Примеры использования The orbital period на Английском языке и их переводы на Русский язык
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The orbital period is approximately 44 years.
One periodicity is related to the orbital period of the binary star system.
The orbital period of this binary is about 101.5 years.
The orbital period of Moon(a lunar"year") is approximately 27,322 days.
It was observed also a periodicity of 1.32 hours,which is attributed to the orbital period of the system.
The orbital period of the pair is greater than 5000 years.
For all ellipses with a given semi-major axis the orbital period is the same, regardless of eccentricity.
The orbital period is slowly changing due to mass exchange between the stars.
This means that the time required to execute each phase of the transfer is half the orbital period of each transfer ellipse.
The orbital period was originally estimated at 83 days and has now been revised to 66 days.
This brightness variation has a larger amplitude than the variation with the orbital period and is known as the superhump.
Deiss measured the orbital period of Mercury around the axis, receiving the result of 58.65 days.
The orbital period of the external electron is twice more that the orbital period of the internal electron.
It can be calculated from observable quantities only, namely the orbital period of the binary system, and the peak radial velocity of the observed star.
The orbital period P o r b{\displaystyle P_{\mathrm{orb}}} is found fromthe periodicity in the radial velocity curve.
In that case, the tidal bulge stays directly under the moon,there is no transfer of angular momentum, and the orbital period will not change.
In the case of 38 Virginis b, the orbital period would have to be no greater than 80 days(a little over 2 months) in order to have a stable orbit.
Since the satellite is in geostationary orbit, the concept of a"nodalperiod" is not applicable. However, the orbital period is approximately 86,166 seconds.
The orbital period of J0737-3039(2.4 hours) is the shortest yet known for such an object(one-third that of the Taylor-Hulse object).
Stars in the high state, either permanently or during an outburst,often show brightness variations with a fairly consistent period different from the orbital period.
These data show that the orbital period of the two stars is steadily decreasing at a rate of 1.2 milliseconds per year as they thus are getting closer by approximately 60 centimetres(2.0 ft) per day.
Radiotelescopic observations revealedIo's influence on the Jovian magnetosphere, as demonstrated by decametric wavelength bursts tied to the orbital period of Io.
It relates the orbital period(the time it takes to complete one full orbit) with the distance between the two bodies(the orbital separation), and the sum of their masses.
No orbital velocity shifts have been detected,so the orbital separation is probably large(several AU) and the orbital period is years or decades.
The orbital period of J1407b is estimated to be around a decade(3.5 to 13.8 years), and its most probable mass is approximately 13 to 26 Jupiter masses, but with considerable uncertainty.
A secondary period of 7003105100000000000♠1,051 seconds(17m 31s)is believed to be caused by a superhump-an elevated outburst in the signal that occurs with a period slightly longer than the orbital period.
When the orbital period has shrunk to about 5 minutes,the less-massive(and the larger) of the two white dwarfs will fill its Roche lobe and start mass transfer to its companion.
If the object is directly between Earth and the Sun, then Earth's gravity counteracts some of the Sun's pull on the object, andtherefore increases the orbital period of the object.