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They are known to be heated to high (~106-109 K) temperatures and to cool down through the Comptonization of intrinsic thermal radiation.
      
The formation of radio brightening bands near cool filaments on the Sun
      
We analyze the spatial distribution of the intensity of radio emission from a cool filament in terms of the generalized Kippenhahn-Schluter model.
      
The total luminosity of the hot component is much lower than that of the cool component, but the hot-gas radiation dominates at λ>amp;lt;1800 ?.
      
The clouds cool down, radiating in the lines of this ion, to temperatures at which Balmer line emission begins.
      
At minimum brightness, the hot component's luminosity fluctuates about that of its cool companion (Lh, bol/Lc, bol≈0.9), and its temperature is Th≈(9-11)×104 K.
      
The "activation" of the cool sources in 1986-1989 nearly coincided with the disappearance of radiation from the hot source.
      
The spectral type of the cool star varied between M5III and M7III.
      
The luminosity of the cool giant varied from (6300-9100)L⊙; its radius varied by approximately 30%.
      
The ratio of the luminosities of the dust envelope and the cool giant varied from 0.08 to 0.5; i.e., up to 50% of the cool star's radiation could be absorbed in the envelope.
      
The mass-loss rate of the cool star increased in 1979-1989, reaching ~3.5×10-6 ~3.5×10-6M⊙/yr in 1988.
      
Subsequently (up to the summer of 1999), the envelope itself began to lose mass at a rate exceeding that of the cool star.
      
Spectral features of RZ Psc, a cool star with Algol-like brightness minima
      
The evolution of stars with mass 5M⊙ with an initially cool neutron core (Thorne-Zytkow objects) is computed numerically, taking into account the heating of the neutron star by flows of heat released during the accretion of a surrounding envelope.
      
Models for its stationary, spherically symmetrical, extended dust envelope are computed for two cases of heating: by the radiation of the cool component only and by the combined radiation from both components.
      
Models for highly flattened, rapidly rotating cool stars in a Newtonian approximation
      
A numerical study of the gas dynamics of the flows in the symbiotic star Z And shows that even small variations in the velocity of the wind from the cool giant can abruptly change the flow structure near the hot component.
      
The formation of dust in the cool part of the extended disk and its subsequent collisional coalescence ultimately results in the formation of solar-type planetary systems.
      
Morphology of the interaction between the stream and cool accretion disk in a semidetached binary system
      
The magnetized regions coincide with cool photospheric spots detected in photoelectric observations.
      
 

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