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The gravitational constant appears in the Einstein field equations of general relativity, [4] [5] + =, where G μν is the Einstein tensor (not the gravitational constant despite the use of G), Λ is the cosmological constant, g μν is the metric tensor, T μν is the stress–energy tensor, and κ is the Einstein gravitational constant, a ...
^ Surface gravity derived from the mass m, the gravitational constant G and the radius r: Gm/r 2. ^ Escape velocity derived from the mass m, the gravitational constant G and the radius r: √ (2Gm)/r. ^ Orbital speed is calculated using the mean orbital radius and the orbital period, assuming a circular orbit. ^ Assuming a density of 2.0
where F is the gravitational force acting between two objects, m 1 and m 2 are the masses of the objects, r is the distance between the centers of their masses, and G is the gravitational constant. The first test of Newton's law of gravitation between masses in the laboratory was the Cavendish experiment conducted by the British scientist Henry ...
The constants listed here are known values of physical constants expressed in SI units; that is, physical quantities that are generally believed to be universal in nature and thus are independent of the unit system in which they are measured. Many of these are redundant, in the sense that they obey a known relationship with other physical ...
The rationale for choosing a manifold as the fundamental mathematical structure is to reflect desirable physical properties. For example, in the theory of manifolds, each point is contained in a (by no means unique) coordinate chart, and this chart can be thought of as representing the 'local spacetime' around the observer (represented by the ...
The "force constant" is just the coefficient of the displacement term in the equation of motion: m a + b v + k x + constant = F(X,t) m mass, a acceleration, b viscosity, v velocity, k force constant, x displacement F external force as a function of location/position and time. F is the force being measured, and F / m is the acceleration.
Normalizes the characteristic impedance Z g of gravitational radiation in free space to 1 (normally expressed as 4 π G / c ). [note 2] Eliminates 4 π G from the Bekenstein–Hawking formula (for the entropy of a black hole in terms of its mass m BH and the area of its event horizon A BH) which is simplified to S BH = π A BH = (m BH) 2.
The standard gravitational parameter μ of a celestial body is the product of the gravitational constant G and the mass M of that body. For two bodies, the parameter may be expressed as G ( m 1 + m 2 ) , or as GM when one body is much larger than the other: μ = G ( M + m ) ≈ G M . {\displaystyle \mu =G(M+m)\approx GM.}