ライフサイエンスコーパス: kelvin

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

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

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

4 e orders of magnitude larger (millivolts per kelvin).

5 D'' is relatively cold (DeltaT = 700 +/- 100 kelvin).

6 eme conditions (for example, from P4 at 1100 kelvin).

7 kelvin) and the Oort Cloud (approximately 10 kelvin).

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

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

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

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

12 allistic length of about 400 nanometres at 4 kelvin.

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

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

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

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

17 becoming dominant at temperatures above 220 kelvin.

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

19 plasma transiently heated to almost 100,000 kelvin.

20 hock conditions to ~ 24 gigapascals and 2300 kelvin.

21 ically requires temperatures above about 250 kelvin.

22 component that seems to diverge at about 228 kelvin.

23 ision of the experimental extrapolation to 0 kelvin.

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

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

26 e when the exciton gas is cooled below a few kelvin.

27 ethane and propylene/propane mixtures at 318 kelvin.

28 free-radicals at temperatures as high as 190 kelvin.

29 values (3 to 8 tesla) at a temperature of 4 kelvin.

30 have effective temperatures of around 5,000 kelvin.

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

32 o show ferroelectric switching, all below 71 kelvin.

33 ce (less than 1 decibel) between 300 and 400 kelvin.

34 tter with a hotter (unseen) phase at >>10(6) kelvin.

35 and longitudinal temperature contrasts of 16 kelvin.

36 h peak surface temperatures from ~250 to 300 kelvin.

37 n extraordinary zT value of 1.8 at about 850 kelvin.

38 lly insulating at temperatures less than 125 kelvin.

39 omain at temperatures ranging from 20 to 300 kelvin.

40 primordial gas for temperatures below 10(4) kelvin.

41 ctive temperatures exceeding several hundred kelvin.

42 bsurface temperatures are estimated to be 38 kelvin.

43 were observed at temperatures as high as 400 kelvin.

44 ternal magnetic field up to approximately 50 kelvin.

45 y, at operating temperatures from 80 to 1900 kelvin.

46 ure at approximately 118 gigapascals and 300 kelvin.

47 ing of zT in p-type PbTe to above 1.5 at 773 kelvin.

48 r conductance per chain was 50 picowatts per kelvin.

49 ary temperature is estimated at 3950 +/- 200 kelvin.

50 ncrease at a much slower rate of 1 to 3% per kelvin.

51 ata for Venus indicate values of 3.6 +/- 0.6 kelvin.

52 at 615 km with a temperature minimum of 114 kelvin.

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

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

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

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

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

58 he stage for the planned redefinition of the kelvin.

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

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

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

62 already at nearly ambient pressures at zero Kelvin.

63 uilibrium temperature of approximately 2,500 kelvin.

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

65 conductivity up to 1290 watts per meter per kelvin.

66 at the core-mantle boundary of 5400 +/- 600 kelvins.

67 eters) and entropy (19 +/- 4 joules mole(-1) kelvin(-1)) can be estimated.

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

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

70 unusual inherent Mott MIT is observed at 130 kelvin, also on cooling but without a simultaneous latti

71 we found temperature changes of 42.0 +/- 8.0 kelvin and 19.2 +/- 3.6 kelvin for Earth and Mars, respe

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

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

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

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

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

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

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

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

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

81 equilibrium temperatures of approximately 40 kelvin) and the Oort Cloud (approximately 10 kelvin).

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

83 .5 picoseconds), the temperatures (up to 366 kelvin), and the amplitudes of atomic vibrations (up to

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

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

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

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

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

89 hen sublimation temperatures of at least 180 kelvin are required.

