ライフサイエンスコーパス: luminosity

1 ing star formation as it approaches its peak luminosity.

2 f Jupiter, and constrains the planet's tidal luminosity.

3 es resulted in a TBR of 1.14 (P>.5) based on luminosity.

4 face temperatures during a time of low solar luminosity.

5 ing systematically with stellar rotation and luminosity.

6 ic nucleus it harbours, to its high infrared luminosity.

7 , which is sufficient to supply the observed luminosity.

8 high species diversity and low turbidity and luminosity.

9 increased redness, yellowness and decreased luminosity.

10 surface as temperatures increase with solar luminosity.

11 alogous to some Galactic black holes at peak luminosity.

12 fs are more massive than expected from their luminosity.

13 nctionally adjusted to various environmental luminosities.

14 aters that have repetitive flares of similar luminosities.

15 found with other z > 6.1 quasars with lower luminosities.

16 etween their light-curve widths, colors, and luminosities.

17 They are also distinguished by lower luminosities.

18 spectroscopic confirmation of this very low luminosity (~0.05 L*) galaxy at z = 9.79, observed 480 M

19 it evolves in energy (~12 to ~6 MeV) and in luminosity (~1.1 to <0.43 x 10(50) erg second(-1)) but h

20 seconds long), hard-X-ray bursts, with peak luminosities(1) of 10(36) to 10(43) erg per second.

21 expected to enter an unstable phase at high luminosity(1).

22 dwarfs each with a lower mass and intrinsic luminosity(1,4).

23 ard states', when a hot corona dominates the luminosity(3).

24 afterglow produced by this outburst, with a luminosity 500 times larger than the only other detectio

25 It has an optical and near-infrared luminosity a few times greater than those of previously

26 when plotted as a function of observed 5-GHz luminosity; a combination of source counts and the appar

27 Blue compact dwarf (BCD) galaxies are low-luminosity (absolute K-band magnitude, M(K) > -21 mag)(1

28 ent width and ratio of PAH to total infrared luminosity across the galaxy.

29 Low-luminosity active galactic nuclei have hot accretion flo

30 odic outflows (QPOuts) from a previously low-luminosity active galactic nucleus after an outburst, li

31 e source appears to be co-located with a low-luminosity active galactic nucleus or a previously unkno

32 in typical quiescent galaxies that host low-luminosity active nuclei.

33 At some additive doses, luminosity analysis demonstrated an incremental fluoresc

34 Although the luminosities and brightness fluctuations of quasars in t

35 ay-absorbed active galactic nuclei that have luminosities and redshifts characteristic of the sources

36 Analysis of the luminosities and spectra of accreting black holes has yi

37 The two galaxies exhibit lower infrared luminosities and star-formation rates than extreme starb

38 ive than theoretical predictions given their luminosities and the ages of their host stars(1-3).

39 Hence we propose that increasing solar luminosity and a decrease in seafloor spreading rate ove

40 Blanching and boiling caused a decrease in luminosity and a loss of green coloration in both variet

41 jecta of low kinetic energy, a faint optical luminosity and a small mass fraction of radioactive nick

42 However, the luminosity and brilliance demands of high-energy physics

43 A blue object, having luminosity and colours consistent with those of some WRS

44 of soaking presented higher head rice yield, luminosity and hardness, with decreases in cooking time,

45 tichoke, tomato, lemon powders in FB reduced luminosity and hardness.

46 This combination of high luminosity and low metal-line opacity cannot be reconcil

47 circle) and M(middle dot in circle) are the luminosity and mass of the Sun).

48 reliable information on gas column density, luminosity and mass, has left the main physical mechanis

49 The low luminosity and redshift of GRB 190829A reduce both inter

50 ent fingerprint visualization owing to their luminosity and resistance to photobleaching.

51 axy orbital motions and the relation between luminosity and rotation in galaxies, although not in clu

52 e psychophysiological responses modulated by luminosity and sleep.

53 chlorine-free pyrotechnic illuminant of high luminosity and spectral purity was investigated.

54 were discovered, each of whose extreme X-ray luminosity and synchrotron radio emission were interpret

55 he observed high-energy properties and radio luminosity and the inferred rate of such events.

56 relation between the persistent radio source luminosity and the rotation measure itself(7,9).

