invoke neutron star magnetospheres(3-5) or relativistic shocks far from

181 could be a binary composed of two 0.9 M ( ) stars, making a triple system.

182 This study aimed to determine whether STAR mapping using sequential recordings from convention

183 astic trajectory analysis of ranked signals (STAR) mapping approach to guide atrial fibrillation (AF)

184 drivers (AFDs) were identified on sequential STAR maps created with PentaRay, IntellaMap Orion, or Ad

185 lide perovskites have emerged as a series of star materials for solar cells, lasers and detectors.

186 r, Tatsumi found that the core of a magnetar star may be a quark nugget in a ferromagnetic state with

187 The novel magnetic black star (MBS) stent provided with a customized retrieval de

188 The binary neutron star merger event GW170817 was detected through both ele

189 found following the discovery of the neutron-star merger GW170817 by gravitational-wave detectors(10)

190 kilonova associated with the binary neutron-star merger GW170817 remains the only confirmed electrom

191 with the expectations from standard neutron-star merger models.

192 circumstantial evidence(6) point to neutron-star mergers as a probable r-process site; the optical/i

193 As neutron-star mergers occur infrequently, their deposition of rad

194 ith the event-rate density of binary neutron-star mergers that is robustly inferred from the detectio

195 Observations of neutron-star mergers with distinct messengers, including gravita

196 olar System point to their origin in neutron-star mergers, and indicate substantial deposition by a s

197 the origin of r-process elements in neutron-star mergers, and shows that neutron stars are made of n

198 vent GW190425, both originating from neutron-star mergers.

199 ld be reported, and we encourage this in our STAR Methods guidelines for all papers.

200 ock number, and feeding schedules within the STAR Methods section and Experimental Models section of

201 /213 were present in aphid gut as mature and star miRNAs.

202 olarization topological structures of lemon, star, monstar, spiral, dipole and quadrupole are created

203 In mice, these star nanoparticles trafficked to lymph nodes (LNs) by 4

204 ntly available databases on miRNAs and NSDs, star NSD miRNAs, NSD spectrum width, miRNA spectrum widt

205 ar anion binding affinities to the metalated Star of David catenane in solution-also display no ion t

206 The (Fe(II))(6)-coordinated Star of David catenane, derived from a hexameric cyclic

207 (Fe(II))(6)-coordinated triply interlocked ("Star of David") [2]catenane (6(1)(2) link) and a (Fe(II)

208 bserve and quantify it, has been the guiding star of my work.

209 However, a large group of pulsating stars of intermediate mass-the so-called delta Scuti sta

210 lipsing binary systems composed of late-type stars offer the most precise and accurate way to measure

211 n-depth analysis of N-glycans from a brittle star (Ophiactis savignyi) as an example member of the cl

212 During the day, the brittle star Ophiocoma wendtii demonstrates spatial vision due t

213 cular vision research [1-7], and the brittle star Ophiocoma wendtii, which exhibits light-responsive

214 final state (for example, as a single merged star or a tighter, surviving binary(11)).

215 r magnetospheres of compact objects (neutron stars or black holes) or relativistic shocks launched fr

216 able zone (HZ), which is the region around a star (or multiple stars) where standing bodies of water

217 manship task known colloquially as the Death Star over six training days.

218 Star-PAP control of the distal-specific isoform is stimu

219 ecific NQO1 mRNA isoforms in the presence of Star-PAP expression, and reverses molecular events of hy

220 STAR particles are millimeter-scale particles made of al

221 very of tetanus toxoid vaccine to mice using STAR particles generated immune responses that were at l

222 treated with topical 5-fluorouracil, use of STAR particles increased the efficacy of the drug in sup

223 Use of STAR particles provides a simple, low-cost and well-tole

224 STAR particles were well tolerated and effective at crea

225 , we developed star-shaped particles, termed STAR particles, to dramatically increase skin permeabili

226 t protect centrioles from removal in the bat star Patiria miniata.

227 Star plot show that woody aroma compounds are dominant i

228 this photoswitch to a poly(ethylene glycol) star polymer, we can tune the stiffness of covalent adap

229 rst-principles mode-coupling theory (MCT) of star-polymer vitrimers.

230 polymer gel comprising poly(ethylene glycol) star polymers linked by Cu(24) L(24) metal-organic cages

231 of linear polymers or the alpha-chain end of star polymers.

232 ome (SSWS), a disease that has decimated sea star populations across the West Coast of the United Sta

233 rge diversity of densoviruses present in sea star populations.

234 of a Sierpinski triangular prism and a cubic star possessing three and six cavitand-based motifs, res

235 cultivars of broccoli sprouts i.e., Southern star, Prominence and Monotop.

236 Modelling of these pulsating stars provides stringent tests of white dwarf models and

237 al number of antibiotic items prescribed per STAR-PU (specific therapeutic group age/sex-related pres

238 ity control (QC) measurements to establish a star rating system.