90 200 nanometers) and temperatures (10 to 300 kelvin) are consistent with the classically expected beh

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

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

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

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

95 388 gigapascals at 300 kelvin, and up to 465 kelvin at 350 gigapascals; we do not observe phase V in

96 diating with a temperature of about 17 to 23 kelvin at a rate of about 220 times the luminosity of th

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

98 1.5 kelvin in the unstrained material to 3.4 kelvin at compression by approximately 0.6%, and then fa

99 as small as 0.05 watts per meter per degree kelvin at room temperature, 30 times smaller than the c-

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

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

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

103 We used a second-order generalized Kelvin body to model tether-force behavior from which se

104 t only ferroelectric (with Tc as high as 250 kelvin) but also polarize the quantum paraelectric SrTiO

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

106 gh ZT values in the range 1.5-1.8 at 750-900 kelvin, but still falls short of the generally desired t

107 Tc was tuned by approximately 500 kelvin by varying the thicknesses of the BaTiO3 and SrTi

108 Kelvin calculated the age of the Earth to be about 24 mi

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

110 ions at extremely low temperatures (10 to 20 kelvin), characteristic of cold molecular clouds and the

111 ums to radiation temperatures of 3.3 million kelvin, compressing 1.8-millimeter-diameter capsules by

112 By using an energetic argument and a Kelvin condensation model, the quasi-equilibrium liquid-

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

114 Kelvin considered it unlikely that sufficient time had e

115 n of a vapor cloud at a temperature of ~1000 kelvin, containing ~570 kilograms (kg) of carbon monoxid

116 y, we show that "warm-hot" plasma at 10(5.5) kelvin contains 10 to 150 times more mass than the cold

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

118 imately 10 megabars and approximately 10,000 kelvin, cotunnite-type SiO2 should have thermally activa

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

120 ide thermal anomaly (DeltaT(max) ~300 to 400 kelvin) deep in the transition zone west of Hawaii sugge

121 ange of more than 55 joules per kilogram per kelvin degree and adiabatic temperature change of more t

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

123 This Kelvin effect is analogous to the electrochemical behavi

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

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

126 ly assigned, the superconducting state at 38 kelvin emerges directly from a localized electron antife

127 med at temperatures of a few hundredths of a kelvin, engineered nanomechanical resonators coupled to

128 as up to several hundred to several thousand kelvin, ensuring that the fragmentation produces relativ

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

130 TEM-derived particle size using the modified Kelvin equation for particles in the size range of 5-40

131 Based on the modified Kelvin equation, the surface tension of Ag NPs was found

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

133 sured TEM sizes as predicted by the modified Kelvin equation.

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

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

136 d graphene, 3000 to 5000 watts per meter per kelvin, exceeds that of diamond and graphite.

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

138 /- 1 Jupiter masses) and coldest (850 +/- 50 kelvin) exoplanets to have been directly imaged.

139 r disk, where temperatures were less than 30 kelvin, experienced ultraviolet irradiation exposures an

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

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

142 nges of 42.0 +/- 8.0 kelvin and 19.2 +/- 3.6 kelvin for Earth and Mars, respectively.

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

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

145 Upper limits of 140 kelvin (for a filled pixel) are derived for the temperat

146 lative humidity (RH), as determined by using Kelvin force microscopy (KFM).

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

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

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

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

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

152 merger process, the fields are amplified by Kelvin-Helmholtz instabilities beyond magnetar field str

153 Turbulence through Kelvin-Helmholtz instabilities occurring at the interfac

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

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

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

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

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

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

160 events, azimuthal rotations consistent with Kelvin-Helmholtz waves along the magnetopause, and exten

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

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

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

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

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

166 solution and conformationally frozen near 10 kelvin in gas-phase clusters.

167 observed with a magnitude of microvolts per kelvin in magnetically ordered materials, ferromagnetic

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

169 trate a ZT value of approximately 2.2 at 915 kelvin in p-type PbTe endotaxially nanostructured with S

170 gnitude in oxygen fugacity and of 100 to 200 kelvin in temperature.

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

172 and 1900 kelvin to 2200 kilometers and 2300 kelvin in the lower mantle.

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

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

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

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

177 14.7 teslas, and 13 million per cent at 0.53 kelvins in a magnetic field of 60 teslas.

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

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

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

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

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

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

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

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

186 Previous studies suggest 3 kelvin (K) as the best estimate, 2 to 4.5 K as the 66% p

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

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

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

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

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

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

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

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

195 +/- 0.74 (2sigma) watts per square meter per kelvin, meaning that it is likely positive.

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

197 o temperatures between ~0.02 and 0.1 million kelvin (MK) and a small but sufficient fraction to tempe

198 layer exists at a temperature of millions of kelvins, much hotter than the solar surface we observe.

