Английская Википедия:Accelerating expansion of the universe

Lambda-CDM, accelerated expansion of the universe. The timeline in this schematic diagram extends from the Big Bang/inflation era 13.8 billion years ago to the present cosmological time.

Observations show that the expansion of the universe is accelerating, such that the velocity at which a distant galaxy recedes from the observer is continuously increasing with time.^[1]^[2]^[3] The accelerated expansion of the universe was discovered in 1998 by two independent projects, the Supernova Cosmology Project and the High-Z Supernova Search Team, which used distant type Ia supernovae to measure the acceleration.^[4]^[5]^[6] The idea was that as type Ia supernovae have almost the same intrinsic brightness (a standard candle), and since objects that are farther away appear dimmer, the observed brightness of these supernovae can be used to measure the distance to them. The distance can then be compared to the supernovae's cosmological redshift, which measures how much the universe has expanded since the supernova occurred; the Hubble law established that the farther away that an object is, the faster it is receding. The unexpected result was that objects in the universe are moving away from one another at an accelerating rate. Cosmologists at the time expected that recession velocity would always be decelerating, due to the gravitational attraction of the matter in the universe. Three members of these two groups have subsequently been awarded Nobel Prizes for their discovery.^[7] Confirmatory evidence has been found in baryon acoustic oscillations, and in analyses of the clustering of galaxies.

The accelerated expansion of the universe is thought to have begun since the universe entered its dark-energy-dominated era roughly 5 billion years ago.^[8]Шаблон:Refn Within the framework of general relativity, an accelerated expansion can be accounted for by a positive value of the cosmological constant Шаблон:Mvar, equivalent to the presence of a positive vacuum energy, dubbed "dark energy". While there are alternative possible explanations, the description assuming dark energy (positive Шаблон:Mvar) is used in the current standard model of cosmology, which also includes cold dark matter (CDM) and is known as the Lambda-CDM model.

Background

Шаблон:Nature timeline Шаблон:Further In the decades since the detection of cosmic microwave background (CMB) in 1965,^[9] the Big Bang model has become the most accepted model explaining the evolution of our universe. The Friedmann equation defines how the energy in the universe drives its expansion.

<math> H^2={\left ( \frac{\dot{a}}{a} \right )}^2=\frac{8{\pi}G}{3}\rho-\frac{{\kappa}c^2}{a^2} </math>

where Шаблон:Mvar represents the curvature of the universe, Шаблон:Math is the scale factor, Шаблон:Mvar is the total energy density of the universe, and Шаблон:Mvar is the Hubble parameter.^[10]

We define a critical density

and the density parameter

<math> \Omega=\frac{\rho}{\rho_c} </math>

We can then rewrite the Hubble parameter as

<math> H(a)=H_0 \sqrt{{\Omega_ka^{-2} + \Omega}_ma^{-3} + \Omega_ra^{-4} + \Omega_\mathrm{DE}a^{-3(1+w)}} </math>

where the four currently hypothesized contributors to the energy density of the universe are curvature, matter, radiation and dark energy.^[11] Each of the components decreases with the expansion of the universe (increasing scale factor), except perhaps the dark energy term. It is the values of these cosmological parameters which physicists use to determine the acceleration of the universe.

The acceleration equation describes the evolution of the scale factor with time

<math> \frac{\ddot{a}}{a}=-\frac{4{\pi}G}{3}\left( \rho + \frac{3P}{c^2} \right) </math>

where the pressure Шаблон:Mvar is defined by the cosmological model chosen. (see explanatory models below)

Physicists at one time were so assured of the deceleration of the universe's expansion that they introduced a so-called deceleration parameter Шаблон:Math.^[12] Current observations indicate this deceleration parameter is negative.

Relation to inflation

According to the theory of cosmic inflation, the very early universe underwent a period of very rapid, quasi-exponential expansion. While the time-scale for this period of expansion was far shorter than that of the current expansion, this was a period of accelerated expansion with some similarities to the current epoch.

