ライフサイエンスコーパス: kelvin

1 within a film are very small (less than one kelvin).

2 ium when cooling metallic K3C60 below Tc (20 kelvin).

3 ottest and coolest parts of its surface (200 kelvin).

4 ation climate models (about 1-3 per cent per kelvin).

5 of the cold dense molecular phase (10 to 100 kelvin).

6 s at still cooler temperatures (around 1,300 kelvin).

7 microwave background at that time (about 30 kelvin).

8 es from 5.5 to 3.3 kelvin and from 176 to 73 kelvin).

9 ronger than the seasonal variability (~a few Kelvins).

10 ions, even at temperatures greater than one kelvin.

11 91 kelvin at the hot-side temperature of 350 kelvin.

12 ide temperature of KELT-9b to be about 4,600 kelvin.

13 uilibrium temperature of approximately 2,500 kelvin.

14 id tin at temperatures of around 1,473-1,673 kelvin.

15 ic hydrogen at 495 gigapascals at 5.5 and 83 kelvin.

16 nt", later coined as Maxwell's demon by Lord Kelvin.

17 alue of 98 kelvin and reaches as high as 270 kelvin.

18 al gate set at temperatures greater than one kelvin.

19 and persisting up to temperatures of T > 50 kelvin.

20 ious estimates, at 18-44 watts per metre per kelvin.

21 he stage for the planned redefinition of the kelvin.

22 ut of a single qubit at one gigahertz at 4.2 kelvin.

23 ' in D2 occurs above 310 gigapascals and 300 kelvin.

24 t electric-field control of magnetism at 200 kelvin.

25 already at nearly ambient pressures at zero Kelvin.

26 us relative humidity levels up to 85% at 298 kelvin.

27 conductivity up to 1290 watts per meter per kelvin.

28 xtremely narrow excitonic linewidth below 50 kelvin.

29 allistic length of about 400 nanometres at 4 kelvin.

30 single-layer cuprate with the highest Tc, 95 kelvin.

31 time of 370 +/- 60 minutes was achieved at 2 kelvin.

32 ) and an effective temperature of 600 to 750 kelvin.

33 en the SST anomaly becomes greater than +0.5 Kelvin.

34 becoming dominant at temperatures above 220 kelvin.

35 rmed at low-temperature conditions below ~30 kelvin.

36 plasma transiently heated to almost 100,000 kelvin.

37 hock conditions to ~ 24 gigapascals and 2300 kelvin.

38 ically requires temperatures above about 250 kelvin.

39 component that seems to diverge at about 228 kelvin.

40 m temperature of the 21.8-day planet is ~350 kelvin.

41 ision of the experimental extrapolation to 0 kelvin.

42 th a mean brightness temperature of 29 +/- 5 kelvin.

43 l release 53 +/- 17 gigatonnes of carbon per kelvin.

44 the onset of an anomalous Hall signal at 50 kelvin.

45 at electron temperatures between 77 and 300 kelvin.

46 erved below critical temperatures of up to 3 kelvin.

47 Indian Ocean with a standard error of 0.0060 kelvin.

48 ting transition temperature of about 9 to 15 kelvin.

49 ) display temperature changes of less than 3 kelvin.

50 ed by intrinsic thermal fluctuations at 0.19 kelvin.

51 igapascals and high temperatures above 2,000 kelvin.

52 mples to 100-400 gigapascals and 2,000-3,000 kelvin.

53 ed matter at temperatures up to thousands of kelvins.

54 ntum coherence effects up to several tens of kelvins.

55 uperconducting transition temperature of 1.6 kelvin(5).

56 to existing alloys: 3.7 gigapascals at 1,000 kelvin(9,13).

