ライフサイエンスコーパス: luminosity

1 ing systematically with stellar rotation and 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 ic nucleus it harbours, to its high infrared luminosity.

6 , which is sufficient to supply the observed luminosity.

7 surface as temperatures increase with solar luminosity.

8 alogous to some Galactic black holes at peak luminosity.

9 fs are more massive than expected from their luminosity.

10 increased redness, yellowness and decreased luminosity.

11 ing star formation as it approaches its peak luminosity.

12 aters that have repetitive flares of similar luminosities.

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

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

15 They are also distinguished by lower luminosities.

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

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

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

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

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

21 Although the luminosities and brightness fluctuations of quasars in t

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

76 o be inactive or showed intermittent channel luminosity enhancements.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

99 0-UCD1's stellar mass is consistent with its luminosity, implying a large population of previously un

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

155 The luminosity of the progenitor system (especially the comp

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

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

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

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

160 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

161 Solar luminosity on the early Earth was significantly lower th

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

205 Luminosity was negatively correlated with individual det

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

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

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

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

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