Technical definition

The definition of "accelerating expansion" is that the second time derivative of the cosmic scale factor, <math> \ddot{a} </math>, is positive, which is equivalent to the deceleration parameter, <math>q</math>, being negative. However, note this does not imply that the Hubble parameter is increasing with time. Since the Hubble parameter is defined as <math> H(t) \equiv \dot{a}(t) / a(t) </math>, it follows from the definitions that the derivative of the Hubble parameter is given by

so the Hubble parameter is decreasing with time unless <math> q < -1 </math>. Observations prefer <math> q \approx -0.55 </math>, which implies that <math> \ddot{a} </math> is positive but <math> dH/dt </math> is negative. Essentially, this implies that the cosmic recession velocity of any one particular galaxy is increasing with time, but its velocity/distance ratio is still decreasing; thus different galaxies expanding across a sphere of fixed radius cross the sphere more slowly at later times.

It is seen from above that the case of "zero acceleration/deceleration" corresponds to <math> a(t)</math> is a linear function of <math>t</math>, <math> q = 0 </math>, <math> \dot{a} = const</math>, and <math> H(t) = 1/t </math>.

Evidence for acceleration

The rate of expansion of the universe can be analyzed using the magnitude-redshift relationship of astronomical objects using standard candles, or their distance-redshift relationship using standard rulers. Also a factor is the growth of large-scale structure, finding that the observed values of the cosmological parameters are best described by models which include an accelerating expansion.

Supernova observation

Файл:Asymmetric Ashes (artist's impression).jpg

Artist's impression of a Type Ia supernova, as revealed by spectro-polarimetry observations

In 1998, the first evidence for acceleration came from the observation of Type Ia supernovae, which are exploding white dwarf stars that have exceeded their stability limit. Because they all have similar masses, their intrinsic luminosity can be standardized. Repeated imaging of selected areas of the sky is used to discover the supernovae, then follow-up observations give their peak brightness, which is converted into a quantity known as luminosity distance (see distance measures in cosmology for details).^[13] Spectral lines of their light can be used to determine their redshift.

For supernovae at redshift less than around 0.1, or light travel time less than 10 percent of the age of the universe, this gives a nearly linear distance–redshift relation due to Hubble's law. At larger distances, since the expansion rate of the universe has changed over time, the distance-redshift relation deviates from linearity, and this deviation depends on how the expansion rate has changed over time. The full calculation requires computer integration of the Friedmann equation, but a simple derivation can be given as follows: the redshift Шаблон:Mvar directly gives the cosmic scale factor at the time the supernova exploded.

So a supernova with a measured redshift Шаблон:Math implies the universe was Шаблон:Sfrac = Шаблон:Sfrac of its present size when the supernova exploded. In the case of accelerated expansion, <math> \ddot{a} </math> is positive; therefore, <math> \dot{a} </math> was smaller in the past than today. Thus, an accelerating universe took a longer time to expand from 2/3 to 1 times its present size, compared to a non-accelerating universe with constant <math> \dot{a} </math> and the same present-day value of the Hubble constant. This results in a larger light-travel time, larger distance and fainter supernovae, which corresponds to the actual observations. Adam Riess et al. found that "the distances of the high-redshift SNe Ia were, on average, 10% to 15% farther than expected in a low mass density Шаблон:Math universe without a cosmological constant".^[14] This means that the measured high-redshift distances were too large, compared to nearby ones, for a decelerating universe.^[15]

Several researchers have questioned the majority opinion on the acceleration or the assumption of the "cosmological principle" (that the universe is homogeneous and isotropic).^[16] For example, a 2019 paper analyzed the Joint Light-curve Analysis catalog of Type Ia supernovas, containing ten times as many supernova as were used in the 1998 analyses, and concluded that there was little evidence for a "monopole", that is, for an isotropic acceleration in all directions.^[17]^[18] See also the section on Alternate theories below.

