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The result of this process, which lasts for 10 to 100 million years, is the formation of a limited number of Earth-sized bodies. Simulations show that the number of surviving planets is on average from 2 to 5. [2] [21] [62] [66] In the Solar System they may be represented by Earth and Venus. [21]
In general relativity, however, space and time may have curvature, so this distance formula must be modified to a more general form = just as we generalized the formula to measure distance on the surface of the Earth. The exact form of the metric g μν depends on the gravitating mass, momentum and energy, as described by the Einstein field ...
There are large variations in surface temperature over space and time on airless or near-airless bodies like Mars, which has daily surface temperature variations of 50–60 K. [18] [19] Because of a relative lack of air to transport or retain heat, significant variations in temperature develop. Assuming the planet radiates as a blackbody (i.e ...
Absolute equilibrium of free heat is the state of this fluid in a portion of space which receives as much of it as it lets escape. Relative equilibrium of free heat is the state of this fluid in two portions of space which receive from each other equal quantities of heat, and which moreover are in absolute equilibrium, or experience precisely ...
Munk & Wunsch (1998) estimated that Earth experiences 3.7 TW (0.0073 W/m 2) of tidal heating, of which 95% (3.5 TW or 0.0069 W/m 2) is associated with ocean tides and 5% (0.2 TW or 0.0004 W/m 2) is associated with Earth tides, with 3.2 TW being due to tidal interactions with the Moon and 0.5 TW being due to tidal interactions with the Sun. [3] Egbert & Ray (2001) confirmed that overall ...
Under Newtonian physics, an object in an (isolated) two-body system, consisting of the object orbiting a spherical mass, would trace out an ellipse with the center of mass of the system at a focus of the ellipse. The point of closest approach, called the periapsis (or when the central body is the Sun, perihelion), is fixed. Hence the major axis ...
Thus, any energy that enters a system but does not leave must be retained within the system. So, the amount of energy retained on Earth (in Earth's climate system) is governed by an equation: [change in Earth's energy] = [energy arriving] − [energy leaving]. Energy arrives in the form of absorbed solar radiation (ASR). Energy leaves as ...
In physics, the special theory of relativity, or special relativity for short, is a scientific theory of the relationship between space and time.In Albert Einstein's 1905 paper, On the Electrodynamics of Moving Bodies, the theory is presented as being based on just two postulates: [p 1] [1] [2]