ライフサイエンスコーパス: disk

1 f material that formed in the protoplanetary disk.

2 a strongly warped intermediate region of the disk.

3 ces in multiple star systems can disrupt the disk.

4 before the dissipation of the protoplanetary disk.

5 onstrain the warped shape of the Milky Way's disk.

6 for rapid accretion of the protoplanetesimal disk.

7 a change in the inner edge of the accretion disk.

8 thin membranes supported upon a porous steel disk.

9 ng the evolution of the Solar protoplanetary disk.

10 urrent injection into a microscopic magnetic disk.

11 t differs markedly from that of the Galactic disk.

12 ossibly overlapping with the outer accretion disk.

13 re and evolution of the Solar protoplanetary disk.

14 Py film by local vortex imprinting from a Co disk.

15 ligned with the orbital planes and the outer disk.

16 e preliminary colorimetric readout on the PT-Disk.

17 m (SR) junctional cisternae, and apo-GP at Z disk.

18 nd atrophic changes radiating from the optic disks.

19 metry (UPLC-MS) of samples eluted from RAMES disks.

20 iously established ZDs around the carbapenem disks.

21 amming point of a bidisperse mixture of soft disks.

22 nscription in developing Drosophila imaginal disks.

23 ustained rotation and motion of the hydrogel disks.

24 iodic geometry of stacked thylakoid membrane disks.

25 ere collected parallel to the intervertebral disks.

26 ontaining the host star and a protoplanetary disk(1-3), of which the internal properties (for example

27 rees C) and high binding capacity (9.5 mg Hg disk(-1)) toward Hg(2+).

28 d emission-signatures of dusty circumstellar disks(12), stellar activity(13) and accretion(14).

29 lipid scramblases in mammalian photoreceptor disks [16], yet chromophore-independent roles of opsin a

30 her hidden, still-forming planets within the disk(2) or (magneto-)hydrodynamic instabilities(3).

31 binding capacity of 4.24 mug per binding gel disk (3.14 cm(2)), ensuring sufficient capacity to measu

32 ry-mass bodies carving rings and gaps in the disk(4).

33 y torus that surrounds the central accretion disk(5).

34 rs is rotating in alignment with the stellar disk(6,7), as are more centrally located clusters(8,9).

35 ting in their atmospheres(5), in warm debris disks(6-9) or orbiting very closely(10-12), which has be

36 a reduction in the truncation radius of the disk(8,9) or by a reduction in the spatial extent of the

37 dy is the study designed to validate the IBD Disk, a visual tool easily useable in daily practice to

38 cts, and in fact led to small but measurable disk activations in V1 and V2 for disparity.

39 For disparity, disk activations were only found in V3, while suppressio

40 ower than for STEM images using conventional disk and annular detectors.

41 ulture primary HLA-G+ EVT from the placental disk and chorionic membrane from healthy term pregnancy.

42 ient will fill in the two questionnaires IBD Disk and IBD-DI at baseline, then between 3 and 12 month

43 s, with its C-terminus embedded within the Z-disk and its N-terminus extending out toward the thin fi

44 Electrochemical techniques with disk and nano-tip electrodes, together with calcium imag

45 ds and planets from a gas-rich circumstellar disk and the final distribution of their mass around the

46 t corona(4,5) positioned above its accretion disk, and then transitions to a soft (lower-energy) spec

47 emitting corona and the irradiated accretion disk are 6 to 20 times shorter than previously seen.

48 Similar accretion disks are expected to form in collapsars (the supernova-

49 How disks are formed within the cilium remains an area of ac

50 Protoplanetary disks are known to possess a variety of substructures in

51 bulk acoustic wave (BAW) modes of solid SiC disks are mostly free of bulk thermoelastic damping.

52 heir subsequent storage and transport in the disk, are still poorly understood, and their origin and

53 The detection(1) of a dust disk around the white dwarf star G29-38 and transits fro

54 (4) that gas flows inwards towards accretion disks around black holes, and such an inflow has been me

55 stant astronomical objects such as accretion disks around black holes.

56 Annular structures (rings and gaps) in disks around pre-main-sequence stars have been detected

57 les 15-90 degrees , and a multi-ink hydrogel disk array.