199 emperature to be +8.7 +/- 2.1 microvolts per kelvin (muV/K), +12.9 +/- 2.2 muV/K, and +14.2 +/- 3.2 m

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

201 ill as high as about 600 watts per meter per kelvin near room temperature, exceeding those of metals

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

203 atmosphere will increase at a rate of 7% per kelvin of surface warming.

204 T occurs in the bulk at a temperature of 154 kelvin on cooling.

205 ty plasma at temperatures in excess of 10(6) kelvin on inertial-confinement timescales using an X-ray

206 outh polar troughs at temperatures up to 145 kelvin or higher, making Enceladus only the third known

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

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

209 rmly heat a metallic glass at rates of 10(6) kelvin per second to temperatures spanning the undercool

210 onstrate a giant electrocaloric effect (0.48 kelvin per volt) in 350-nanometer PbZr(0.95)Ti(0.05)O3 f

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

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

213 The Kelvin probe force microscope is a tool for measuring lo

214 The Kelvin probe force microscope presented here is based on

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

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

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

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

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

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

221 Kelvin probe force microscopy and Raman mapping confirm

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

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

224 Using the scanning probe technique known as Kelvin probe force microscopy it is possible to successf

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

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

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

228 nanoelectrical characterization technique of Kelvin probe force microscopy.

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

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

231 electrochemical cells (LECs) using Scanning Kelvin Probe Microscopy (SKPM) and compare the results a

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

233 Kelvin probe microscopy displays that in the presence of

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

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

236 Kelvin probe spectroscopy measurements indicate that ele

237 opy, inverse photoemission spectroscopy, and Kelvin probe techniques.

238 90 K the ions began moving, as measured by a Kelvin probe.

239 n of 30 to 200 square meters to at least 950 kelvin, providing a sustained heat source for the sublim

240 imum magma temperatures in the 1150- to 1335-kelvin range, consistent with basaltic composition.

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

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

243 a with temperatures of 10(5) kelvin to 10(7) kelvin) residing in low-redshift filaments has been obse

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

245 inement of data collected between 293 and 30 kelvin revealed a total of eight symmetry-independent ad

246 this time span, in surprising agreement with Kelvin's result, the Earth cooled by about 4,000 K in re

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

248 Kelvin-solid models produced better predictions of tempo

249 Kelvin-solid models, especially the Prony Series model a

250 ops where this boundary extrapolates to zero Kelvin, suggesting that fluctuations associated with thi

251 eciprocal of the denaturation temperature in Kelvin, T(max), and the water volume fraction, epsilon (

252 ct region as a result of a approximately 500-kelvin temperature increase.

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

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

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

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

257 2 Near the phase-transition temperature (190 kelvin), the energy of the electronic mode fell to zero

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

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

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

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

262 (a sparse plasma with temperatures of 10(5) kelvin to 10(7) kelvin) residing in low-redshift filamen

263 from about 1000 kilometers in depth and 1900 kelvin to 2200 kilometers and 2300 kelvin in the lower m

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

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

266 n hold approximately 83 liters of CO2 at 273 kelvin under ambient pressure.

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

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

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

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

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

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

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

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

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

276 reinforces the PJ pattern via a tropospheric Kelvin wave.

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

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

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

280 orce eastward-propagating oceanic equatorial Kelvin waves that extend downward to 1500 meters.

281 At low temperature (8.7 kelvin), we report an optically tunable delay of 50 nano

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 rved rapid heating to temperatures of 25,000 kelvin when the scattering spectra show the collective p

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 t temperatures in the range (2.5-12) x 10(5) kelvin, which is 25-120 times hotter than the overlying

290 ness over a temperature range from 30 to 150 kelvin, which is consistent with a coherent phonon heat

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

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

293 3 gigapascals and at temperatures up to 1700 kelvin with nuclear inelastic x-ray scattering in a lase

294 been measured up to 95 gigapascals and 2000 kelvin with x-ray emission in a laser-heated diamond cel

295 - 2.1 electron volts at a temperature of 5.5 kelvin, with a corresponding electron carrier density of

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

297 e coherence lengths beyond 1 micrometer at 4 kelvin, with mobilities exceeding 2.5 square meters per

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

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