57 d power-law behavior is observed between the luminosity and the spectral peak energy that is inconsis

58 tween predictable fluctuations in night-time luminosity and the underlying risk-resource landscape sh

59 When combined with the high luminosity and unusual outburst behaviour, these charact

60 s estimate stellar masses by determining the luminosity and using the 'mass-luminosity' relationship,

61 solar masses) because of its extremely high luminosity and variability characteristics, although som

62 that repeating FRBs may have a wide range of luminosities, and originate from diverse host galaxies a

63 y that robustly establishes absolute fluxes, luminosities, and temperatures.

64 n in structure (crystallinity), composition, luminosity, and chromaticity were investigated revealing

65 verting protocols (average, weighted average/luminosity, and software specific) have been compared in

66 Wind accretion explains the X-ray luminosity, and the black-hole spin can be natal.

67 physical properties-radius, temperature and luminosity-and how those properties evolve with time.

68 Its exceptionally low optical luminosity (approximately 10(35) erg s(-1)) and radiated

69 of variable (pulsating) stars whose absolute luminosities are related in a simple manner to their pul

70 and its quiescent activity levels and X-ray luminosity are comparable to those of the Sun.

71 t that jet magnetic field and accretion disk luminosity are tightly correlated over seven orders of m

72 Variations in the Sun's total energy output (luminosity) are caused by changing dark (sunspot) and br

73 lar masses that is undergoing an outburst in luminosity arising from a temporary increase in the accr

74 Periodic increases in luminosity arising from variable accretion rates have be

75 or the pulsar in supernova 1987a is the same luminosity as the Crab pulsar has today 936 years after

76 to determine the Earth's total antineutrino luminosity at .

77 climate models to compensate for lower solar luminosity at 2.75 Gyr.

78 is shown that the molecular gas mass per CO luminosity at extremely low metallicity is approximately

79 We compare output and luminosity at the country level and at the 1 degrees lat

80 y more compact than galaxies with equivalent luminosity at z ~ 6 to 8, leading to a high star formati

81 ated supernovae, they overestimate the X-ray luminosity because the density of the core gas is too hi

82 ep regime that leads to the red-giant-branch luminosity bump.

83 een able to form galaxies with the requisite luminosities, but have otherwise been unable to simultan

84 erms of an extreme wind driven by the star's luminosity, but the fast material reported here indicate

85 greatly advanced our understanding of solar luminosity change, and this new understanding indicates

86 After day 600, the infrared luminosity closely followed the intrinsic luminosity exp

87 The progenitor system's luminosity, colours, environment and similarity to the p

88 rrelated and highly variable X-ray and radio luminosities, combined with other observational properti

89 retained its atmosphere despite the greater luminosity (compared to the present-day) of its host sta

90 E sources show long-term decays in quiescent luminosity consistent with TDEs(4,12) and two observed T

91 of years are controlled by changes in solar luminosity, continent distribution, and atmosphere compo

92 vidence that biofluorescence creates greater luminosity contrast with the surrounding background, hig

93 ant to large amplitude changes in background luminosity, contrast, and body temperature.

94 Unlike its low-redshift and low-luminosity counterparts, SDSS J0749 + 2255 is hosted by

95 w surface gravity and a detectable long-term luminosity decay, which is uncharacteristic for its evol

96 We find that the luminosity densities of these star-forming regions are c

97 roximately 10, as galaxies increased in both luminosity density and volume density from z approximate

98 tuation measurements to find the ultraviolet luminosity density of galaxies at redshifts greater than

99 ance of quasar host galaxies, as well as the luminosity density provided by the quasars, has therefor

100 Their maximum (Eddington) luminosity depends on the mass of the black hole, and th

101 certain history of this star and the extreme luminosity difference between the components make it dif

102 ately 300 K ( approximately 10 per cent) and luminosities differing by approximately 50 per cent, bot

103 on between the spectral peak energy and peak luminosity discovered in observations.

104 ational wave cosmology appeals to the direct luminosity distance estimation through the waveform sign

105 ncy methods; and (3) detailed information on luminosity distance, inclination and masses, which can b

106 A patch or arc segment of enhanced luminosity, distinctly brighter than the diffuse backgro

107 The kilonova of GRB 211211A has a similar luminosity, duration and colour to that which accompanie

108 s and could be basis for future compact high-luminosity electron-positron colliders.

