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The climate changed from moderate-dry to cool-wet, and then to warm-wet in turn, and the lake level rose accordingly, showing the characteristic of a high lake level.
      
Investigation of the Effect of Electric Field on the Characteristics of Heat Transfer in a Combustion Chamber with a Porous Cool
      
A device is described that allows one to cool the sensitive element of a vacuum photoemissive device to the liquid-nitrogen temperature, thus improving the device resolution.
      
To cool it below room temperature, the unit uses thermoelectric converters based on the Peltier effect.
      
The refrigerators are designed to cool photodetectors or samples in experiments that do not require a high refrigerating capacity.
      
Pd complexes of (RR)- and (SS)-1,5-methylbenzyl-3,7-diphenyl-1,5-diaza-3,7-diphosphacyclooctane as catalysts in alternating cool
      
Temperature-Dependent Physiology of Poa secunda, a Cool Season Grass Native to the Great Basin, United States
      
Expressions are derived for the energy release during accretion onto a cool (with constant entropy), rapidly rotating neutron star (NS) in the Newtonian theory and in general relativity.
      
Absorption features in the profiles of "cool" and "normal" Na I lines have been found to be enhanced compared to the LTE approximation.
      
Parameters of the cool stars themselves and the dust envelopes are estimated.
      
Their distances are 2.8±0.6 and 1.8±0.4 kpc, respectively; the luminosities and radii of their cool components (Miras) are 8.6×103L⊙, 1×104L⊙, 500R⊙, and 540R⊙.
      
To explain this shape of the V light curve, which is only slightly affected by nebular emission, it should be assumed that the cool component of YY Her fills much of its Roche lobe and has a hot spot on the hemisphere facing the hot component.
      
The 3.5-and 5-μm radiation from the eclipsing binary ε Aur outside the eclipse exhibits excess (relative to the light from an F supergiant) fluxes which correspond to the emission from a cool source with a temperature of ~1000 K.
      
Relativistic gravitational collapse of a cool white dwarf with allowance for the neutronization kinetics
      
We consider and numerically solve the problem of the relativistic gravitational collapse of a spherically symmetric cool nonrotating white dwarf with allowance for the neutronization kinetics.
      
The spectral types of the hot and cool stars are B5 V and G2 III, respectively.
      
The cool component exhibits an ultraviolet excess of .
      
The new oscillator strengths were tested by analyzing the Eu abundance using Eu II and Eu III lines in the spectra of hot peculiar stars (α2 CVn is a typical representative) and cool peculiar stars (β CrB is a typical representative).
      
Using the new Eu III oscillator strengths to analyze the spectrum of the cool Ap star β CrB, we found a significant deviation of the n(Eu II)/n(Eu III) ratio from its equilibrium value.
      
The unusual spectrum at the premaximum stage originated in the expanding photosphere of a cool K-type giant.
      
 

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