58 tiple annular substructures observed towards disks at young ages can act as an early foothold for dus

59 autoantibodies (AHAs) and anti-intercalated disk autoantibodies (AIDAs) are autoimmune markers in my

60 rom heterozygous to homozygous TC muscles, Z-disks become increasingly out of register while passive

61 0 ME, and 16 mE (27.6%) using the 2019 CLSI disk breakpoints.

62 inor errors (mE) (46.6%) using the 2019 CLSI disk breakpoints.

63 d localization of Connexin43 to intercalated disks) by activating canonical Wnt signaling.

64 multiplexed tri-mode signal outputs, the PT-Disk can quantify prostate specific antigen with limits

65 his study demonstrates the use of dual-fluid disk centrifuge photosedimentometry coupled with rheolog

66 or anti-CD61, were immobilized on monolithic disk columns for isolation of lipoproteins and extracell

67 IRS 63 also has a relatively large disk compared to other young disks (greater than 50 astr

68 at is accreting from a circumstellar gaseous disk composed of hydrogen, oxygen and sulfur at a rate o

69 e integrated Atomic Force (AFM) and spinning disk confocal (SDC) microscope.

70 different commercial wide-field and spinning-disk confocal microscopes, obtaining >10-fold improvemen

71 Using simultaneous two-color spinning-disk confocal microscopy, we monitor the DSB dynamics an

72 The PT-Disk consisted of a dissociative thermoresponsive hydrog

73 e is the boundary zone of the carbon working disk contacted by the paper crown soaked in the polyelec

74 Responsive hydrogel disks, containing patterned metal NPs, form characterist

75 e dynamics of the precessing inner accretion disk could play a role in either directly launching or r

76 ckdown strain with both flagellar length and disk defects.

77 MIC and disk diameter results were interpreted using United Stat

78 tudy was to evaluate oxacillin and cefoxitin disk diffusion (DD) and broth microdilution (BMD) method

79 upplemented fosfomycin Etest and Kirby-Bauer disk diffusion (DD) assays, and the results were compare

80 tin and oxacillin broth microdilution (BMD), disk diffusion (DD), and PBP2a immunoassay, and the resu

81 ine whether agar dilution, research-use-only disk diffusion (Mast Group Ltd., Bootle Merseyside, UK),

82 Comparison of EUCAST to CLSI for disk diffusion (with EUCAST used as the reference) showe

83 We evaluated the performance of disk diffusion and Etest compared to that of reference b

84 In general, the disk diffusion and Etest methods performed well with thi

85 According to the disk diffusion assay, the activity of both antibiotics w

86 actam disk mass of 30/20 mug was used in the disk diffusion assay.

87 arctic Streptomyces strains was evaluated by disk diffusion assays and minimum inhibitory concentrati

88 Current disk diffusion breakpoints (>=21/<=20 mm for susceptible

89 We assessed the ceftazidime-avibactam disk diffusion breakpoints that provide the lowest discr

90 linical and Laboratory Standard Institute by disk diffusion method.

91 Our objective was to compare cefiderocol disk diffusion methods (DD) to broth microdilution (BMD)

92 Broth microdilution (BMD) and disk diffusion methods have been developed to determine

93 eptibility tested by broth microdilution and disk diffusion methods in 3 laboratories.

94 Disk diffusion performed poorly relative to BMD under CL

95 2 study design, broth microdilution MIC and disk diffusion quality control (QC) ranges were determin

96 Interpretations of MIC or disk diffusion test results, such as "susceptible" or "r

97 modified carbapenem inactivation method, and disk diffusion with carbapenems.

98 n method, levofloxacin but not ciprofloxacin disk diffusion yielded an acceptable minor error rate of

99 Disk diffusion yielded inhibition zone diameter QC range

100 in 2017 (broth microdilution MIC) and 2019 (disk diffusion).

101 ement was 98.0% for agar dilution, 73.1% for disk diffusion, 96.3% for Etest, and 96.6% for MTS.

102 methods: agar dilution, broth microdilution, disk diffusion, and Etest.