109 ics of the outer parts of three intermediate-luminosity elliptical galaxies were studied with the Pla

110 with AGN and GRBs lying at the low- and high-luminosity ends, respectively, of the correlation.

111 o be inactive or showed intermittent channel luminosity enhancements.

112 The correction to redshift vs. luminosity entails an adjustable free parameter that int

113 d Muc5AC (mucin 5AC) (Delta + 263.2 +/- 92.7 luminosity/epithelial area) and decreased ciliated cells

114 ease in residual carbon leads to decrease in luminosity even with increase in hue.

115 tandard accretion models fail to explain its luminosity, even assuming beamed emission, but a strong

116 ty of the hypothesis of (redshift-dependent) luminosity evolution in galaxies is tested by statistica

117 In this case there must be significant luminosity evolution in these objects, but little veloci

118 bright cluster galaxy samples, and proposed luminosity evolution, are briefly considered.

119 he nuclei of nearby galaxies and whose X-ray luminosities exceed the theoretical maximum for spherica

120 source in the nearby galaxy M 31, whose peak luminosity exceeded 10(39) erg s(-1).

121 e nucleus of the host galaxy with bolometric luminosities exceeding 10(39) erg s(-1).

122 ed luminosity closely followed the intrinsic luminosity expected for thermalized 56Co gamma rays, dem

123 a type II-plateau supernova of extremely low luminosity, exploding in a lenticular galaxy with residu

124 ration GRBs, while its temporal lag and peak luminosity fall entirely within the short-duration GRB s

125 Faraday rotation measure, the expected radio luminosity falls below the limit-of-detection threshold

126 large-scale magnetospheres that can scale to luminosities far greater than those observed in our Sola

127 accretion disk, and a collimated core, with luminosity fluctuations propagating upwards from its bas

128 affect the absorption and emission spectra, luminosity, fluorescence lifetimes, and two-photon absor

129 f freezing white dwarfs maintains a constant luminosity for a duration comparable with the age of the

130 dings suggest that other extreme ULXs (x-ray luminosity [Formula: see text] 10(41) erg second[Formula

131 We found that the annihilation luminosity from kinematically cold substructure could be

132 the rate of these events with similar radio luminosity from M dwarfs is 0.84-0.69+1.94 x 10-3 per da

133 est that current glare models using photopic luminosity function as a spectral weighting are not effe

134 presentative of the bright end of the [C ii] luminosity function, then they can account for the popul

135 ic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-o

136 a short gamma-ray burst seen off-axis, a low-luminosity gamma-ray burst at high redshift, or a tidal

137 We find that luminosity has informational value for countries with lo

138 re than 10(44) ergs per second at their peak luminosity have recently been discovered in faint galaxi

139 For this age and luminosity, "hot-start" formation models indicate a mass

140 among these species against the rising solar luminosity, i.e. the Gaia hypothesis.

141 These extreme luminosities-if the emission is isotropic and below the

142 The observed gamma-ray luminosity implies an upper limit of 60 millisecond puls

143 0-UCD1's stellar mass is consistent with its luminosity, implying a large population of previously un

144 s, point sources in galaxies, and have X-ray luminosities in excess of 3 x 10(39) ergs per second.

145 Their X-ray luminosities in the 0.5-10 kiloelectronvolt energy band

146 Some of the sources observed to have high luminosities in the far infrared could be obscured QSOs

147 f 0.07 to 0.2 per cent relative to the total luminosity in dark-matter haloes of 10(9) to 10(12) sola

148 face temperatures in the face of lower solar luminosity in early Earth history.

149 th a variable source that can reach an X-ray luminosity in the 0.3-10 kiloelectronvolt range of 1.8 x

150 he pulsed flux alone corresponds to an X-ray luminosity in the 3-30 kiloelectronvolt range of 4.9 x 1

151 urces that produce the bulk of the accretion luminosity in the universe.

152 e first AXP with transient emission when its luminosity increased 100-fold from the quiescent level;

153 During these bursts, the optical/ultraviolet luminosity increases by a factor of more than three in l

154 When solar luminosity increases to a critical value, a desert forms

155 cally alters night-time visibility, with low luminosity increasing hunting success of African lions.

