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Boltzmann constant: 1.380 649 × 10 −23 J⋅K −1: 0 [5] Newtonian constant of gravitation: 6.674 30 (15) × 10 −11 m 3 ⋅kg −1 ⋅s −2: 2.2 × 10 −5 [6] cosmological constant: 1.089(29) × 10 −52 m −2 [c] 1.088(30) × 10 −52 m −2 [d] 0.027 0.028 [7] [8]
The astronomical unit of length is that length (A) for which the Gaussian gravitational constant (k) takes the value 0.017 202 098 95 when the units of measurement are the astronomical units of length, mass and time. The dimensions of k 2 are those of the constant of gravitation (G), i.e., T −2 L 3 M −1.
The measured value of the constant is known with some certainty to four significant digits. In SI units, its value is approximately 6.6743 × 10 −11 m 3 kg −1 s −2. [1] The modern notation of Newton's law involving G was introduced in the 1890s by C. V. Boys.
Assuming SI units, F is measured in newtons (N), m 1 and m 2 in kilograms (kg), r in meters (m), and the constant G is 6.674 30 (15) × 10 −11 m 3 ⋅kg −1 ⋅s −2. [12] The value of the constant G was first accurately determined from the results of the Cavendish experiment conducted by the British scientist Henry Cavendish in 1798 ...
newton meter squared per kilogram squared (N⋅m 2 /kg 2) shear modulus: pascal (Pa) or newton per square meter (N/m 2) gluon field strength tensor: inverse length squared (1/m 2) acceleration due to gravity: meters per second squared (m/s 2), or equivalently, newtons per kilogram (N/kg) magnetic field strength
kg⋅m/s L M T −1: vector, extensive Pop: p →: Rate of change of crackle per unit time: the sixth time derivative of position m/s 6: L T −6: vector Pressure gradient: Pressure per unit distance pascal/m L −2 M 1 T −2: vector Temperature gradient: steepest rate of temperature change at a particular location K/m
In SI units, this acceleration is expressed in metres per second squared (in symbols, m/s 2 or m·s −2) or equivalently in newtons per kilogram (N/kg or N·kg −1). Near Earth's surface, the acceleration due to gravity, accurate to 2 significant figures, is 9.8 m/s 2 (32 ft/s 2).
μ = Gm 1 + Gm 2 = μ 1 + μ 2, where m 1 and m 2 are the masses of the two bodies. Then: for circular orbits, rv 2 = r 3 ω 2 = 4π 2 r 3 /T 2 = μ; for elliptic orbits, 4π 2 a 3 /T 2 = μ (with a expressed in AU; T in years and M the total mass relative to that of the Sun, we get a 3 /T 2 = M) for parabolic trajectories, rv 2 is constant and ...