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expansion post - Übersetzung nach russisch
нефтегазовая промышленность
раздвижная стойка, телескопическая стойка
![metric]] seen on the left. This visualization can be confusing because it appears as if the universe is expanding into a pre-existing empty space over time. Instead, the expansion created, and continues to create, all of known space and time.](https://commons.wikimedia.org/wiki/Special:FilePath/CMB Timeline300 no WMAP.jpg?width=200 "metric]] seen on the left. This visualization can be confusing because it appears as if the universe is expanding into a pre-existing empty space over time. Instead, the expansion created, and continues to create, all of known space and time.")
![critical density]] (<math>\Omega_m</math>).](https://commons.wikimedia.org/wiki/Special:FilePath/Evolution of the universe.svg?width=200 "critical density]] (<math>\Omega_m</math>).")
![When an object is receding, its light gets stretched ([[redshift]]ed). When the object is approaching, its light gets compressed ([[blueshift]]ed).](https://commons.wikimedia.org/wiki/Special:FilePath/Redshift blueshift.svg?width=200 "When an object is receding, its light gets stretched ([[redshift]]ed). When the object is approaching, its light gets compressed ([[blueshift]]ed).")
.png?width=200 "The diagram depicts the expansion of the universe and the relative observer phenomenon. The blue galaxies have expanded further apart than the white galaxies. When choosing an arbitrary reference point such as the gold galaxy or the red galaxy, the increased distance to other galaxies the further away they are appear the same. This phenomenon of expansion indicates two factors: there is no centralized point in the universe, and that the Milky Way Galaxy is not the center of the universe. The appearance of centrality is due to an observer bias that is equivalent no matter what location an observer sits.")
математика
асимптотически сходящаяся
Definition
Wikipedia
In general relativity, post-Newtonian expansions (PN expansions) are used for finding an approximate solution of Einstein field equations for the metric tensor. The approximations are expanded in small parameters that express orders of deviations from Newton's law of universal gravitation. This allows approximations to Einstein's equations to be made in the case of weak fields. Higher-order terms can be added to increase accuracy, but for strong fields sometimes it is preferable to solve the complete equations numerically. This method is a common mark of effective field theories. In the limit, when the small parameters are equal to 0, the post-Newtonian expansion reduces to Newton's law of gravity.