57 out slowly, compression of ice I even at 100 kelvin (a region in which HDA typically forms) gives pro

58 The resistance divergence ends at about 3 kelvin, a behavior that may arise from surface conductan

59 n effective temperature of only around 3,050 kelvin, a luminosity of 0.15 per cent of that of the Sun

60 ting transition temperature of 287.7 +/- 1.2 kelvin (about 15 degrees Celsius) achieved at 267 +/- 10

61 yside brightness temperature of 1,040 +/- 40 kelvin and a nightside temperature consistent with zero

62 glass transition temperature of up to 1,162 kelvin and a supercooled liquid region of 136 kelvin tha

63 ), featuring a transition temperature of 1.6 kelvin and a very large and anisotropic upper critical f

64 eation temperature (TH) at approximately 232 kelvin and above about 160 kelvin, and where rapid ice c

65 2 other foam-based heterostructures based on Kelvin and C15 foams that have somewhat smaller but stil

66 y jets reach temperatures of at least ~10(5) kelvin and constitute an important element of the transi

67 at electron temperatures of 1.9-2.3 million kelvin and electron densities of (0.7-4.0) x 10(22) per

68 on would reduce these values from 5.5 to 3.3 kelvin and from 176 to 73 kelvin).

69 brown dwarfs have temperatures of 400 to 450 kelvin and masses almost equal to 5 to 20 times that of

70 s greatly enhanced from the bulk value of 98 kelvin and reaches as high as 270 kelvin.

71 s temperature of the planet to 1,380 +/- 400 kelvin and the temperature of the warmest hemisphere (ce

72 o well-known equatorially trapped waves, the Kelvin and Yanai modes, owing to the breaking of time-re

73 stability at high temperatures (up to 1,373 kelvin) and achieving high-throughput production of mono

74 Yet, the very high temperatures (>3140 kelvin) and chemical reactivity of molten UO2 have preve

75 ) kelvin), warm ionized(5,6) (10(4) to 10(5) kelvin) and cool atomic(7,8) (10(3) to 10(4) kelvin) gas

76 A large reservoir of hot (10(7) kelvin) and cooler (10(2) to 10(4) kelvin) gas surrounds

77 de and nightside of the substellar donor (57 kelvin) and the maximum difference between the hottest a

78 ype stars (with temperatures of 7,300-10,000 kelvin), and no planets are known to transit the even ho

79 elting temperature(7-13) to several thousand kelvin, and (3) favours new ice structures with a close-

80 m [Formula: see text] to [Formula: see text] kelvin, and determined a photospheric velocity of roughl

81 ce I to 11 kilobar at temperatures below 130 kelvin, and the process was described as thermodynamic m

82 V in H2 and HD up to 388 gigapascals at 300 kelvin, and up to 465 kelvin at 350 gigapascals; we do n

83 approximately 232 kelvin and above about 160 kelvin, and where rapid ice crystallization has prevente

84 king-disordered critical crystallites at 230 kelvin are about 14 kilojoules per mole of crystallite m

85 th effective temperatures of less than 2,700 kelvin are referred to as 'ultracool dwarfs'.

86 200 nanometers) and temperatures (10 to 300 kelvin) are consistent with the classically expected beh

87 coherence times (up to 8.4 microseconds at 5 kelvin) are obtained at unusually high concentrations.

88 temporal increase of tropic temperature (~10 Kelvins) around the tropopause of Saturn (i.e., 50 mbar)

89 ns of filamentary structures of gas at 10(7) kelvin associated with the galaxy cluster Abell 2744.

90 th a confirmed transition temperature of 203 kelvin at 155 gigapascals(3,6).

91 rconducting transition temperature Tc of 203 kelvin at 155 gigapascals--the highest Tc reported for a

92 388 gigapascals at 300 kelvin, and up to 465 kelvin at 350 gigapascals; we do not observe phase V in

93 netic hysteresis at temperatures of up to 60 kelvin at a sweep rate of 22 oersted per second.

94 1.5 kelvin in the unstrained material to 3.4 kelvin at compression by approximately 0.6%, and then fa

95 at critical temperatures between 240 and 320 kelvin at megabar pressures(3-6).

