Примеры использования Radial velocity на Английском языке и их переводы на Русский язык
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The discovery was made by measuring the star's radial velocity.
Measurement of the amplitude and radial velocity of objects observed on the screen;
The radial velocity of the star likewise varies by 39 km/s during each pulsation cycle.
The planet was discovered using the radial velocity method on March 20, 2009.
Positive radial velocity means the star is receding from the Sun.
The component of movement that is in the direction of the observer is called the radial velocity.
This'wobble' can be observed if the radial velocity of the star is sufficiently high.
This data was used to derive HAT-P-33's radial velocity.
In the past, radial velocity variations have been reported, but this remains unconfirmed.
An especially simple and inexpensive method for measuring radial velocity is"externally dispersed interferometry.
The radial velocity of Vega is the component of this star's motion along the line-of-sight to the Earth.
The orbital period P o r b{\displaystyle P_{\mathrm{orb}}}is found from the periodicity in the radial velocity curve.
The planet was detected by the radial velocity method, using the HIRES spectrometer at Keck Observatory.
Kepler 18-b, c, and d: A System Of Three Planets Confirmed by Transit Timing Variations, Lightcurve Validation,Spitzer Photometry and Radial Velocity Measurements.
He was measuring the stars' radial velocity, the distance in parsecs, And the cartesian coordinates.
The radial velocity can be deduced from the displacement in the parent star's spectral lines due to the Doppler effect.
Analysis of the resulting data found that the radial velocity variations most likely indicated the existence of a planet.
The radial velocity variations of the pulsar follow from the varying intervals between the arrival times of the pulses.
It became apparent to the investigating science team that radial velocity data alone could not prove the existence of HAT-P-33b.
The radial velocity of this cluster is unusually high at 490 km/s, larger than any other cluster known.
The orbit was determined in 1921 by Clifford Crump using 69 radial velocity measurements obtained at Yerkes Observatory.
Precise radial velocity measurements have shown variations in the stellar radial velocities and spectral line profiles.
The plan involved measuring the apparent magnitude,spectral type, radial velocity, and proper motion of stars in 206 zones.
The amplitude of the radial velocity signal is inconsistent with stellar variations on stars with 55 Cancri A's low level of chromospheric activity.
However, velocity variations down to 3 m/s or even somewhat less can be detected with modern spectrometers,such as the HARPS(High Accuracy Radial Velocity Planet Searcher) spectrometer at the ESO 3.6 meter telescope in La Silla Observatory, Chile, or the HIRES spectrometer at the Keck telescopes.
The amplitude of the radial velocity oscillations means that the planet has a mass at least 5.7 times that of Jupiter in the Solar System.
The brighter member of this pair shows photometric and radial velocity periodicities with a cycle time of 0.7 days, which may indicate its rotation period.
The radial velocity of the star and changes in its position over time(proper motion) can be used to measure its velocity relative to the Sun.
Although a periodicity of 73.26 days has been observed in the star's radial velocity, it seems likely to be bound more to stellar activity than to a planetary object in close orbit.
However, the radial velocity method only yields a minimum value on the planet's mass, depending on the orbital inclination to our line-of-sight.