239 produced in the simulations, and the merged star rejuvenates such that it appears younger and bluer

240 zymatic domains, Them1 contains a C-terminal StAR-related lipid transfer (START) domain with unknown

241 up was to build on findings from the initial STAR report to further clarify the expectations, limitat

242 s also characterised by the frequency of the star's fundamental oscillation mode (f-mode).

243 we used observations of the Galactic Center star S0-2 to test this prediction.

244 Overall, STAR-Fusion, Arriba, and STAR-SEQR are the most accurate and fastest for fusion d

245 lotype with closely related singletons in a 'star-shape' surrounding it.

246 Astrocytes, the star-shaped brain cells, are known chemosensitive cells

247 A star-shaped DNA architecture, carrying five molecular be

248 rophilic and hydrophobic quasi-spherical and star-shaped gold (Au)NPs are synthesized to explore the

249 ings proceed to completion, on a three-armed star-shaped macromolecule to maximize efficiency during

250 Here, we developed star-shaped particles, termed STAR particles, to dramati

251 The C(3) -symmetric star-shaped phenothiazene-substituted truxene 1 was reac

252 g of a superparamagnetic iron oxide core and star-shaped plasmonic shell with high-aspect-ratio gold

253 developed to determine the branch number of star-shaped PLGAs, and to separate PLGAs based on L:G ra

254 the comprehensive analysis of (1) linear and star-shaped polymers, (2) hydrogenated and deuterated po

255 Glu-PLGA is a branched (also known as star-shaped) polymer and determining its properties has

256 mation environment, through either dynamical star-star interactions or external photoevaporation by n

257 e, they may lead to the creation of atypical stars (such as magnetic stars(3), blue stragglers(4) and

258 We present observations of the triple-star system GW Orionis, finding evidence for disk tearin

259 alactic population of merging double neutron-star systems (that is, those that will coalesce within b

260 Gravitational forces in multiple star systems can disrupt the disk.

261 but common phase in the evolution of binary star systems(1,2).

262 centration (all patients) and cardiac MRI T2-star (T2*; patients aged >10 years) to show non-inferior

263 properties of the magnetic 'blue straggler' star tau Sco in the Upper Scorpius association that has

264 st rocky exoplanets orbiting closer to their star than the habitable zone that were formed with thick

265 d was no more represented in symptomatic sea stars than in asymptomatic sea stars.

266 s (composed of a greater number of co-moving stars than unstructured space) and the field.

267 hind a supramassive or even a stable neutron star that spins rapidly with a strong magnetic field(5-8

268 s close to massive black holes can rip apart stars that come too close to them.

269 ide the Solar System(1), most of which orbit stars that will eventually evolve into red giants and th

270 (1,2)), a cluster of young, massive stars (the S stars(3)) and various gaseous features(4,5)

271 is misaligned with the orbital plane of the stars, the disk should warp and break into precessing ri

272 are likely due to core collapses of massive stars; these are concentrated in the thin Galactic disk

273 About ten per cent of 'massive' stars (those of more than 1.5 solar masses) have strong,

274 Dying low-mass stars throw off their enriched outer layers, leaving beh

275 es and has been related to bites of the lone star tick (Amblyomma americanum).

276 sed to characterize the IgE response to lone star tick proteins administered through the skin of mice

277 argely conforms to the territory of the lone star tick.

278 we report for the first time that adult lone star ticks, Amblyomma americanum, also actively drink nu

279 ut its source and interactions, from distant stars to biological samples.

280 We used 179 publicly available sea star transcriptomes to complement our approaches for den

281 White areas of star-type bicolour petals of petunia (Petunia hybrida) a

282 sence of the triangular prop, a four-pointed star was produced.

283 The first signs of sea star wasting disease (SSWD) epidemic occurred in just fe

284 ns more consistent with observed data on sea star wasting disease, which suggests that environmental

285 A viral etiology of sea star wasting syndrome (SSWS) was originally explored wit

286 y SSaDV, has been their association with sea star wasting syndrome (SSWS), a disease that has decimat

287 Using rtp-star, we inferred the network of ATHB13, a downstream ge

288 age, mass, metallicity and distance from the star, we obtain highly significant differences (with p v

289 ht atmospheres on warm exoplanets orbiting M-stars, we should target worlds that formed H(2)-poor, th

290 ich is the region around a star (or multiple stars) where standing bodies of water could exist on the

291 ggering collapse of rapidly rotating massive stars), which have previously been speculated to produce

292 These stars, which are supported by electron degeneracy pressu

293 modes in 60 intermediate-mass main-sequence stars, which enables definitive mode identification.

294 Supernovae can leave behind neutron stars, which may later merge to produce additional heavy

295 Most known terrestrial planets orbit small stars with radii less than 60 per cent of that of the Su

296 Similar extensions are shown for stars with stellar effective temperatures between 2,600-

297 We observed a sample of AGB stars with the Atacama Large Millimeter/submillimeter Ar

298 orrelation between the masses of hot gas and stars within dark matter halos of fixed total mass.

299 appears to cross the debris ring around the star without the expected gravitational perturbations.

300 the Galactic plane suggest that it is an old star, yet it has abnormally low surface gravity and a de