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3.6 ks: The length of one hour (h), the time for the minute hand of a clock to cycle once around the face, approximately 1/24 of one mean solar day 7.2 ks (2 h): The typical length of feature films 35.73 ks: the rotational period of planet Jupiter, fastest planet to rotate 38.0196 ks: rotational period of Saturn, second shortest rotational period
2.68 microseconds – the amount of time subtracted from the Earth's day as a result of the 2004 Indian Ocean earthquake. [2] 3.33564095 microseconds – the time taken by light to travel one kilometre in a vacuum. 5.4 microseconds – the time taken by light to travel one mile in a vacuum (or radio waves point-to-point in a near vacuum).
After 6 months on the International Space Station (ISS), orbiting Earth at a speed of about 7,700 m/s, an astronaut would have aged about 0.005 seconds less than he would have on Earth. [11] The cosmonauts Sergei Krikalev and Sergey Avdeev both experienced time dilation of about 20 milliseconds compared to time that passed on Earth. [12] [13]
Once every one million years 10 −12: 1 picohertz (pHz) 1.23 pHz Precession of the Earth's axis (about every 25,700 years) 10 −11: 10 pHz ~31.71 pHz: Once per millennium 10 −10: 100 pHz ~317.1 pHz: Once per century 10 −9: 1 nanohertz (nHz) ~1 nHz: Once per generation (about every 30 years) ~2.9 nHz: Average solar cycle (about every 11 ...
The amount of time light takes to travel one Planck length. quectosecond: 10 −30 s: One nonillionth of a second. rontosecond: 10 −27 s: One octillionth of a second. yoctosecond: 10 −24 s: One septillionth of a second. jiffy (physics) 3 × 10 −24 s: The amount of time light takes to travel one fermi (about the size of a nucleon) in a ...
A millisecond (from milli-and second; symbol: ms) is a unit of time in the International System of Units equal to one thousandth (0.001 or 10 −3 or 1 / 1000) of a second [1] [2] or 1000 microseconds. A millisecond is to one second, as one second is to approximately 16.67 minutes.
A sidereal rotation is the time it takes the Earth to make one revolution with rotation to the stars, approximately 23 hours 56 minutes 4 seconds. A mean solar day is about 3 minutes 56 seconds longer than a mean sidereal day, or 1 ⁄ 366 more than a mean sidereal day.
To show that, one can apply Noether's theorem to a body that freely falls into the well from infinity. Then the time invariance of the metric implies conservation of the quantity g ( v , d t ) = v 0 / T 2 {\displaystyle g(v,dt)=v^{0}/T^{2}} , where v 0 {\displaystyle v^{0}} is the time component of the 4-velocity v {\displaystyle v} of the body.