de sitter universe造句

• By using the de Sitter universe instead, where the expansion is truly exponential, there are many simplifications.
• In particular O ( 4, 1 ) is the isometry group of the de Sitter universe dS 4, a cosmological model.
• When ( 3 space dimensions plus time ), it is a cosmological model for the physical universe; see de Sitter universe.
• Therefore, any observer in a de Sitter universe would see event horizons beyond which that observer can never see nor learn any information.
• An example of a cosmological model with an event horizon is a universe dominated by the cosmological constant ( a de Sitter universe ).
• Eventually there will be almost nothing left but the vacuum energy, tiny thermal fluctuations, quantum fluctuations and our universe will have become a de Sitter universe.
• Because our Universe entered the Dark Energy Dominated Era about five billion years ago, our universe is probably approaching a de Sitter universe in the infinite future.
• An anti-de Sitter universe would be " curved " in such a manner that the expansion from the big bang would gradually decelerate and collapse into a big crunch.
• For the case of a horizon perceived by an occupant of a de Sitter universe, the horizon always appears to be a fixed distance away for a non-accelerating observer.
• He also came up with the concept of the de Sitter space and de Sitter universe, a solution for Einstein's general relativity in which there is no matter and a positive cosmological constant.
• However, as the exponential growth of the near-de Sitter universe dilutes the bubbles nucleated, it is not obvious that the bubbles will really coalesse, in fact Guth and Weinberg proved the following statements:
• Following the discovery by Edwin Hubble of a linear relation between the redshifts of the galaxies and their distance in 1929, Einstein abandoned his static model of the universe and proposed expanding models such as the Friedmann-Einstein universe and the Einstein-de Sitter universe.
• Following the discovery of the recession of the nebulae by Edwin Hubble in 1929, Einstein abandoned his static model of the universe, and proposed two dynamic models of the cosmos, The Friedmann-Einstein universe of 1931 and the Einstein de Sitter universe of 1932.
• If our universe is approaching a de Sitter universe then eventually we will not be able to observe any galaxies other than our own Milky Way ( and any others in the gravitationally bound Local Group, assuming they were to somehow survive to that time without merging ).
• Since the simplest cosmological model ( the De Sitter universe ) that solves that equation is a spherically symmetric, stationary, closed universe ( exhibiting a cosmological red shift, which is more conventionally interpreted as due to expansion ), it seemed to explain the overall form of the universe.
• A simple example of an asymptotically flat spacetime is the Schwarzschild-de Sitter lambdavacuum solution ( sometimes called the K鰐tler solution ), which models a spherically symmetric massive object immersed in a de Sitter universe, is an example of an " asymptotically simple " spacetime which is not asymptotically flat.
• Unique to universes described by the FLRW metric, a de Sitter universe has a Hubble Law that is not only consistent through all space, but also through all time ( since the deceleration parameter is q =-1 ), thus satisfying the perfect cosmological principle that assumes isotropy and homogeneity throughout space and time.
• The Schwarzschild solution is the simplest spherically symmetric solution of the Einstein equations with zero cosmological constant, and it describes a black hole event horizon in otherwise empty space . de Sitter Schwarzschild is a combination of the two, and describes a black hole horizon spherically centered in an otherwise de Sitter universe.