156 The HCN line luminosity indicates the presence of 10 billion solar ma

157 The radio luminosity is extremely high and shows variability on a

158 We conclude that most of the luminosity is generated through the accretion process, w

159 m ordinary radio pulsars in that their X-ray luminosity is orders of magnitude greater than their rat

160 ized 56Co gamma rays, demonstrating that the luminosity is powered by radioactivity and that the dust

161 During the quasar phase, a huge luminosity is released as matter falls onto the black ho

162 accompanied by a prodigious increase in its luminosity, is causing the vaporization of a collection

163 Galaxies brighter than the characteristic luminosity L* (refs. (1,2)) do not provide enough ionizi

164 e spectrum together with the high bolometric luminosity (L(bol) = (1.1 +/- 0.3) x 10(45) erg s(-1)) i

165 s one main light-curve peak, or a plateau in luminosity, lasting approximately 100 days before declin

166 ude of Mu ,AB = -23.5 +/- 0.1 and bolometric luminosity Lbol = (2.2 +/- 0.2) x 10(45) ergs s(-1), whi

167 is unique in that it exceeded the Eddington luminosity limit for ten years.

168 Luminosity-line width and Dn-sigma methods are less accu

169 we show that a negative feedback among solar luminosity, liquid water and carbonate formation can exp

170 Instead, the high peak luminosities, long flare timescales, and immense radiate

171 xpanding the predicted relation into the low luminosity-low Faraday rotation measure regime (<1,000 r

172 nd ROSAT revealed a larger population of low-luminosity (< 10(33) ergs(-1)) x-ray sources.

173 The powering of the High Luminosity magnets of the Large Hadron Collider relies o

174 ssive stars are very rare, but their extreme luminosities make them both the only type of young star

175 way that is correlated with their intrinsic luminosity, making them useful as 'standard candles' for

176 A)) that is very quiescent at present with a luminosity many orders of magnitude below those of activ

177 standard sources, the present study examines luminosity (measures of nighttime lights visible from sp

178 Therefore, solar luminosity models suggest that, in the atmosphere of the

179 r 1 has long been suspected to be the quasar luminosity normalized by the mass of the hole (the 'Eddi

180 eling of the spectra and photometry yields a luminosity (normalized by the luminosity of the Sun) of

181 r substructure of seven to eleven large, low-luminosity objects.

182 porate multiple parameters (e.g., landcover, luminosity, observer effect) influencing lion abundance

183 c giant flares from galactic magnetars (peak luminosities of 10(44)-10(47) ergs per second, lasting a

184 ter Aperture Spherical radio Telescope, with luminosities of about eight decades fainter than FRB 202

185 h magnetic fields up to around 10(15) gauss, luminosities of approximately 10(31)-10(36) ergs per sec

186 This brings the core entropy and X-ray luminosities of clusters into agreement with the observa

187 death of massive stars, the electromagnetic luminosities of GRBs and XRFs exceed those of ordinary t

188 t of ultraluminous X-ray sources (those with luminosities of less than 10(40) erg s(-1); ref.

189 t of ultraluminous X-ray sources (those with luminosities of less than 10(40) erg s(-1); ref. 1) are

190 They have luminosities of more than 3 x 10(39) ergs per second, un

191 ce was at the distance of NGC 4697, then the luminosities of the flares were greater than 10(39) erg

192 The luminosities of type Ia supernovae (SNe), the thermonucl

193 X-ray sources with similar X-ray spectra and luminosities of up to a few times 10(40) ergs per second

194 Achieving peak luminosities of up to one million times that of the Sun,

195 e temperature of only around 3,050 kelvin, a luminosity of 0.15 per cent of that of the Sun, a measur

196 per cent of the emission, with a quasar-like luminosity of 1.5 x 10(46) ergs per second.

197 t observed around black holes above an X-ray luminosity of 10(44) ergs per second.

198 peak amplitude corresponding to an isotropic luminosity of 2.4 _ 1040 erg s-1 in M82 and a period of

199 This quasar has a bolometric luminosity of 4 x 10(13) times the luminosity of the Sun

200 ULAS J1120+0641 has a luminosity of 6.3 x 10(13)L(middle dot in circle) and ho

201 One source flared once to a peak luminosity of 9 x 10(40) erg per second; the other flare

202 It has an isotropic peak luminosity of [Formula: see text]1000 times the Eddingto

203 upper limit to the soft intrinsic bolometric luminosity of a pulsar central engine.