103 boratories, most widely used AST methods are disk diffusion, gradient diffusion, broth dilution, or c

104 For disk diffusion, standard Mueller-Hinton agar is recommen

105 For ciprofloxacin disk diffusion, the categorical agreement (CA) was 46.6%

106 Also, an inverted disk-diffusion methodology was applied to overcome the l

107 If planets can form within the warped disk, disk tearing could provide a mechanism for forming

108 er post-treatment rinsing, the L-PRF-treated disks displayed a significant reduction in bacterial cou

109 Because the volume of the disks does not change on a millisecond timescale, their

110 Tillage methods included moldboard (MP), disk (DP) and sweep (SW), and the N application rates we

111 end-of-life magnet feedstocks including hard disk drives (HDDs), MRI, cell phone, bonded, swarf, and

112 rding, which enables ultrahigh-capacity hard disk drives(9).

113 s into high-capacity storage to replace hard disk drives, fuelling the expansion of the global storag

114 ated bioanalytical scanners based on compact disk drives.

115 ntribute to the highly curved rim domains at disk edges.

116 tion of ORR activity using standard rotating disk electrode (RDE) measurements.

117 l scavenging capabilities in a Rotating Ring-Disk Electrode (RRDE) electrochemical system against in-

118 In this work, a rotating ring disk electrode (RRDE) setup has been developed to study

119 oxidation reaction activity in both rotating disk electrode and membrane electrode assembly measureme

120 ptimal gel probe based on 25 mum diameter Pt disk electrode of R(g) ~ 2, the lateral physical resolut

121 en peroxide (H(2)O(2)) using a rotating ring-disk electrode, further work is needed to develop a non-

122 The gold disk electrodes (GDEs) with DET-type FADGDH prepared usi

123 The use of rotating disk electrodes (RDEs) is probably the most convenient w

124 -electrode distance and fusion pore size for disk electrodes are 239 and 11.5 nm, while for nanotip e

125 ments for planar and nanorod-structured gold disk electrodes at 100 Hz to 1 MHz frequency range and i

126 the sensors behaved almost identically to Au disk electrodes for the oxidation of an outer-sphere red

127 Platinum disk electrodes of different diameters and NaClO(4) supp

128 ow a slightly higher and narrower spike than disk electrodes when measuring exocytosis.

129 ning method, using replaceable glassy carbon disk electrodes, which enables the rapid and reliable ev

130 For motion, the disk elicited retinotopically organized activations star

131 These methods were a colistin broth disk elution (CBDE) and a colistin agar test (CAT), the

132 evaluate the accuracy of the colistin broth disk elution (CBDE) test compared to that of broth micro

133 Thus, we modified the colistin broth-disk elution (CBDE) test to screen for plasmid-mediated

134 ry, France) and (ii) the EDTA-colistin broth disk elution (EDTA-CBDE) screening test method.

135 ultra-soft and can be described by accretion disk emission with luminosity proportional to the fourth

136 We analyze 6 years' worth of Earth disk emissions at far ultraviolet wavelengths acquired b

137 e present a thorough analysis using the wing disk epithelium to show the consequences of modulating m

138 with diverse geometrical (cylindrical, bent, disk, etc.) and chemical (neutral, ionic, etc.) natures

139 lens capsule, and a shallow unilateral optic disk excavation.

140 ity of Ru(7)Ni(3)/C, as measured in rotating disk experiments, is about 21 and 25 times that of Pt/C,

141 (2) and spatially resolved(3) edge-on debris disk extending from about 35 to 210 astronomical units f

142 gest that the corona is compact and that the disk extends nearly to the central black hole(14,15).

143 The COMPASS CM clamps onto the nucleosome disk-face via an extensive interface to capture the flex

144 highly clustered at the myocyte intercalated disk, facilitating formation of Na(+) nanodomains in the

145 By dual-color spinning disk fluorescence microscopy with a time resolution of ~

146 he internal nanogrooved structure of Blu-ray disks for label-free immunosensing.

147 le studies that nudC is integral to rod cell disk formation and photoreceptor protein localization.

148 brane at the initiation of new outer segment disk formation.

149 6) delayed outflows from a remnant accretion disk formed around the newly born black hole(7-10) as th

150 en abundant species in the cold zones of the disk, [Formula: see text] or [Formula: see text] are onl

151 ationally, it has been difficult to identify disk galaxies in emission at high redshift(5,6) in order

152 Massive disk galaxies like the Milky Way are expected to form at

153 such a massive, rotationally supported, cold disk galaxy when the Universe was only 1.5 billion years

154 /C (LMNA); 24 (5%) structural cytoskeleton-Z disk genes; 16 (3.5%) desmosomal genes; 46 (9.5%) sarcom

155 rochemical biosensing electrodes (e.g., gold disk, glassy carbon electrode, etc.) can undergo sophist

156 19% ME, and 0 to 20% VME and varied based on disk, GNB, and BPs evaluated.

