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Что (кто) такое oldness$54835$ - определение
![The relative density Ω against [[cosmic time]] ''t'' (neither axis to scale). Each curve represents a possible universe: note that Ω diverges rapidly from 1. The blue curve is a universe similar to our own, which at the present time (right of the graph) has a small |Ω − 1| and therefore must have begun with Ω very close to 1 indeed. The red curve is a hypothetical different universe in which the initial value of Ω differed slightly too much from 1: by the present day it has diverged extremely and would not be able to support galaxies, stars or planets.](https://commons.wikimedia.org/wiki/Special:FilePath/Flatness problem density graph.svg?width=200 "The relative density Ω against [[cosmic time]] ''t'' (neither axis to scale). Each curve represents a possible universe: note that Ω diverges rapidly from 1. The blue curve is a universe similar to our own, which at the present time (right of the graph) has a small |Ω − 1| and therefore must have begun with Ω very close to 1 indeed. The red curve is a hypothetical different universe in which the initial value of Ω differed slightly too much from 1: by the present day it has diverged extremely and would not be able to support galaxies, stars or planets.")
![Comparison of a normal aged brain (left) and a brain affected by [[Alzheimer's disease]]](https://commons.wikimedia.org/wiki/Special:FilePath/Alzheimer's disease brain comparison.jpg?width=200 "Comparison of a normal aged brain (left) and a brain affected by [[Alzheimer's disease]]")
![Somali]] woman](https://commons.wikimedia.org/wiki/Special:FilePath/Habibaadansalat.jpg?width=200 "Somali]] woman")
![Hydra]]'', a relative of the jellyfish](https://commons.wikimedia.org/wiki/Special:FilePath/Hydras (8).JPG?width=200 "Hydra]]'', a relative of the jellyfish")
![[[Christoffer Wilhelm Eckersberg]]: ''Ages of Man''](https://commons.wikimedia.org/wiki/Special:FilePath/Menneske Aldrene (C. W. Eckersberg).png?width=200 "[[Christoffer Wilhelm Eckersberg]]: ''Ages of Man''")
Википедия
The flatness problem (also known as the oldness problem) is a cosmological fine-tuning problem within the Big Bang model of the universe. Such problems arise from the observation that some of the initial conditions of the universe appear to be fine-tuned to very 'special' values, and that small deviations from these values would have extreme effects on the appearance of the universe at the current time.
In the case of the flatness problem, the parameter which appears fine-tuned is the density of matter and energy in the universe. This value affects the curvature of space-time, with a very specific critical value being required for a flat universe. The current density of the universe is observed to be very close to this critical value. Since any departure of the total density from the critical value would increase rapidly over cosmic time, the early universe must have had a density even closer to the critical density, departing from it by one part in 1062 or less. This leads cosmologists to question how the initial density came to be so closely fine-tuned to this 'special' value.
The problem was first mentioned by Robert Dicke in 1969.: 62, : 61 The most commonly accepted solution among cosmologists is cosmic inflation, the idea that the universe went through a brief period of extremely rapid expansion in the first fraction of a second after the Big Bang; along with the monopole problem and the horizon problem, the flatness problem is one of the three primary motivations for inflationary theory.
