Detail; Chronology; Radiation-dominated era; Matter-dominated era; Dark-energy-dominated era (a) If The Scale Factor A = 1 Today, What Will A Be When Our Sun Burns Out 5 Billion Years From Now? This leads to dominance of radiation in the very early universe but a transition to a matter dominated universe at a later time.
Dark energy dominates the total energy (74%) while dark matter (22%) constitutes most of the mass. Using the dimensionless scale factor R to characterized the expansion of the universe, the effective energy densities of radiation and mass scale differently. What is the corresponding redshift? There is therefore a stage, at a finite time in the past, at which the scale factor must shrink to zero and the energy density becomes infinite. Thus, at times sufficiently far in the future from a mp, the phantom energy term must dominate, so this becomes effectively a single component universe with a Friedmann equation ˙ a 2 H 2 0 ≈ 1-Ω m, 0 a 1+3 w p where we’ve dropped the negligible contribution to the energy density from matter (diluting as a-3) and multiplied through by a 2. Estimated relative distribution for components of the energy density of the universe. Question: Let’s Say Dark Energy Continues To Dominate The Energy Density Of The Universe Into The Future. In this universe the energy density is, in total, decreasing. At which scale factor a started the cosmological constant to dominate the energy density of the Universe? However recombination happened about 380,000 thousand years after the Big Bang and by then the energy density of radiation made a negligible contribution to the total energy density. We have seen that in a homogeneous, isotropic universe the only change allowed is an overall expansion or contraction, which is characterised by the scale length R(t).The rate of change of R (the "speed" of expansion of the universe) is written , but it is usually more convenient to work with the Hubble parameter H = /R. In order to know the actual density and how redshift relates to the age of the universe you must know the Hubble parameter today as well as the current ratio between the energy densities. - EARLY EXPONENTIAL PHASE OF GROWTH OF SCALE FACTOR (after T ~ TGUT ~ 1015 GeV) -Phenomenologically similar to Universe with a dominant cosmological constant, however inflation needs to end while exponential scale factor growth in a Λ-dominated phase does not need to end (de Sitter solution of Friedmann eqs.) The relative expansion of the universe is parametrized by a dimensionless scale factor.Also known as the cosmic scale factor or sometimes the Robertson Walker scale factor, [1] this is a key parameter of the Friedmann equations.. for the details of the calculation. Just for the clarity of those who might be less familiar with this topic, the dimensionless scale factor [math]a(t)[/math] indicates that the universe is expanding. The upper line corresponds to k = -1, the middle line to the flat k = 0 model, and the lowest line to the recollapsing closed k = +1 universe. You can easily compute how matter or dark energy density scales with the scale factor (and therefore with redshift). Contents. Of the remaining baryonic matter (4%), only one tenth is compact. Scale factor (cosmology) Last updated December 29, 2019. 2. Figure 3.4. At which scale factor a started matter to dominate the energy density of the Universe? 1.
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