96 ice displays Mott insulating states below 20 kelvin at one-quarter and one-half fillings of the state

97 ured kappa greater than 1600 watts per meter-kelvin at room temperature in samples with enriched (10)

98 n ten, reaching about 4 and 6 microvolts per kelvin at room temperature, respectively, close to the h

99 oduced a large temperature difference of ~91 kelvin at the hot-side temperature of 350 kelvin.

100 constant persists to temperatures of several kelvin at zero magnetic field.

101 a nightside temperature consistent with zero kelvin (at one standard deviation).

102 be about 1,300 kelvin hotter (2,700 +/- 270 kelvin) at a wavelength of 4.5 micrometres, which indica

103 As the particles increase in size and the Kelvin barrier falls, subsequent growth is primarily due

104 the planet's temperature is much lower, <60 Kelvin, because the host star is only 0.10 to 0.15 solar

105 at the vacuum-solid interface often at a few Kelvin, but is not a notion immediately associated with

106 u theory) above the Curie temperature of 290 kelvin by electric fields of 29.0 volts per micrometre.

107 manipulation on bilayer NaCl on Cu(111) at 5 kelvin by eliminating carbon monoxide from a cyclocarbon

108 sound in graphite at temperatures above 100 kelvins by using time-resolved optical measurements of t

109 +x at above the transition temperature of 52 kelvin causes a simultaneous increase and decrease in th

110 The increase of around 50 kelvin compared with the previous highest critical tempe

111 lvin for starting temperatures that span 176 kelvin (complete thermalization would reduce these value

112 re evacuated at temperatures from 525 to 575 kelvin, conditions under which formate is not stable on

113 Kelvin considered it unlikely that sufficient time had e

114 ion experiments reach ~200 mK, the first sub-Kelvin cooling with any molecular nanomagnet, and reveal

115 he afternoon, and the presence of a possible Kelvin (curvature) effect, which inhibits organic vapour

116 rvations of ~0.02 solar masses of warm (~100 kelvin) dust seen near the center of the ~10,000-year-ol

117 This Kelvin effect is analogous to the electrochemical behavi

118 by organic surfactants, which diminishes the Kelvin effect, is expected to be negated by a concomitan

119 or increasing solute concentration, and the Kelvin effect, whereby activation potential decreases wi

120 he IRI of AF(G)P-inspired Au colloids to the Kelvin effect.

121 here with a virial temperature of 60 million Kelvin, enriched with metals to the same extent as are l

122 plets, to show that the applicability of the Kelvin equation extends to unexpectedly small lengths, o

123 and so of particular practical interest, the Kelvin equation is expected to break down because the re

124 at this scale, we find that the macroscopic Kelvin equation using the characteristics of bulk water

125 The century-old Kelvin equation(5) is frequently used to describe conden

126 scription of the vapor pressure based on the Kelvin equation.

127 tion approach implemented in program package KELVIN, especially designed for complex pedigrees, sever

128 s the metallic phase to temperatures below 5 kelvin, even after the ionic liquid is completely remove

129 GJ 436b is a warm--approximately 800 kelvin--exoplanet that periodically eclipses its low-mas

130 /- 1 Jupiter masses) and coldest (850 +/- 50 kelvin) exoplanets to have been directly imaged.

131 Theoretically, connecting the zero-kelvin, first-principles-based, microscopic quantities o

132 tantially-from 240 kelvin for LuFe2O4 to 281 kelvin for (LuFeO3)9/(LuFe2O4)1.

133 nce of itinerant ferromagnetic order below 4 kelvin for doping beyond the superconducting dome in thi

134 ransition temperature substantially-from 240 kelvin for LuFe2O4 to 281 kelvin for (LuFeO3)9/(LuFe2O4)

135 egrees W) can consequently be reduced by 0.6 Kelvin for one-year predictions.

136 .5 kelvin near room temperature and exceed 3 kelvin for starting temperatures that span 176 kelvin (c

137 f superconductivity ('domes') emerge below 1 kelvin for the electron- and hole-doped sides of the one

138 o-range by atomic force microscopy (AFM) and Kelvin force microscopy (KFM).