204 Here we report that the infrared luminosity of a young protostar (of age about 10(5) year

205 hour-scale periodic X-ray transients with a luminosity of about 10(33) erg s(-1) linked to exception

206 This association implies a luminosity of about 100 times the Eddington limit for a

207 This object has an X-ray luminosity of about 4 x 10(39) erg s(-1), which rules ou

208 tely 4 x 10(5) solar masses) with peak X-ray luminosity of about 5 x 10(42) erg per second.

209 Our finding explains the high luminosity of GN-z11 and can also provide an explanation

210 has been invoked to explain both the excess luminosity of Saturn(1,3), and the depletion of He and n

211 e implies that some 200 years ago, the X-ray luminosity of Sgr A(*) was briefly comparable to that of

212 ity relations overestimate the near-infrared luminosity of such objects by about a factor of approxim

213 the greenhouse gas that countered the lower luminosity of the early Sun.

214 However, the observed x-ray luminosity of the gas is typically less than a few perce

215 The degree of luminosity of the grain, however, was able to better pre

216 and the stellar velocity dispersion or bulge luminosity of the host galaxy.

217 The luminosity of the progenitor system (especially the comp

218 olometric luminosity of 4 x 10(13) times the luminosity of the Sun and a black-hole mass of 8 x 10(8)

219 and Whitfield suggested in 1982 that, as the luminosity of the Sun increases over its life cycle, bio

220 metry yields a luminosity (normalized by the luminosity of the Sun) of 1.6 to 4.0 x 10(-6) and an eff

221 o 23 kelvin at a rate of about 220 times the luminosity of the Sun.

222 iable X-ray source with a maximum 0.2-10 keV luminosity of up to 1.1 x 10(42) erg s(-1) in the edge-o

223 of the two ice giants manifested by the low luminosity of Uranus, and lead to a better understanding

224 Solar luminosity on the early Earth was significantly lower th

225 lanets on their observable features, such as luminosity or magnetic field, crucially depends on the p

226 echanism transports the heat flux of a solar luminosity outwards?

227 The increase in solar luminosity over geological timescales should warm the Ea

228 i et al. on 7 January 2006 that had very low luminosity (peak absolute R-band magnitude M(R) of about

229 ion, consistent with relatively massive, low-luminosity primeval galaxies at redshifts greater than 2

230 greenhouse gas during periods of lower solar luminosity, probably dominating over methane after the a

231 ut equally (per logarithmic interval) to the luminosity produced by dark matter annihilation, which w

232 In our model, increasing solar luminosity promoted the stability of liquid water, which

233 be described by accretion disk emission with luminosity proportional to the fourth power of the disk

234 Patterns of ionospheric luminosity provide a unique window into our complex, cou

235 Low-luminosity quasars(4-6) from the Hyper Suprime-Cam Subar

236 h stars in the cluster, or why the blue hook luminosity range in this massive cluster cannot be repro

237 ting from evolution is required to solve the luminosity range problem.

238 (1) The extension of habitability to a wider luminosity range, (2) resistance to the impact of "cheat

239 ree known satellite galaxies that shine with luminosities ranging from about a thousand to a billion

240 The high mass-to-luminosity ratio of the hidden object was originally exp

241 ax,c) ~ 1791 to 1857 K) and the highest soot luminosity region temperature (T*(c) ~ 1600 to 1650K).

242 ritical factor in determining both the width-luminosity relation and the observed scatter about it.

243 der quadratic correction to the redshift vs. luminosity relation for an observer at the center.

244 The slope and normalization of the width-luminosity relation has a weak dependence on certain pro

245 Calibration of the period-luminosity relation is a necessary first step, but the s

246 inuity) that corrections to the redshift vs. luminosity relation observed after the radiation phase o

247 ll allow us to calibrate directly the period-luminosity relation to better than a few per cent.