157 elatively large disk compared to other young disks (greater than 50 astronomical units)(10).

158 However, the IBD Disk has not been validated yet in clinical practice.

159 ic sciatica caused by herniation of a lumbar disk has not been well studied in comparison with acute

160 maller scales, inflows close to an accretion disk have been suggested to explain the results of recen

161 ons of inflows that actually reach accretion disks have been elusive.

162 series for the presence and degree of lumbar disk herniation and spinal nerve root impingement.

163 hat had lasted for 4 to 12 months and lumbar disk herniation at the L4-L5 or L5-S1 level in a 1:1 rat

164 %] vs 665 of 786 [85%]) for detecting lumbar disk herniation compared with standard CT (all compariso

165 um (VNCa) images for the detection of lumbar disk herniation compared with standard CT image reconstr

166 formance and confidence for depicting lumbar disk herniation compared with standard CT.

167 ting more than 4 months and caused by lumbar disk herniation, microdiskectomy was superior to nonsurg

168 t been well studied in comparison with acute disk herniation.

169 tient underwent repeat surgery for recurrent disk herniation.

170 a(+) and K(ATP) channels to the intercalated disk (ICD) of cardiomyocytes.

171 o the actin cytoskeleton at the intercalated disk (ICD), a unique cell-cell junction that couples car

172 disrupting ventricular myocyte intercalated disk (ID) nanodomains rich in cardiac sodium channels (N

173 chinery are concentrated at the intercalated disk (ID).

174 lar ring(1) expel matter and energy from the disk in the form of a galactic wind(2).

175 leading to the suggestion that the accretion disk in the hard-X-ray state of stellar-mass black holes

176 tion may already be underway in even younger disks in the class I phase, when the protostar is still

177 the past decade have detailed properties of disks in the earliest star-forming phases been observed(

178 performed with all reagents prestored on the disk, including cell-line-based DNA as quality control.

179 Disk instabilities may be more efficient in forming plan

180 Bennu's disk-integrated photometric phase function validates mea

181 ces are the primary hot-spots for nucleosome disk interactions, whereas nearly half of the nucleosome

182 of the media which are critical for the head-disk interface reliability.

183 Using state-of-the-art spinning disk intravital microscopy to delineate the different co

184 on the macula and RNFL near the optic nerve disk is investigated, there was significant thinning ide

185 Theoretical models predict that if the disk is misaligned with the orbital plane of the stars,

186 The composition of this disk is unlike all other known planetary debris around w

187 into the series of stacked, highly organized disks is critical for cell function and viability.

188 The biogenesis of these disks is initiated at the OS base, but the driving force

189 The first two PSD-95/disks large/zona occludens (PDZ) domains of PSD-95 have

190 r of wavelength 10.6 mum and a Trumpf Yb-YAG disk laser of wavelength 1.030 mum were used with a beam

191 horesis at locations radial to the electrode disk, leading to transport away from the electrode.

192 Spinning-disk live-cell imaging revealed that S. pneumoniae induc

193 the MIC assay, and a cefepime-enmetazobactam disk mass of 30/20 mug was used in the disk diffusion as

194 ested that an acidic patch on the nucleosome disk may be a common site for recruitment to chromatin,

195 Knockdown of the ventral disk MBP protein also causes severe structural defects t

196 nsion, the area expansion coefficient of the disk membrane also increases as thermally induced fluctu

197 he fractional shift of the charge across the disk membrane.

198 K(-1) near 100 K was measured using the hot disk method.

199 lizing an alternating current (ac) polarized disk microelectrode as a probe.

200 etween two types of electrodes, carbon fiber disk microelectrodes and nanotip conical-shape carbon fi

201 ding characteristics of the aptamer-modified disk-monoliths, resulting in the optimum binding pH and

202 NudC regulates photoreceptor disk morphogenesis and rhodopsin localization.

203 n for the continuity of rim formation during disk morphogenesis.

