But Einstein’s cosmological constant is back and now in play again (Sawyer 33, Reiss 18). Models with total > 1 are always spatially closed (open for 1), although closed models can still expand to infinity if v 0.

The 1998 Report The team who uncovered the accelerating expansion studied Type Ia supernova and gathered values of high redshift (far away) versus low redshift (close by) in order to get a good value for the cosmological constant, or Λ. Figure 3.5.

In this article the phenomenon of degravitation of the cosmological constant is studied in the framework of bigravity. Several months ago the Discovery Channel aired a television series featuring Stephen Hawking called Curiosity.. This plot shows the different possibilities for the cosmological expansion as a function of matter density and vacuum energy. The density of the dark energy is not varying rapidly as the universe expands, and if it is truly time-independent then it is just the effect that would be expected from a cosmological constant. In other words, it is no longer necessary to assume an expansion of the universe, because there is enough gas in the universe to produce the same red shift. This would imply a non-zero value for the 'Cosmological Constant' (CC). If the cosmological constant is negative, recollapse always occurs; recollapse is also possible with a positive v if m >> v. The cosmological constant represents the biggest problem in physics today. Whereas in his book The Grand Design Hawking claimed that God is not necessary to explain the origin of the universe given the existence of physical laws such as gravity, in Curiosity he argued that God could not have created the universe because there was no time in which … However this works out, it is still puzzling why the cosmological constant is not as large as would be expected from calculations of quantum fluctuations. The gravitational effect of matter caused an acceleration in this model which Einstein did not want, since at the time the Universe was not known to be expanding. As matter becomes less and less important, dark energy becomes the only term that matters. The smaller is the value of w, the greater its accelerating e®ect. This Is Why Dark Energy Is The Biggest Unsolved Problem In The Universe. Einstein's original cosmological model was a static, homogeneous model with spherical geometry. In physical cosmology, cosmic inflation, cosmological inflation, or just inflation, is a theory of exponential expansion of space in the early universe.The inflationary epoch lasted from 10 −36 seconds after the conjectured Big Bang singularity to some time between 10 −33 and 10 −32 seconds after the singularity. "If new observations came in tomorrow and showed we were wrong, and the cosmological constant was zero, 99% of physicists would breathe a sigh of relief," says Ben Allanach from the University of Cambridge. Observational data (primarily the CMB) tell us that the curvature must be close to flat, but do not tell us that it is exactly flat. cosmological constant has w precisely equal to ¡ 1. Both mentioned cosmological constant problems can be considered in the framework of the extension of the standard cosmological [LAMBDA]CDM model in which the cosmological constant (naturally interpreted as related to the vacuum energy density) is running and its value is changing during the cosmic evolution. The data points to a true cosmological "constant," but other possibilities are still allowed. where M=e 2 h/(3pe o c 5 m e 2 C 4), h is the Planck constant.Thus, M=2.73´10-21 K-2 From this mechanism, it has been calculated that an average density of 0.01 atom/cm 3 is sufficient to produce a red shift equal to the Hubble parameter. Furthermore, because the quintessence component evolves in time, it is, by general covariance, Unlike a cosmological constant, the quintessential pressure and energy density evolve in time, and w may also do so.


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