The gravitational constant, also known as the universal gravitational constant, or as Newton's constant, denoted by the letter G, is an empirical physical constant involved in the calculation of gravitational effects in Sir Isaac Newton's law of universal gravitation and in Albert Einstein's general theory of relativity. Its measured value is approximately ×10−11 m3⋅kg−1⋅s−2. 6.674
Law of gravitation
According to Newton's law of universal gravitation, the attractive force (F) between two point-like bodies is directly proportional to the product of their masses (m1 and m2), and inversely proportional to the square of the distance, r, (inverse-square law) between them:
The constant of proportionality, G, is the gravitational constant. Colloquially, the gravitational constant is also called "Big G", for disambiguation with "small g" (g), which is the local gravitational field of Earth (equivalent to the free-fall acceleration). The two quantities are related by g = GME/rE2 (where ME is the mass of the Earth and rE is the radius of the Earth).
In the general theory of relativity, the Einstein field equations,
Newton's constant appears in the proportionality between the spacetime curvature and the energy density component of the stress–energy tensor. The scaled gravitational constant κ = 8π/c4G ≈ ×10−43 s2⋅m−1⋅kg−12.071 (depending on the choice of definition of the stress–energy tensor it can also be normalized as κ = 8π/c2G ≈ ×10−26 m⋅kg−11.866) is also known as Einstein's constant.
Value and dimensions
The gravitational constant is a physical constant that is difficult to measure with high accuracy. This is because the gravitational force is extremely weak compared with other fundamental forces.[a]
In SI units, the 2014 CODATA-recommended value of the gravitational constant (with standard uncertainty in parentheses) is:
This corresponds to a relative standard uncertainty of ×10−5. 4.7
The dimensions assigned to the gravitational constant are force times length squared divided by mass squared; this is equivalent to length cubed, divided by mass and by time squared:
In SI base units, this amounts to meters cubed per kilogram per second squared:
In cgs, G can be written as G ≈ ×10−8 cm3⋅g−1⋅s−2. 6.674
The gravitational constant is taken as the basis of the Planck units: it is equal to the cube of the Planck length divided by the product of the Planck mass and the square of Planck time:
In other words, in Planck units, G has the numerical value of . 1
Thus, in Planck units, and other natural units taking G as their basis, the gravitational constant cannot be measured as it is set to its value by definition. Depending on the choice of units, variation in a physical constant in one system of units shows up as variation of another constant in another system of units; variation in dimensionless physical constants is preserved independently of the choice of units; in the case of the gravitational constant, such a dimensionless value is the gravitational coupling constant,
a measure for the gravitational attraction between a pair of electrons, proportional to the square of the electron rest mass.
In astrophysics, it is convenient to measure distances in parsecs (pc), velocities in kilometers per second (km/s) and masses in solar units M⊙. In these units, the gravitational constant is:
For situations where tides are important, the relevant length scales are solar radii, rather than parsecs. In these units, the gravitational constant is:
In orbital mechanics, the period P of an object in circular orbit around a spherical object obeys
where V is the volume inside the radius of the orbit. It follows that
This way of expressing G shows the relationship between the average density of a planet and the period of a satellite orbiting just above its surface.
For elliptical orbits, applying Kepler's 3rd law, expressed in units characteristic of Earth's orbit:
where distance is measured in astronomical units (AU), time in years, and mass in solar masses (M⊙).
History of measurement
Diagram of torsion balance used in the Cavendish experiment
performed by Henry Cavendish
in 1798, to measure G, with the help of a pulley, large balls hung from a frame were rotated into position next to the small balls.
The gravitational constant appears in Newton's law of universal gravitation, but it was not measured until 1798, seventy-one years after Newton's death, when Henry Cavendish performed his Cavendish experiment (Philosophical Transactions 1798). Cavendish measured G implicitly, using a torsion balance invented by the geologist Rev. John Michell. He used a horizontal torsion beam with lead balls whose inertia (in relation to the torsion constant) he could tell by timing the beam's oscillation. Their faint attraction to other balls placed alongside the beam was detectable by the deflection it caused. Cavendish's aim was not actually to measure the gravitational constant, but rather to measure Earth's density relative to water, through the precise knowledge of the gravitational interaction. In modern units, the density that Cavendish calculated implied a value for G of ×10−11 m3⋅kg−1⋅s−26.674.
