These models solve the horizon problem through an expanding epoch well before the Big Bang, and then generate the required spectrum of primordial density perturbations during a contracting phase leading to a Big Crunch. Planck survey of the CMB. Cosmic inflation refers to the very early universe undergoing a sudden and massive expansion. Get breaking space news and the latest updates on rocket launches, skywatching events and more! Coleman found the most likely decay pathway for vacuum decay and calculated the inverse lifetime per unit volume. The theory of cosmic inflation, first proposed in the 1980s by MIT’s Alan Guth, the V.F. [23], Inflation is a period of supercooled expansion, when the temperature drops by a factor of 100,000 or so. Things are constantly moving beyond the cosmological horizon, which is a fixed distance away, and everything becomes homogeneous. COSMIC RAYS - Smiling Expert. 2 1. horizon problem 2. flatness problem 3. structure problem. Starobinsky's and Guth's scenarios both predicted an initial de Sitter phase, differing only in mechanistic details. The spatial slices are expanding very fast to cover huge volumes. The idea is that the geometry and uniformity of the cosmos were established during an intense early growth spurt. 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. So it is not seen as problematic that a field responsible for cosmic inflation and the metric expansion of space has not yet been discovered. Expansion refers to the rate at which the universe is getting larger. If this field did not exist, scientists would have to propose a different explanation for all the observations that strongly suggest a metric expansion of space has occurred, and is still occurring (much more slowly) today. String theory requires that, in addition to the three observable spatial dimensions, additional dimensions exist that are curled up or compactified (see also Kaluza–Klein theory). This prediction implies that the total ordinary matter, dark matter and residual vacuum energy in the Universe have to add up to the critical density, and the evidence supports this. Cosmic inflation theory, first proposed by Alan Guth in 1981, modified the Big Bang theory (the Standard Model) by proposing that the universe, instead of unfolding at a steady pace, expanded rapidly shortly after it was created, which could account for apparent fine-tuning. After all, the whole point of inflation is that it takes the quantum-scale dynamics of spacetime itself and magnifies them to cosmic proportions. In particular, high precision measurements of the so-called "B-modes" of the polarization of the background radiation could provide evidence of the gravitational radiation produced by inflation, and could also show whether the energy scale of inflation predicted by the simplest models (1015–1016 GeV) is correct. 12 This theory, governed by the Dirac-Born-Infeld action, is different from ordinary inflation. Inflation supposedly was far, far faster than light. The view from Mars: Here's the 1st photo from NASA's Perseverance rover. These problems arise from the observation that to look like it does today, the Universe would have to have started from very finely tuned, or "special" initial conditions at the Big Bang. [88] Other forthcoming measurements, such as those of 21 centimeter radiation (radiation emitted and absorbed from neutral hydrogen before the first stars formed), may measure the power spectrum with even greater resolution than the CMB and galaxy surveys, although it is not known if these measurements will be possible or if interference with radio sources on Earth and in the galaxy will be too great.[89]. If the energy density is larger than can be held by the quantized spacetime, it is thought to bounce back.[123]. n The inflationary epoch lasted from 10 seconds after the conjectured Big Bang singularity to some time between 10 and 10 seconds after the singularity. The minimal coupling between torsion and Dirac spinors generates a spin-spin interaction that is significant in fermionic matter at extremely high densities. It appears that special conditions are necessary since inflation occurs in tunneling between two vacua in the string landscape. The ekpyrotic and cyclic models are also considered adjuncts to inflation. Like a metastable phase in statistical mechanics—water below the freezing temperature or above the boiling point—a quantum field would need to nucleate a large enough bubble of the new vacuum, the new phase, in order to make a transition.
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