139 ntact-mode atomic force microscopy (AFM) and Kelvin force microscopy (KFM).

140 UV and X-ray photoelectron spectroscopy, and Kelvin force microscopy to characterize the bulk and sur

141 anion, LkCa 15 b, evincing hot (about 10,000 kelvin) gas falling deep into the potential well of an a

142 ot (10(7) kelvin) and cooler (10(2) to 10(4) kelvin) gas surrounds it within a few parsecs(3).

143 kelvin) and cool atomic(7,8) (10(3) to 10(4) kelvin) gas.

144 ressures greater than 325 gigapascals at 300 kelvin, H2 and hydrogen deuteride (HD) transform to a ne

145 etary disk (at temperatures of more than 100 kelvin) has not hitherto been seen, as it generally lies

146 s transition temperatures greater than 1,000 kelvin have been developed, but the supercooled liquid r

147 xide snow-line (at temperatures of around 20 kelvin) have recently been imaged in the disks surroundi

148 the lower layers of vegetated canopies, (ii) Kelvin-Helmholtz as well as attached eddies near the veg

149 Turbulence through Kelvin-Helmholtz instabilities occurring at the interfac

150 ity analysis suggested that the ripples were Kelvin-Helmholtz Instabilities.

151 too small for spontaneous reconnection, the Kelvin-Helmholtz instability driven by a super-Alfvenic

152 ed that the non-linear vortex flows from the Kelvin-Helmholtz instability gives rise to vortex-induce

153 er higher than previous expectations for the Kelvin-Helmholtz instability.

154 f surface structures is equal or above (1/4) Kelvin-Helmholtz wavelength.

155 less likely at the dayside magnetopause, and Kelvin-Helmholtz waves (KHWs) may be important agents fo

156 ields maps with a statistical precision of 3 kelvin/hertz(-1/2), an accuracy of 10%, and nanometer-sc

157 U0 is going to zero at the extrapolated zero-kelvin Hirr value.

158 (centred on the hot spot) to be about 1,300 kelvin hotter (2,700 +/- 270 kelvin) at a wavelength of

159 ve thermopower of 17.0 millivolts per degree Kelvin in a flexible, quasi-solid-state, ionic thermoele

160 drives the thermal phase transition near 200 kelvin in Cd2Re2O7 and induces a parity-breaking lattice

161 limates but decreasing DeltaT by 1.5 +/- 0.2 kelvin in dry climates.

162 the discovery(1) of superconductivity at 203 kelvin in H(3)S, attention returned to conventional supe

163 at high temperatures ranging from 240 to 340 kelvin in metallic vanadium dioxide in the vicinity of i

164 te appears below the Neel temperature of 150 kelvin in NiPS(3), an antiferromagnetic van der Waals ma

165 The broken symmetry that develops below 17.5 kelvin in the heavy-fermion compound URu(2)Si(2) has lon

166 hile being heated from 10 kelvin to over 100 kelvin in the mid-plane, but it has hitherto not been po

167 id water down to temperatures of 227(-1)(+2) kelvin in the previously largely unexplored no man's lan

168 nsition temperature (Tc) increasing from 1.5 kelvin in the unstrained material to 3.4 kelvin at compr

169 dichalcogenide WTe2: 452,700 per cent at 4.5 kelvins in a magnetic field of 14.7 teslas, and 13 milli

170 14.7 teslas, and 13 million per cent at 0.53 kelvins in a magnetic field of 60 teslas.

171 nsiently induced up to room temperature (300 kelvin) in YBa2Cu3O6+x.

172 ation: illumination that produces only a sub-Kelvin increase in average temperature can reduce, by ma

173 Here we report imaging of a 10(4)-kelvin ionized gas disk within 2 x 10(4) Schwarzschild r

174 existence of a halo of warm (roughly 500,000 kelvin) ionized gas around the LMC (the 'Magellanic Coro

175 Its Curie temperature of 45 kelvin is only slightly lower than that of the bulk crys

176 o below temperatures of 0.03J, where J ~ 200 kelvin is the copper-copper superexchange interaction.

