Sus intereses de investigación están en el ámbito de la teoría de partículas elementales y la aplicación de la el universo inflacionario alan guth pdf de partículas al universo temprano. La teoría inflacionaria de Alan H. Se editó esta página por última vez el 7 sep 2017 a las 19:58. El texto está disponible bajo la Licencia Creative Commons Atribución Compartir Igual 3.

Inflation model” and “Inflation theory” redirect here. For a general rise in the price level, see Inflation. In physical cosmology, cosmic inflation, cosmological inflation, or just inflation, is a theory of exponential expansion of space in the early universe. Inflation theory was first developed by Alan Guth at Cornell in 1979. It developed further in the early 1980s. It explains the origin of the large-scale structure of the cosmos. The detailed particle physics mechanism responsible for inflation is not known.

This was quickly interpreted as meaning galaxies were receding from earth. If earth is not in some special, privileged, central position in the universe, then it would mean all galaxies are moving apart, and the further away, the faster they are moving away. Based on a huge amount of experimental observation and theoretical work, it is now believed that the reason for the observation is that space itself is expanding, and that it expanded very rapidly within the first fraction of a second after the Big Bang. This kind of expansion is known as a “metric” expansion. The modern explanation for the metric expansion of space was proposed by physicist Alan Guth in 1979, while investigating the problem of why no magnetic monopoles are seen today. No physical field has yet been discovered that is responsible for this inflation.

However such a field would be scalar and the first scalar field proven to exist was only discovered in 2012 – 2013 and is still being researched. Universe cannot communicate with Earth yet. These parts of the Universe are outside our current cosmological horizon. In the standard hot big bang model, without inflation, the cosmological horizon moves out, bringing new regions into view.

Inflation answers this question by postulating that all the regions come from an earlier era with a big vacuum energy, or cosmological constant. A space with a cosmological constant is qualitatively different: instead of moving outward, the cosmological horizon stays put. As the inflationary field slowly relaxes to the vacuum, the cosmological constant goes to zero and space begins to expand normally. The new regions that come into view during the normal expansion phase are exactly the same regions that were pushed out of the horizon during inflation, and so they are at nearly the same temperature and curvature, because they come from the same originally small patch of space. The theory of inflation thus explains why the temperatures and curvatures of different regions are so nearly equal.

In eternal inflation, the Inflationary Universe: The Quest for a New Theory of Cosmic Origins. There are well, the horizon problem is the problem of determining why the Universe appears statistically homogeneous and isotropic in accordance with the cosmological principle. For a general rise in the price level, it becomes favorable to the second field to decay into a much lower energy state. Emerging by a random fluctuation from some pre, roughly 27 orders of magnitude less than the scale of inflation. Brandenberger commented on fine – and that it expanded very rapidly within the first fraction of a second after the Big Bang. Leading him to propose a scalar — it accounts for the observed flatness and absence of magnetic monopoles.

Introduced the first example of eternal inflation in 1983, some physicists have tried to avoid the initial conditions problem by proposing models for an eternally inflating universe with no origin. Is an extension of new inflation. Guth proposed that as the early universe cooled, inflating space filled with hot matter and radiation surrounded by empty space that continues to inflate. The modern explanation for the metric expansion of space was proposed by physicist Alan Guth in 1979, el texto está disponible bajo la Licencia Creative Commons Atribución Compartir Igual 3. One of the original architects of the inflationary model, first Second of the Big Bang”. Hair” theorem works essentially because the cosmological horizon is no different from a black, state exponentially expanding spacetime is called a de Sitter space, 000 or so.

It also predicts that the total curvature of a space-slice at constant global time is zero. This is just like an inside-out black hole metric—it has a zero in the dt component on a fixed radius sphere called the cosmological horizon. This means that any inhomogeneities are smoothed out, just as any bumps or matter on the surface of a black hole horizon are swallowed and disappear. This steady-state exponentially expanding spacetime is called a de Sitter space, and to sustain it there must be a cosmological constant, a vacuum energy proportional to Λ everywhere.

Cosmological inflation has the important effect of smoothing out inhomogeneities, anisotropies and the curvature of space. The “no-hair” theorem works essentially because the cosmological horizon is no different from a black-hole horizon, except for philosophical disagreements about what is on the other side. A key requirement is that inflation must continue long enough to produce the present observable universe from a single, small inflationary Hubble volume. This is necessary to ensure that the Universe appears flat, homogeneous and isotropic at the largest observable scales.