248 an reproduce this general trend in the width-luminosity relation; but the processes of ignition and d

249 nosity, we have found that the standard mass-luminosity relations overestimate the near-infrared lumi

250 alaxy with which to calibrate Cepheid period-luminosity relations, and as a result has become the bes

251 nty in the calibration of the Cepheid period-luminosity relationship(2,3) (also known as the Leavitt

252 y measuring the period and using the 'period-luminosity' relationship, astronomers can use the observ

253 termining the luminosity and using the 'mass-luminosity' relationship, but this relationship has neve

254 ion is whether their extremely high infrared luminosities result from the active galactic nucleus, fr

255 The infrared luminosity sets an upper limit to the soft intrinsic bol

256 d flaring radio emission from LP944-20, with luminosities several orders of magnitude larger than pre

257 cies richness and with greater turbidity and luminosity, showing that most bromeliad tanks presented

258 like event with two peaks (FRB 200428) and a luminosity slightly lower than the faintest extragalacti

259 However, the low-luminosity sources proved difficult to classify.

260 AT observations of 55 clusters, about 25 low-luminosity sources were found.

261 It was realized early on that the high-luminosity sources were low-mass x-ray binaries in outbu

262 tar) may distinguish typical bursts from low-luminosity, spherical events like XRF 060218.

263 , when taken together with the low gamma-ray luminosity, suggests that GRB 031203 is the first cosmic

264 , extending further in redshift and to lower luminosity than what had previously been found by submil

265 gest an extragalactic origin and imply radio luminosities that are orders of magnitude larger than th

266 pirical relation between the X-ray and radio luminosities that has been found for many types of stars

267 ined by this potential radiate X-rays with a luminosity that depends mainly on the gas density in the

268 blackbody temperature of 1,000 Kelvin and a luminosity that is 4 percent that of the star lasting fo

269 t fluxes convey the excess part of the solar luminosity that radiative diffusion cannot.

270 Although jet dynamics depend sensitively on luminosity, the correlation holds regardless.

271 it, it leaves unexplained the observed X-ray luminosity, the star's underluminosity, the black hole's

272 er-massive black hole generates vast radiant luminosities through the gravitational accretion of gas.

273 This planet also has a sufficiently low luminosity to be consistent with the "cold-start" core-a

274 some point sufficient temperature, mass, and luminosity to be detected.

275 extended post-impact remnant with sufficient luminosity to explain the infrared observations.

276 We use nighttime luminosity to represent temporal trends in coastal econo

277 rgoing an accretion burst(7), increasing its luminosity to roughly 200 L((.)) (ref.

278 gher masses imply less extreme ratios of the luminosity to the isotropic Eddington limit, theoretical

279 information, whereas H1/2 cells are probably luminosity-type cells that process luminance information

280 nged periods of darkness on the responses of luminosity-type horizontal cells (L-HCs) in the freshwat

281 s ultra-faint galaxy (M(UV) = -17.35)-with a luminosity typical of the sources responsible for cosmic

282 ains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed

283 the accumulated envelope of gas, leading to luminosities up to a million times that of the Sun and a

284 Those intended for the high-luminosity upgrade of the Large Hardon Collider (LHC) at

285 escope observations have only provided water luminosity upper limits for dust-depleted inner disks(7)

286 racers, albeit intermittently with accretion luminosity variations ranging from zero to 50 per cent f

287 The X-ray luminosity varies by a factor of seven in a few hours, w

288 lations between observable properties (e.g., luminosity, velocity dispersion, oscillation period).

289 r than any gamma-ray burst, whereas its peak luminosity was approximately 100 times higher than brigh

290 tion occurred in the distant past when solar luminosity was low, it might have been irreversible beca

291 emains a key challenge, given that the Sun's luminosity was much lower in the past.

292 Luminosity was negatively correlated with individual det

293 escence than the cysts, and the most intense luminosity was observed in the UV range.

294 First, we show that the luminosity, wavelength, and intermittency of solid-state

295 From the measured X-ray luminosity, we derive an instantaneous accretion rate of

296 Given its measured 1-2-micrometre luminosity, we have found that the standard mass-luminos

297 rement of their atmospheric compositions and luminosities, which are influenced by their formation me

298 dius of the obscuring material with incident luminosity, which arises from the sublimation of dust; b

299 The PP addition decreased expansion and luminosity; while increasing redness of the extrudates c

300 d by accelerated particles and the gamma-ray luminosity, with AGN and GRBs lying at the low- and high