177 -linear resistivity, the scattering rate per kelvin is well approximated by the ratio of the Boltzman

178 extreme temperatures (more than about 1,300 kelvin) is impractical for many applications.

179 r, which develops at temperatures below ~150 kelvin, is essentially two dimensional, at lower tempera

180 d a high phase-transition temperature of 406 kelvin (K) (16 K above that of BTO).

181 ion of collision energy over the range 0.005 kelvin (K) to 30 K and of individual Ca fine-structure l

182 bond cleavage at temperatures as low as 150 kelvin (K).

183 ng fast laser heating before quenching to 70 kelvin (K).

184 ally improved the zT to 1.86 +/- 0.15 at 320 kelvin (K).

185 Starting with Gauss and Kelvin, knots in fields were postulated to behave like p

186 ensity plasma at temperatures of 10(5)-10(7) kelvin, known as the warm-hot intergalactic medium.

187 As they cool below about 2,300 kelvin, liquid or crystalline particles composed of calc

188 or stars with temperatures of 4,500 to 6,750 kelvin, log surface gravities of 2.5 to 4.5 (cgs units)

189 ghly turbulent reservoirs of cool (about 100 kelvin), low-density gas, extending far (more than 10 ki

190 te, increasing daytime DeltaT by 3.0 +/- 0.3 kelvin (mean and standard error) in humid climates but d

191 Therefore, Kelvin microscopy, under variable humidity, is a rigorou

192 ctivity in vacuum [~2.4 milliwatts per meter-kelvin (mW/m.K)] and in air (~20 mW/m.K).

193 s, and electron temperatures were below 1160 kelvin near closest approach.

194 ge central area of the capacitor peak at 5.5 kelvin near room temperature and exceed 3 kelvin for sta

195 lycol, are about 389 joules per kilogram per kelvin near room temperature.

196 was increased suddenly by even a few degrees Kelvin, nuclei displayed a repeatable and reversible tem

197 expected cooling rates of ten to a thousand kelvin per hour.

198 ent, reaching a value of about 5 amperes per kelvin per metre with a logarithmic temperature dependen

199 he magnitude of summer cooling via mixing (4 kelvin per month) is equivalent to that required to coun

200 e, observed up to temperatures exceeding 290 kelvin, persists for hours after the optical pump is int

201 e what is up and down, even in the cool 6000-kelvin photosphere just above the solar surface: This re

202 atial mapping of skin temperature with milli-Kelvin precision (+/-50 mK) and sub-millimetre spatial r

203 We demonstrate that frequency-modulated Kelvin probe force microscopy (FM-KPFM) provides more ac

204 Kelvin probe force microscopy (KPFM) has provided deep i

205 C resistance, AC impedance spectroscopy, and Kelvin Probe Force Microscopy (KPFM), demonstrate differ

206 ondary ion mass spectrometer (HIM-SIMS) with Kelvin probe force microscopy (KPFM), we demonstrate tha

207 scanning probe microscopy techniques such as Kelvin probe force microscopy (KPFM).

208 force detection to form peak force infrared-Kelvin probe force microscopy (PFIR-KPFM), which enables

209 Mapping surface potential with time-resolved Kelvin probe force microscopy (tr-KPFM) in LiNbO3 period

210 ealed by scanning probe microscopy, scanning Kelvin probe force microscopy and first-principle calcul

211 Kelvin probe force microscopy and Raman mapping confirm

212 By combining Kelvin probe force microscopy imaging and phase-field si

213 ys can be use as ultrasensitive platform for Kelvin probe force microscopy in sensing experiments.

214 On a local scale, Kelvin probe force microscopy provides a complete and de

215 2'''-quaterthiophen-5,5'''-diyl)] films with Kelvin probe force microscopy to highlight the role of t

216 Using frequency-modulated Kelvin probe force microscopy we were able to resolve th

217 nation of piezoresponse force microscopy and Kelvin probe force microscopy, we demonstrate that the s

218 e-domain spectroscopy mapping and calibrated Kelvin probe force microscopy.