204 For weak confinements in disks, multiple continuously nucleating and annihilating

205 e cutaneous papillae located around the oral disk, nostril, gill pores, and on the dorsal fins and th

206 an isolated tissue volume (a 20 mm diameter disk of 5 mm thickness) representing a 20% increase in t

207 ng preferentially toward algae embedded in a disk of agar.

208 Here, we use the wing imaginal disk of Drosophila as a model to examine the functions t

209 oung stars are surrounded by a circumstellar disk of gas and dust, within which planet formation can

210 Whether or not planets already exist in the disk of IRS 63, it is clear that the planet-formation pr

211 et these observations in terms of a rotating disk of mass 10(-5) to 10(-4) solar masses and mean hydr

212 alization away from the A-band towards the Z-disk of the sarcomere.

213 that show four annular substructures in the disk of the young (less than 500,000 years old)(8) proto

214 components of gas in the upper layers of the disk of the young star HD 163296, as traced by emission

215 Pure disks of this material exhibit an outstanding activity f

216 ations of a planet co-existing with a debris disk offer the opportunity to test the predictions of cu

217 were embedded inside of a nanoporous ceramic disk on one end, while their free end was submerged in a

218 rradiation of the clip-magazine-assembled PT-Disk, on-chip photothermal effect of PB NPs triggered bo

219 diverse as old VHS tapes, modern hard-drive disks, or magnetic bands on credit cards.

220 results in short flagella, aberrant ventral disk organization, loss of the funis, defective axoneme

221 ctive study, 41 patients (243 intervertebral disks; overall mean age, 68 years; 24 women [mean age, 6

222 nferior temporal quadrant of the optic nerve disk (p = 0.020) in CVT patients compared to normal indi

223 tions, whereas nearly half of the nucleosome disk participates only minimally in protein binding.

224 , we asked whether the position of the solar disk per se is relevant for compass orientation in a mig

225 Disk potentiation testing was performed using sodium pho

226 osphorylation in important myofilament and Z-disk proteins with a linear correlation suggests PTM cro

227 tro (abnormal redistribution of intercalated disk proteins, myocyte apoptosis, release of inflammator

228 bundances in the gas phase of protoplanetary disks, providing important insights on the nonthermal pr

229 ly (methyl methacrylate) (PMMA)/paper hybrid disk (PT-Disk) was developed as a novel photothermal imm

230 atients (10.1%), consisting of increased cup-disk ratio (3.8%), vessel tortuosity (2.5%), retinal pig

231 ch immobilizes phytochemicals on glass fiber disks, reducing compound degradation, allowing long-term

232 The SiC disk resonators are anchored upon an acoustically-engine

233 Capacitively-transduced SiC BAW disk resonators consistently display gyroscopic m = 3 mo

234 -high quality-factors (Q) in gyroscopic-mode disk resonators.

235 f inhibition around a bacitracin-impregnated disk, respectively.

236 cifically organized as ectopic incisures and disk rims.

237 ing HER from water reduction with increasing disk rotation rate is responsible for the enhanced CO2RR

238 is an increase in selection latency when the disk's color changed smoothly compared to randomly.

239 h we subsequently validated using a rotating disk setup.

240 The biconcave disk shape of the mammalian red blood cell (RBC) is uniq

241 The electrolyte can be pumped through the disk-shaped gap between the ring working electrode and t

242 ilar strengths are obtained for the lens and disk-shaped implants in the higher spectrum.

243 nvestigate the acoustic signals generated by disk-shaped implants when stimulated by external US sour

244 nematic phase of a standard LLC composed of disk-shaped micelles.

245 s of each bird's trajectory by interposing a disk-shaped obstacle in its preferred flight path.

246 problems is examining an annular structure (disk-shaped such as a cell, vesicle or molecule) interac

247 ned with the orbital plane of the stars, the disk should warp and break into precessing rings, a phen

248 ce TED due to microscale roughness along the disk sidewalls.

249 KO mice showed replacement of intervertebral disk structures (annulus fibrosus and nucleus pulposus)

250 established comparing it with other compact disk structures.

251 "dense" interstellar clouds and protostellar disks surrounding forming stars because these environmen

252 e produced through the accretion of gas into disks surrounding supermassive black holes(1-3).

