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outer planets
According to estimates in [1], the heat shield mass for entry of a probe into the atmospheres of the outer planets can make up 20-50% of its total mass; here the radiative component predominates in the aerodynamic heating.
      
The main classes of stable stellar-planetary systems resulting from the dynamical evolution of groups are identified (the outer planets around binary stars and "star + planet" binary systems), and their main characteristics analyzed.
      
Solar-system objects which appear to be partly or wholly made of CCMM are the satellites of Mars, most asteroids, interplanetary dust, and, perhaps, comets, satellites of the outer planets and the rings of Uranus.
      
Nuclear fission reactors as energy sources for the giant outer planets
      
Interaction of the solar wind with the outer planets
      
One of the outstanding problems in planetary cosmogony is to account for the depletion of hydrogen in the outer planets, Neptune and Uranus.
      
Meridian observations of outer planets at Bordeaux observatory
      
A systematic bias in right ascensions in the DE200 ephemeris for the outer planets is confirmed.
      
A fraction of the constituent iron needles will be expected to be carried along with expanding gas to the periphery of the solar nebula where the outer planets and comets condensed.
      
Studies of element abundances and values of D/H in the atmospheres of the outer planets and Titan support a two-step model for the formation of these bodies.
      
The extrema of the roots of the zeroth-order Bessel function predict the ratios of the measured planetary velocities almost without error for the outer planets.
      
The solution makes exact predictions for the outer planets where the Titius-Bode series fails completely.
      
Methane spectral features in the visible to near-IR region are prominent in the spectra of the outer planets but laboratory data for the appropriate methane conditions are required to interpret the observational data.
      
On the perturbations of the five outer planets by the four inner ones
      
A determination of the masses of the five outer planets
      
Planetary masses are determined from an extensive analysis of observations of the five outer planets and of seven selected minor planets.
      
The limitations on determining the masses of the outer planets from their mutual perturbations are investigated based on the magnitudes of the periodic perturbations given in general theories and the accuracy of the observational data.
      
Future space missions to the outer planets may depend upon the use of low-thrust propulsion systems.
      
Analytical stability conditions are established for satellites, for inner planets and for outer planets, allowing arbitrary values for the mass-ratio of the binary.
      
The outer planets of the solar system are found stable and the possible existence of other than the presently known planets between Jupiter and Pluto are indicated.
      
 

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