219 states across the interface, as revealed by Kelvin probe force microscopy.

220 nanoelectrical characterization technique of Kelvin probe force microscopy.

221 by the surface potential change assessed by Kelvin probe force microscopy.

222 ditions by using atomic force microscopy and Kelvin probe force microscopy.

223 mission spectroscopy of material energetics, Kelvin probe measurements of work function, Mott-Schottk

224 on of the charge distribution using scanning Kelvin probe microcopy (SKPM) were performed.

225 resolved infrared spectroscopy, and scanning Kelvin probe microscopy are used to investigate the drif

226 ission electron microscopy, in situ scanning Kelvin probe microscopy characterization, and phase-fiel

227 Kelvin probe microscopy displays that in the presence of

228 A method based on scanning Kelvin probe microscopy is developed to probe the effect

229 responding WF change is measured by scanning Kelvin probe microscopy.

230 Kelvin probe spectroscopy measurements indicate that ele

231 atalytic behavior was studied using scanning kelvin probe technique.

232 tation and external injection is obtained by Kelvin-probe and scanning-capacitance microscopies.

233 On the basis of Kelvin-probe force microscopic potential characterizatio

234 s originally introduced as a solution to the Kelvin problem of finding the 3D tessellation composed o

235 s phases at temperatures of less than 10,000 kelvin reaching distances of 20 kiloparsecs and velociti

236 ith ZT ranging from 0.7 to 2.0 at 300 to 773 kelvin, realized in hole-doped tin selenide (SnSe) cryst

237 thermal hysteresis loops of more than a few Kelvin remains relatively uncommon and unpredictable, so

238 mperatures of up to 90 gigapascals and 1,300 kelvin, respectively.

239 Sb(67)Te(26) and Ge(15)Sb(85) at 660 and 610 kelvin, respectively.

240 brought the collision temperature down to 1 kelvin, restricting scattering to s and p partial waves.

241 louds ahead of the MJO center, enhancing the Kelvin-Rossby wave feedback.

242 ent, as measured with an approximately 1,455-kelvin silicon carbide emitter.

243 ping threshold as low as 27 nanowatts at 130 kelvin, similar to the value achieved in quantum-dot PCC

244 ease: the change in [Formula: see text]O per Kelvin temperature increase reduces with DO event amplit

245 ng tunnelling microscopy measurements at sub-kelvin temperatures and high magnetic fields on the II-V

246 down the long-time monopole dynamics at sub-Kelvin temperatures.

247 ially-Mars was moderately hotter (100 to 200 kelvin) than it is today, and that its mantle sluggishly

248 ron oxide (FeO2) at 76 gigapascals and 1,800 kelvin that holds an excessive amount of oxygen.

249 elvin and a supercooled liquid region of 136 kelvin that is wider than that of most existing metallic

250 n iron and water at 86 gigapascals and 2,200 kelvin that produces FeO2Hx.

251 2 Near the phase-transition temperature (190 kelvin), the energy of the electronic mode fell to zero

252 At low temperature (<1 kelvin), the thermal conductivity resembles that of a di

253 At approximately 10,170 kelvin, the host star is at the dividing line between st

254 e young Universe had fallen below some 4,000 kelvin, the ions of the light elements produced in Big B

255 er" (HO) phase below the temperature of 17.5 kelvin; the symmetry of the associated order parameter h

256 Below a few kelvin, these universal properties have been successfull

257 ecs, depositing metal-enriched gas at 10,000 kelvin through an hourglass-shaped nebula that resembles

258 ysteresis temperatures have increased from 4 kelvin to only about 14 kelvin using a consistent magnet

259 pe into the disk, while being heated from 10 kelvin to over 100 kelvin in the mid-plane, but it has h

260 anging from the universal Wigner laws near 0 kelvin to the occurrence of scattering resonances at hig

261 in the deeply supercooled regime (below 228 kelvin) to explain many of the anomalies of water(2) (su

262 the melting temperature of the matrix (1,356 kelvin) under an applied stress ranging from 0.85 per ce

263 ely cool (temperatures of the order of 10(4) kelvin), unshocked gas streaming along filaments of the

264 ave increased from 4 kelvin to only about 14 kelvin using a consistent magnetic field sweep rate of a

265 amorphous ice to temperatures of 205 +/- 10 kelvin, using an infrared femtosecond laser.

