Sir Isaac Newton's laws of motion contain an important formula: "F" = "ma". "F" is force. "m" is mass. "a" is acceleration. An object with a mass ("m") of one kilogram will accelerate ("a") at one meter per second per second when acted upon by a force ("F") of one newton. This about one-tenth the acceleration due to earth’s gravity.
The weight of matter depends on the strength of gravity. The mass of matter does not. The mass of an object is the same everywhere. Matter has invariant mass assuming it is not traveling at a relativistic speed with respect to an observer. According to Einstein’s theory of special relativity, the relativistic mass (apparent mass with respect to an observer) of an object or particle with rest mass "m" increases with its speed as "M"=γ"m" (where γ is the Lorentz factor). This effect is vanishingly small at everyday speeds, which are by orders of magnitude less than the speed of light, but becomes noticeable at very high speeds. For example, traveling at just 10% the speed of light with respect to an observer—exceedingly fast compared to everyday speeds (about )—increases an object’s relativistic mass just over 0.5%.
As regards the kilogram, relativity’s effect upon the constancy of matter’s mass is simply an interesting scientific phenomenon that has zero effect on the definition of the kilogram and its practical realizations.</ref> Objects are "weightless" for astronauts in microgravity. However, the objects still have their mass and inertia. Astronaut must use ten times as much force to accelerate a ten-kilogram object at the same rate as a one-kilogram object.
A common swing, as shown in the picture, can show the relationship of force, mass and acceleration. Someone could push an adult on the swing. The adult would accelerate slowly. They would only swing a short distance forward before the swing would change direction. If a child is sitting on the swing, then the child would swing forward faster and further.
Second
The second (symbol: s), is a unit of time. There are around 60 seconds in a minute, 60 minutes in an hour, and 24 hours in a day. This tradition dates back to the Babylonian.
In science, a second is the time it takes for a caesium atom to vibrate 9,192,631,770 (around 9 billion) times. Scientists measure the second this way because the length of a day changes all the time. For example, when the dinosaurs lived, a day was about an hour shorter. Vibrations of atoms on the other hand always take the same time. This atomic second is also called the SI second.
Metric prefixes are frequently combined with the word "second" to denote subdivisions of the second, "e.g.", the millisecond (one thousandth of a second) and nanosecond (one billionth of a second). Though SI prefixes may also be used to form multiples of the second (such as “kilosecond”, or one thousand seconds), such units are rarely used in practice. More commonly encountered, non-SI units of time such as the minute, hour, and day increase by multiples of 60 and 24 (rather than by powers of ten as in the SI system).
One heartbeat of an adult at rest, will last about one second.
Under the International System of Units, the second is currently defined as the duration of 9,192,631,770 periods of the radiation corresponding to the transition between the two hyperfine levels of the ground state of the caesium-133 atom. This definition refers to a caesium atom at rest at a temperature of (absolute zero). The ground state is defined at zero magnetic field. The second thus defined is equivalent to the ephemeris second.
The international standard symbol for a second is s (see ISO 31-1)
1 international second is equal to:
There are 31,536,000 seconds in a common year, 31,622,400 seconds in a leap year, and 31,557,600 seconds in a Julian year
Originally, the second was known as a "second minute", meaning the second minute (i.e. small) division of an hour. The first division was known as a "prime minute" and is equivalent to the minute we know today. Third and fourth minutes were sometimes used in calculations.
The factor of 60 comes from the Babylonians who used a sexagesimal (base-60) numeral system. However, the Babylonians did not subdivide their time units sexagesimally (except for the day). The hour had been defined by the ancient Egyptians as either 1/12 of daytime or 1/12 of nighttime, hence both varied with the seasons. Greek astronomers, for example Hipparchus and Ptolemy, defined the hour as 1/24 of a mean solar day. Sexagesimally subdividing this mean solar hour made the second 1/86,400 of a mean solar day.
Greek time periods, for example the mean synodic month, were usually specified quite precisely because they were "calculated" from carefully selected eclipses separated by hundreds of years—individual "mean" synodic months and similar time periods cannot be measured. Nevertheless, with the development of pendulum clocks keeping "mean time" (as opposed to the "apparent time" displayed by sundials), the second became measurable. The seconds pendulum was proposed as a unit of length as early as 1660 by the Royal Society of London. The duration of a beat or half period (one swing, not back and forth) of a pendulum one metre in length on the Earth's surface is approximately one second.
In 1956 the second was defined in terms of the period of revolution of the Earth around the Sun for a particular epoch, because by then it had become recognized that the Earth's rotation on its own axis was not sufficiently uniform as a standard of time. The Earth's motion was described in Newcomb's Tables of the Sun, which provides a formula for the motion of the Sun at the epoch 1900 based on astronomical observations made between 1750 and 1892. The second thus defined is
This definition was ratified by the Eleventh General Conference on Weights and Measures in 1960. The "tropical year" in the definition was not measured, but calculated from a formula describing a tropical year which decreased linearly over time, hence the curious reference to a specific "instantaneous" tropical year. Because this second was the independent variable of time used in ephemerides of the Sun and Moon during most of the twentieth century (Newcomb's Tables of the Sun were used from 1900 through 1983, and Brown's Tables of the Moon were used from 1920 through 1983), it was called the ephemeris second.
When atomic clocks were made, they became the basis of the definition of the second, rather than the revolution of the Earth around the Sun.
Following several years of work, Louis Essen from the National Physical Laboratory (Teddington, England) and William Markowitz from the United States Naval Observatory (USNO) determined the relationship between the hyperfine transition frequency of the caesium atom and the ephemeris second. Using a common-view measurement method based on the received signals from radio station WWV, they determined the orbital motion of the Moon about the Earth, from which the apparent motion of the Sun could be inferred, in terms of time as measured by an atomic clock. As a result, in 1967 the Thirteenth General Conference on Weights and Measures defined the second of atomic time in the International System of Units (SI) as
The ground state is defined at zero magnetic field. The second thus defined is equivalent to the ephemeris second.
The definition of the second was later refined at the 1997 meeting of the BIPM to include the statement
The revised definition would seem to imply that the ideal atomic clock would contain a single caesium atom at rest emitting a single frequency. In practice, however, the definition means that high-precision realizations of the second should compensate for the effects of the ambient temperature (black-body radiation) within which atomic clocks operate and extrapolate accordingly to the value of the second as defined above.