The small universe inflated by a large amount and the part of the universe you can observe appears to be nearly flat.
That solves the flatness problem.
The horizon problem is solved by inflation because regions that appear to be isolated from each other were in contact with each other before the inflation period.Jun 28, 2022.
The flatness problem is naturally solved by the Einstein–Cartan–Sciama–Kibble theory of gravity, without an exotic form of matter required in inflationary theory..
In a universe with zero curvature, the local geometry is flat.
The most obvious global structure is that of Euclidean space, which is infinite in extent.
Flat universes that are finite in extent include the torus and Klein bottle..
In a flat universe, as seen on the left, a straight line will extend out to infinity.
A closed universe, right, is curled up like the surface of a sphere.
In it, a straight line will eventually return to its starting point..
This seems like a truly remarkable coincidence and has become known as the 'flatness problem'.
There is no known reason for the density of the Universe to be so close to the critical density, and this appears to be an unacceptably strange coincidence in the view of most astronomers.
Hence the flatness 'problem'..
The problem is that according to the original Big Bang theory there hasn't been enough expansion since the Big Bang to smooth out the curvature of the observable universe.
And the chances of the whole universe being flat are so astronomically low that it's effectively impossible.Feb 23, 2023.
This seems like a truly remarkable coincidence and has become known as the 'flatness problem'.
There is no known reason for the density of the Universe to be so close to the critical density, and this appears to be an unacceptably strange coincidence in the view of most astronomers.
Hence the flatness 'problem'..
The flatness problem (also known as the oldness problem) is a cosmological fine-tuning problem within the Big Bang model of the universe
According to Einstein's field equations of general relativity, the structure of spacetime is affected by the presence of matter and energy
The value of Ω at the present time is denoted Ω0. This value can be deduced by measuring the curvature of spacetime (since Ω = 1, or
Some cosmologists agreed with Dicke that the flatness problem was a serious one
• Magnetic monopole• Horizon
Cosmological fine-tuning problem