266 e cycle of myosin motors with a viscoelastic Kelvin-Voigt element that represents the stress fiber.

267 nertial impedance is considered along with a Kelvin-Voigt link with a hydration layer.

268 Furthermore, the Kelvin-Voigt model was introduced to interpret the PEK b

269 o describe the undulatory motion have used a Kelvin-Voigt model, where the elastic and viscous compon

270 ly ionized(3,4) (temperatures of about 10(6) kelvin), warm ionized(5,6) (10(4) to 10(5) kelvin) and c

271 rican monsoon, and the resulting atmospheric Kelvin wave drives equatorial westerly wind anomalies ov

272 slope currents that flow in the direction of Kelvin wave propagation.

273 reinforces the PJ pattern via a tropospheric Kelvin wave.

274 uantized vortices and subsequent emission of Kelvin waves along the vortices are thought to be centra

275 model experiments show that the downwelling Kelvin waves caused by strong westerly wind events over

276 e, we have directly observed the emission of Kelvin waves from quantized vortex reconnection.

277 n and enhancing eastward-propagating oceanic Kelvin waves in the tropical Pacific.

278 atory scale, and partly because WT among the Kelvin waves on quantized vortices is believed to play a

279 s precipitation anomalies were attributed to Kelvin waves only.

280 oding, the enhanced precipitation related to Kelvin waves was found in over 90% of flood events.

281 ity of analyzed floods, convectively coupled Kelvin waves, large scale precipitation systems propagat

282 gigapascals and temperatures of 2200 to 2400 kelvin, we found that such perovskite is unstable; it lo

283 In boreal spring, SST rises by 2 kelvin when heating of the upper ocean by the atmosphere

284 'no man's land' regime, between 145 and 200 kelvin, where kinetics are faster-resulting in crystalli

285 rdering on supercooling to approximately 229 kelvin, where the number of droplets containing ice crys

286 Water was activated over alpha-MoC at 303 kelvin, whereas carbon monoxide adsorbed on adjacent Au

287 to the boiling point of liquid nitrogen (77 kelvin), which is a record for the iron-based supercondu

288 -type star with a temperature of about 7,430 kelvin, which hosts the hottest known transiting planet,

289 h a peak figure of merit (ZT) of ~0.9 at 350 kelvin, which is comparable to the commercial bismuth te

290 htly lower than that of the bulk crystal, 61 kelvin, which is consistent with a weak interlayer coupl

291 The phenomenon persists above 100 kelvin, which is consistent with the predicted critical

292 optical spectroscopy of a hot (about 27,750 kelvin) white dwarf, WD J091405.30+191412.25, that is ac

293 using very fast sweep rates (for example, 30 kelvin with 200 oersted per second).

294 - 2.1 electron volts at a temperature of 5.5 kelvin, with a corresponding electron carrier density of

295 tween protein and solvent dynamics above 160 kelvin, with fast solvent motions, slow protein side-cha

296 sible wavelength on an energy scale of a few kelvin, with wavelength fluctuations coupled to pairing

297 ty with a critical temperature of around 250 kelvin within the [Formula: see text] structure of LaH(1

298 ate helical topological polaritons up to 200 kelvin without external magnetic field in monolayer WS(2

299 The hot (10(7) to 10(8) kelvin), X-ray-emitting intracluster medium (ICM) is the

300 , a theoretical analysis of the observed sub-Kelvin zero-field hysteretic spin dynamics of {Cr(III)Dy