Results 351 to 360 of about 2,485,700 (388)
Fluid mechanics of sarcomeres as porous media.
Soft MatterSevern J, Vacus T, Lauga E.
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The motion of catalytically active colloids approaching a surface.
Soft MatterMelio J +8 more
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Self-consistent models of Earth's mantle and core from long-period seismic and tidal constraints
Munch FD +4 more
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, 2014 In a system consisting of a star and a planet, because of the gravitational force of the planet on the star, the planet and its host star orbit their common center of mass. This causes variations in the distance of the star to the observer creating what is known as radial velocity. Measuring the velocities of stars along the line of sight dates back to
David W. Latham, Nader Haghighipour
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International Astronomical Union Colloquium, 1984
AbstractThe writer reviews the presently available lists of standard-velocity stars approved by IAU Commission 30 and suggests that the time has arrived for major revisions. Many of the currently adopted standards are known or suspected to be variable in velocity at the level of precision to which we can now work. The writer suggests that we need three
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AbstractThe writer reviews the presently available lists of standard-velocity stars approved by IAU Commission 30 and suggests that the time has arrived for major revisions. Many of the currently adopted standards are known or suspected to be variable in velocity at the level of precision to which we can now work. The writer suggests that we need three
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Radial velocities of isolated galaxies
Astrophysics, 1979For 16 galaxies in our list there are independent estimates of the radial velocities based on observations with different telescopes [2-4]. In ten cases out of the 16, the values of V 0 agree to within the errors of the measurements. The mean difference of the estimates is = --14 • 22 (km/sec). The rms difference of the estimates, < ~V~ m_oth } _/2 =
I. D. Karachentsev, V. E. Karachentseva
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The Radial Velocities of the Stars
1928The determination of radial velocities of all stars brighter than magnitude 6,0 nears completion and a large number of velocities of stars down to magnitude 8,5 are also determined. For still fainter stars the present methods of velocity determination are too time-consuming to make possible any rapid progress for these stars. The use of objective prism
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Publications of the Astronomical Society of the Pacific, 1983
A number of techniques for determining stellar radial velocities with a precision better than 100 m s-1 are now becoming available. Three types of precision velocity techniques have been proposed, using for wavelength reference either telluric lines, Fabry-Perot fringes, or lines generated in an absorption cell. The author has used the latter technique,
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A number of techniques for determining stellar radial velocities with a precision better than 100 m s-1 are now becoming available. Three types of precision velocity techniques have been proposed, using for wavelength reference either telluric lines, Fabry-Perot fringes, or lines generated in an absorption cell. The author has used the latter technique,
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RVS' RADIAL VELOCITIES ACCURACY [PDF]
EAS Publications Series, 2002 D. Katz, A. E. Gomez, D. Morin, Y. Viala
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