253 If planets can form within the warped disk, disk tearing could provide a mechanism for forming wide-

254 star system GW Orionis, finding evidence for disk tearing.

255 into precessing rings, a phenomenon known as disk tearing.

256 sity proportional to the fourth power of the disk temperature during long-term evolution.

257 ing precession of a vertically extended slim disk that arises from the super-Eddington accretion rate

258 vigated on a familiar, continuously rotating disk that dissociates the environment into two spatial f

259 ial outflow is seen at the outer edge of the disk that is potentially the base of a wind associated w

260 in hundreds of opsin-loaded stacked membrane disks that enable phototransduction.

261 In the context of disks, this question was posed nearly two decades ago an

262 protein that spans the half-sarcomere from Z-disk to M-band.

263 pe transformations, from initially biconcave disks to elongated and folded geometries with noncircula

264 al substantial flows from the surface of the disk towards its midplane at the radial locations of gap

265 e an accessible exemplar of an astrophysical disk, tracing the Saturn system's dynamical processes an

266 nsation times for AOAs are inconsistent with disk transport timescales, indicating that AOAs, and lik

267 to generate homozygous truncations in the Z disk (TTN-Z(-/-)) and A-band (TTN-A(-/-)) regions of the

268 res, the preparation and characterization of disk-type polished tips with the radius <~25 nm remains

269 of single Lactococcus lactis bacteria at Pt disk ultramicroelectrodes (UMEs) were characterized usin

270 riments of L. lactis using a 5 mum radius Pt disk UME in 2 mM ferrocenemethanol (FcM) with either 0.0

271 n experiments with steady-state oxidation at disk UMEs in low ionic strength solutions, electroosmoti

272 simulate, experimentally, ice processing in disks under realistic conditions, that is, layered ices

273 When tested on a ball-on-disk up to 230 m in distance, the composite new solid lu

274 were isolated by defining a central 2-degree disk using random-dot kinematograms and stereograms, res

275 0.1, and 0.5 wt%) manufactured into hydrogel disks using the two methods were shown to yield similarl

276 convection in the vicinity of the electrode disk (velocities >50 mum/s).

277 The IBD Disk was developed, a shortened and self-administered to

278 tinuously up the tubes even when the ceramic disk was elevated over 3 m above the reservoir.

279 l methacrylate) (PMMA)/paper hybrid disk (PT-Disk) was developed as a novel photothermal immunoassay

280 ng of condensation within the protoplanetary disk, we attribute these isotopic compositions to the ra

281 Results A total of 112 herniated lumbar disks were depicted at MRI.

282 sted, large grit, acid-etched (SLA) titanium disks were inoculated with subgingival dental plaque and

283 The disks were rinsed with 0.9% NaCl and exposed to the cell

284 Numerous flat steel disks were spray-coated with the new lubricant formulati

285 ticipants are asked to report the color of a disk when a cue was presented.

286 these are concentrated in the thin Galactic disk where the Sun resides.

287 ission from the geometrically thin accretion disk, which extends to the innermost stable circular orb

288 s capillary interactions between two or more disks, which are either attractive or repulsive dependin

289 d observation of molecules in protoplanetary disks, which can evolve toward solar systems like our ow

290 possess many hundreds of stacked membranous disks, which capture photons and scaffold the phototrans

291 Other psychometric criteria of the IBD Disk will also be analysed as its reliability or its dis

292 Recently, the discovery of a gaseous debris disk with a composition similar to that of ice giant pla

293 hich is highly expressed in the sarcomeric Z-disk with a major structural and functional role.

294 ises from gas inside a cold, dusty, rotating disk with a rotational velocity of about 272 kilometres

295 ll allow to evaluate the validity of the IBD Disk with respect to the IBD-DI in order to generalize i

296 micromagnetic simulations, we study an FeGe disk with two layers of different chirality.

297 is revealed by optical measurements on a SiC disk, with nanoscale smooth sidewalls, exhibiting Q = 18

298 report imaging of a 10(4)-kelvin ionized gas disk within 2 x 10(4) Schwarzschild radii, using the 1.3

299 o as to contact the outer edge of the carbon disk working electrode, as well as peripheral counter an

300 mulations that show that collapsar accretion disks yield sufficient r-process elements to explain obs