WebThis seems like a truly remarkable coincidence and has become known as the ‘ flatness problem ’. To phrase it more scientifically, the flatness problem arises because we … WebPhysical Keys to Cosmology ... The Flatness Problem. Observations indicate that the amount of matter in the universe is surely greater than one-tenth and surely less than ten times the critical amount needed to stop the expansion. It is either barely open or barely closed, or "very nearly flat". There is a good analogy here - a ball thrown up ...
WMAP Inflation Theory - NASA
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 … See more According to Einstein's field equations of general relativity, the structure of spacetime is affected by the presence of matter and energy. On small scales space appears flat – as does the surface of the Earth if one looks … See more Some cosmologists agreed with Dicke that the flatness problem was a serious one, in need of a fundamental reason for the closeness of the … See more Measurement The value of Ω at the present time is denoted Ω0. This value can be deduced by measuring the … See more • Magnetic monopole • Horizon problem See more http://hyperphysics.phy-astr.gsu.edu/hbase/Astro/cosmo.html mns orchids
cosmology - Why is the flatness problem a problem?
WebJan 1, 2024 · They claim that flat space-times in this set are actually typical on this natural measure and that therefore the flatness problem is illusory. I argue that they … WebOne can similarly argue that there are two ways of solving the second major prob- lem of standard cosmology, the so-called flatness problem. Today, space is, to a very good approximation, Euclidean. If it does have any spatial curvature (represented by the ak2 term in the cosmological equations), this is of O(H 2 ), i.e. extremely small. WebApr 23, 2024 · My understanding of the flatness problem is that it says that if we leave out dark energy and inflation, then the density parameter $\Omega(t)$ tends to $\infty$ or $0$ unless we have $\Omega(t) = 1$ exactly. Thus, $\Omega(t) = 1$ is an unstable equilibrium point, making it very strange to observe $\Omega(t_{0})\approx 1$ today. mns otc