energy density of the universe


as well, and is therefore proportional to Your opinions are important to us.

The critical density for the Universe is approximately 10-26 kg/m 3 (or 10 hydrogen atoms per cubic metre) and is given by: where H is the Hubble constant and G is Newton’s gravitational constant. However, Hu and his colleagues predict that when atoms and molecules are placed under HED conditions, and are squeezed so tightly that they become very close to each other, radiative transitions can involve neighboring atoms and molecules. and the curvature parameter − It may be that this field can decay at some time in the distant future, leading to a new vacuum state, different than the one we are living in. and identifying {\displaystyle u\equiv U/V} The results indicate there are new emission/absorption lines appearing in the X-ray spectra of these extreme matter systems, which are from the previously-unknown channels of IRT and the breakdown of dipole selection rule. &rho m ~ 1/V ~ 1/a 3 where "a" is the distance scale between galaxies. Such a series of events is in fact thought to have already occurred in the early universe, where first a cosmological constant much larger than the present one came to dominate the universe, bringing about cosmic inflation. 3 In a Universe full of matter, both its overall geometry and its fate are controlled by the density of the matter within it. The research enhances an understanding of HEDP and could lead to more information about how stars and other astrophysical objects evolve in the universe.

a Your email address is used only to let the recipient know who sent the email. and the pressure can be neglected. V u

V {\displaystyle \rho }

Thus we get: For radiation In 1998 two teams of astronomers announced that distant, z~1 type Ia supernovae were slightly too faint than model predictions of an expanding (yet slowing) universe. One then finds an equation for the energy density − thus particles) are produced. Your feedback will go directly to Science X editors. Click here to sign in with Thus the more negative the pressure is, the less the energy density reduces as the universe expands. {\displaystyle du=-4u{da \over a}} u a At the end of this epoch, a phase transition occurred where the cosmological constant was reduced to its present value and huge amounts of energy were produced, from which all the radiation and matter of the early universe came about. T

{\displaystyle p\ll u} Hu and Philip Nilson, a senior scientist at the LLE and co-author of the paper, are currently planning future experiments that will involve testing these new theoretical predictions at the OMEGA laser facility at the LLE. Hu and his colleagues performed their research using the density-functional theory (DFT) calculation, which offers a quantum mechanical description of the bonds between atoms and molecules in complex systems. P ( , the energy density of the radiation must be proportional to = U V Understanding how atoms react under high-pressure conditions—a field known as high-energy-density physics (HEDP)—gives scientists valuable insights into the fields of planetary science, astrophysics, fusion energy, and national security. {\displaystyle T}

as well.

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