Editing Flatness problem (section)

===Implication===
This tiny value is the crux of the flatness problem. If the initial density of the universe could take any value, it would seem extremely surprising to find it so 'finely tuned' to the critical value <math>\rho_c</math>. Indeed, a very small departure of Ω from 1 in the early universe would have been magnified during billions of years of expansion to create a current density very far from critical. In the case of an overdensity {{nowrap|(<math>\rho > \rho_c</math>)}} this would lead to a universe so dense it would cease expanding and collapse into a [[Big Crunch]] (an opposite to the Big Bang in which all matter and energy falls back into an extremely dense state) in a few years or less; in the case of an underdensity {{nowrap|(<math>\rho < \rho_c</math>)}} it would expand so quickly and become so sparse it would soon seem essentially empty, and [[gravity]] would not be strong enough by comparison to cause matter to collapse and [[galaxy formation|form galaxies]] resulting in a [[big Freeze|big freeze]]. In either case the universe would contain no complex structures such as galaxies, stars, planets and any form of life.<ref>Ryden p. 193</ref>

This problem with the Big Bang model was first pointed out by [[Robert Dicke]] in 1969,<ref name=Reality>{{cite book |url=https://books.google.com/books?id=OIG0F37QrmQC&q=%22flatness+problem+was%22&pg=PT237 |title=The Reality of the Unobservable: Observability, Unobservability and Their Impact on the Issue of Scientific Realism |first=Evandro |last=Agazzi |author2=Massimo Pauri |isbn=978-0-7923-6311-8 |publisher=Springer |date=2000 |page=226|bibcode=2000ruou.book.....A }}</ref> and it motivated a search for some reason the density should take such a specific value.