Baryon acoustic oscillations

Шаблон:Main In the early universe before recombination and decoupling took place, photons and matter existed in a primordial plasma. Points of higher density in the photon-baryon plasma would contract, being compressed by gravity until the pressure became too large and they expanded again.^[12] This contraction and expansion created vibrations in the plasma analogous to sound waves. Since dark matter only interacts gravitationally, it stayed at the centre of the sound wave, the origin of the original overdensity. When decoupling occurred, approximately 380,000 years after the Big Bang,^[19] photons separated from matter and were able to stream freely through the universe, creating the cosmic microwave background as we know it. This left shells of baryonic matter at a fixed radius from the overdensities of dark matter, a distance known as the sound horizon. As time passed and the universe expanded, it was at these inhomogeneities of matter density where galaxies started to form. So by looking at the distances at which galaxies at different redshifts tend to cluster, it is possible to determine a standard angular diameter distance and use that to compare to the distances predicted by different cosmological models.

Peaks have been found in the correlation function (the probability that two galaxies will be a certain distance apart) at Шаблон:Nowrap,^[11] (where h is the dimensionless Hubble constant) indicating that this is the size of the sound horizon today, and by comparing this to the sound horizon at the time of decoupling (using the CMB), we can confirm the accelerated expansion of the universe.^[20]

Clusters of galaxies

Measuring the mass functions of galaxy clusters, which describe the number density of the clusters above a threshold mass, also provides evidence for dark energy Шаблон:Explain.^[21] By comparing these mass functions at high and low redshifts to those predicted by different cosmological models, values for Шаблон:Mvar and Шаблон:Mvar are obtained which confirm a low matter density and a non-zero amount of dark energy.^[15]

Age of the universe

Шаблон:See also Given a cosmological model with certain values of the cosmological density parameters, it is possible to integrate the Friedmann equations and derive the age of the universe.

By comparing this to actual measured values of the cosmological parameters, we can confirm the validity of a model which is accelerating now, and had a slower expansion in the past.^[15]

Gravitational waves as standard sirens

Recent discoveries of gravitational waves through LIGO and VIRGO^[22]^[23]^[24] not only confirmed Einstein's predictions but also opened a new window into the universe. These gravitational waves can work as sort of standard sirens to measure the expansion rate of the universe. Abbot et al. 2017 measured the Hubble constant value to be approximately 70 kilometres per second per megaparsec.^[22] The amplitudes of the strain 'h' is dependent on the masses of the objects causing waves, distances from observation point and gravitational waves detection frequencies. The associated distance measures are dependent on the cosmological parameters like the Hubble Constant for nearby objects^[22] and will be dependent on other cosmological parameters like the dark energy density, matter density, etc. for distant sources.^[25]^[24]

Explanatory models

Файл:Dark Energy.jpg

The expansion of the Universe accelerating. Time flows from bottom to top

Dark energy

Шаблон:Main The most important property of dark energy is that it has negative pressure (repulsive action) which is distributed relatively homogeneously in space.

where Шаблон:Mvar is the speed of light and Шаблон:Mvar is the energy density. Different theories of dark energy suggest different values of Шаблон:Mvar, with Шаблон:Math for cosmic acceleration (this leads to a positive value of Шаблон:Mvar in the acceleration equation above).

The simplest explanation for dark energy is that it is a cosmological constant or vacuum energy; in this case Шаблон:Math. This leads to the Lambda-CDM model, which has generally been known as the Standard Model of Cosmology from 2003 through the present, since it is the simplest model in good agreement with a variety of recent observations. Riess et al. found that their results from supernova observations favoured expanding models with positive cosmological constant (Шаблон:Math) and a current accelerated expansion (Шаблон:Math).^[14]

Phantom energy

Шаблон:Main Current observations allow the possibility of a cosmological model containing a dark energy component with equation of state Шаблон:Math. This phantom energy density would become infinite in finite time, causing such a huge gravitational repulsion that the universe would lose all structure and end in a Big Rip.^[26] For example, for Шаблон:Math and Шаблон:Math =70 km·s⁻¹·Mpc⁻¹, the time remaining before the universe ends in this Big Rip is 22 billion years.^[27]