The accuracy of the measured value of G has increased only modestly since the original Cavendish experiment. G is quite difficult to measure because gravity is much weaker than other fundamental forces, and an experimental apparatus cannot be separated from the gravitational influence of other bodies. Furthermore, gravity has no established relation to other fundamental forces, so it does not appear possible to calculate it indirectly from other constants that can be measured more accurately, as is done in some other areas of physics. Published values of G have varied rather broadly, and some recent measurements of high precision are, in fact, mutually exclusive. This led to the 2010 CODATA value by NIST having 20% increased uncertainty than in 2006. For the 2014 update, CODATA reduced the uncertainty to less than half the 2010 value.
In the January 2007 issue of Science, Fixler et al. described a new measurement of the gravitational constant by atom interferometry, reporting a value of G = ×10−11 m3⋅kg−1⋅s−26.693(34). An improved cold atom measurement by Rosi et al. was published in 2014 of G = 91(99)×10−11 m3 kg−1 s−26.671.
A controversial 2015 study of some previous measurements of G, by Anderson et al., suggested that most of the mutually exclusive values can be explained by a periodic variation. The variation was measured as having a period of 5.9 years, similar to that observed in length-of-day (LOD) measurements, hinting at a common physical cause which is not necessarily a variation in G. A response was produced by some of the original authors of the G measurements used in Anderson et al. This response notes that Anderson et al. not only omitted measurements, they also used the time of publication not the time the experiments were performed. A plot with estimated time of measurement from contacting original authors seriously degrades the length of day correlation. Also taking the data collected over a decade by Karagioz and Izmailov shows no correlation with length of day measurements. As such the variations in G most likely arise from systematic measurement errors which have not properly been accounted for.
Under the assumption that the physics of type Ia supernovae are universal, analysis of observations of 580 type Ia supernovae has shown that the gravitational constant has varied by less than one part in ten billion per year over the last nine billion years.
The GM product
The quantity GM—the product of the gravitational constant and the mass of a given astronomical body such as the Sun or Earth—is known as the standard gravitational parameter and is denoted μ. Depending on the body concerned, it may also be called the geocentric or heliocentric gravitational constant, among other names.
This quantity gives a convenient simplification of various gravity-related formulas. Also, for celestial bodies such as Earth and the Sun, the value of the product GM is known much more accurately than each factor independently. Indeed, the limited accuracy available for G limits the accuracy of determination of such masses in the first place.
For Earth, using M⊕ as the symbol for the mass of Earth, we have
For Sun, we have
Calculations in celestial mechanics can also be carried out using the units of solar masses, mean solar days and astronomical units rather than standard SI units. In this case we use the Gaussian gravitational constant k, where
If instead of mean solar day we use the sidereal year as our time unit, the value of ks is very close to 2π (k = 156.283).
The standard gravitational parameter GM appears as above in Newton's law of universal gravitation, as well as in formulas for the deflection of light caused by gravitational lensing, in Kepler's laws of planetary motion, and in the formula for escape velocity.
- ^ For example, the gravitational force between an electron and proton one meter apart is approximately −67 N, whereas the 10electromagnetic force between the same two particles is approximately −28 N. The electromagnetic force in this example is some 39 10orders of magnitude (i.e. 1039) greater than the force of gravity—roughly the same ratio as the mass of the Sun to a microgram.
- ^ "CODATA Value: Newtonian constant of gravitation". The NIST Reference on Constants, Units, and Uncertainty. US National Institute of Standards and Technology. June 2015. Retrieved 2015-09-25.
2014 CODATA recommended values
- ^ Gundlach, Jens H.; Merkowitz, Stephen M. (2002-12-23). "University of Washington Big G Measurement". Astrophysics Science Division. Goddard Space Flight Center.
Since Cavendish first measured Newton's Gravitational constant 200 years ago, "Big G" remains one of the most elusive constants in physics
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- ^ Mohr, Peter J.; Newell, David B.; Taylor, Barry N. (2015-07-21). "CODATA Recommended Values of the Fundamental Physical Constants: 2014". Reviews of Modern Physics. 88. arXiv:1507.07956 [physics.atom-ph]. Bibcode:2016RvMP...88c5009M. doi:10.1103/RevModPhys.88.035009.
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