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As the universe expands and the matter in it thins, the gravitational attraction decreases (since it is proportional to the density), while the cosmological repulsion increases. Thus, the ultimate fate of the ΛCDM universe is a near-vacuum expanding at an ever-increasing rate under the influence of the cosmological constant.
Fresh corroboration of the perplexing observation that the universe is expanding more rapidly than expected has scientists pondering the cause - perhaps some unknown factor involving the ...
Thus, an accelerating universe took a longer time to expand from 2/3 to 1 times its present size, compared to a non-accelerating universe with constant ˙ and the same present-day value of the Hubble constant. This results in a larger light-travel time, larger distance and fainter supernovae, which corresponds to the actual observations.
In the 1970s, the future of an expanding universe was studied by the astrophysicist Jamal Islam [12] and the physicist Freeman Dyson. [13] Then, in their 1999 book The Five Ages of the Universe, the astrophysicists Fred Adams and Gregory Laughlin divided the past and future history of an expanding universe into five eras.
It appears to be expanding faster today than it did in the past There is something unexpected happening in the universe, Nasa’s most powerful ever telescope shows Skip to main content
By doing so, the researchers hope to uncover fresh clues about how fast the universe is expanding and, just maybe, whether life could exist anywhere else in the universe.
A closed universe with Ω M > 1 and Ω Λ = 0 comes to an end in a Big Crunch and is considerably younger than its Hubble age. An open universe with Ω M ≤ 1 and Ω Λ = 0 expands forever and has an age that is closer to its Hubble age.
The Big Bang is a physical theory that describes how the universe expanded from an initial state of high density and temperature. [1] The notion of an expanding universe was first scientifically originated by physicist Alexander Friedmann in 1922 with the mathematical derivation of the Friedmann equations.