Alternative theories

Шаблон:See also There are many alternative explanations for the accelerating universe. Some examples are quintessence, a proposed form of dark energy with a non-constant state equation, whose density decreases with time. A negative mass cosmology does not assume that the mass density of the universe is positive (as is done in supernova observations), and instead finds a negative cosmological constant. Occam's razor also suggests that this is the 'more parsimonious hypothesis'.^[28]^[29] Dark fluid is an alternative explanation for accelerating expansion which attempts to unite dark matter and dark energy into a single framework.^[30] Alternatively, some authors have argued that the accelerated expansion of the universe could be due to a repulsive gravitational interaction of antimatter^[31]^[32]^[33] or a deviation of the gravitational laws from general relativity, such as massive gravity, meaning that gravitons themselves have mass.^[34] The measurement of the speed of gravity with the gravitational wave event GW170817 ruled out many modified gravity theories as alternative explanations to dark energy.^[35]^[36]^[37] Another type of model, the backreaction conjecture,^[38]^[39] was proposed by cosmologist Syksy Räsänen:^[40] the rate of expansion is not homogenous, but Earth is in a region where expansion is faster than the background. Inhomogeneities in the early universe cause the formation of walls and bubbles, where the inside of a bubble has less matter than on average. According to general relativity, space is less curved than on the walls, and thus appears to have more volume and a higher expansion rate. In the denser regions, the expansion is slowed by a higher gravitational attraction. Therefore, the inward collapse of the denser regions looks the same as an accelerating expansion of the bubbles, leading us to conclude that the universe is undergoing an accelerated expansion.^[41] The benefit is that it does not require any new physics such as dark energy. Räsänen does not consider the model likely, but without any falsification, it must remain a possibility. It would require rather large density fluctuations (20%) to work.^[40]

A final possibility is that dark energy is an illusion caused by some bias in measurements. For example, if we are located in an emptier-than-average region of space, the observed cosmic expansion rate could be mistaken for a variation in time, or acceleration.^[42]^[43]^[44]^[45] A different approach uses a cosmological extension of the equivalence principle to show how space might appear to be expanding more rapidly in the voids surrounding our local cluster. While weak, such effects considered cumulatively over billions of years could become significant, creating the illusion of cosmic acceleration, and making it appear as if we live in a Hubble bubble.^[46]^[47]^[48] Yet other possibilities are that the accelerated expansion of the universe is an illusion caused by the relative motion of us to the rest of the universe,^[49]^[50] or that the supernova sample size used wasn't large enough.^[51]^[52]

Theories for the consequences to the universe

Шаблон:See also As the universe expands, the density of radiation and ordinary dark matter declines more quickly than the density of dark energy (see equation of state) and, eventually, dark energy dominates. Specifically, when the scale of the universe doubles, the density of matter is reduced by a factor of 8, but the density of dark energy is nearly unchanged (it is exactly constant if the dark energy is the cosmological constant).^[12]

In models where dark energy is the cosmological constant, the universe will expand exponentially with time in the far future, coming closer and closer to a de Sitter universe. This will eventually lead to all evidence for the Big Bang disappearing, as the cosmic microwave background is redshifted to lower intensities and longer wavelengths. Eventually, its frequency will be low enough that it will be absorbed by the interstellar medium, and so be screened from any observer within the galaxy. This will occur when the universe is less than 50 times its current age, leading to the end of cosmology as we know it as the distant universe turns dark.^[53]

A constantly expanding universe with a non-zero cosmological constant has mass density decreasing over time. In such a scenario, the current understanding is that all matter will ionize and disintegrate into isolated stable particles such as electrons and neutrinos, with all complex structures dissipating away.^[54] This scenario is known as "heat death of the universe" (also known as the Big Freeze).

Alternatives for the ultimate fate of the universe include the Big Rip mentioned above, a Big Bounce, or a Big Crunch.

Notes

Шаблон:Reflist

References