The Big Bang theory explains the beginning of the universe’s expansion, what happened during and after that moment. According to the standard theory, this theory states that the universe began from an initial point (singularity: zone of infinite density), which has expanded over billions of years ( around 13.7 billion years ago) to form the universe as we now know it. In 1922 Alexander Friedmann of Russia is credited with developing a dynamic equation for the expanding universe. We are taught that the universe began as a singularity – an infinitely small and infinitely dense point. Once the singularity was created, it began to expand through a process called inflation.
After that, it expanded and cooled, going from very small and very hot, to the size and temperature of our current universe. Astronomers observed the relationship between the number density of distant radio sources and quasars( quasars are intense sources of X-rays as well as visible light) and the energy received from them per unit area per unit time have discovered new evidence about the rate at which the universe is expanding. The research shows a slow enough expansion to explain the ages of the oldest globular star clusters, as long as the universe has a low density.
Stockton observed faint galaxies near in the sky to bright quasars at moderate redshifts. The redshift of an object is the amount by which the spectral lines in the source are shifted to the red.
Quasars are associated with galaxies that have the same redshift as the quasar and have just the brightness expected if the quasars are at their cosmological distances. The redshift caused by the expansion is often confused with the redshift generated by the Doppler effect.
The Doppler redshift and the cosmological redshift are governed by two distinct formulas. The first comes from special relativity; the second comes from general relativity. If the redshift is interpreted as a Doppler shift, the recessional velocity of the object can be calculated. In an expanding Universe, distant objects are redshifted, with for small distances. This law was discovered by Hubble and is known as the Hubble constant.
At large distances, the conversion between cosmological redshift and distance is much more complicated, depending on the geometry of spacetime and the expansion history of the Universe.
Big Bang Theory – Evidence for the Theory
The universe had a beginning. Galaxies appear to be moving away from us at speeds proportional to their distance. This is called “Hubble’s Law,” named after Edwin Hubble (1889-1953) who discovered this phenomenon in 1929. This observation supports the expansion of the universe.
In 1965, while tuning a small, yet very powerful and highly sensitive horn antenna for conducting radio astronomy experiments, Arno Penzias and Robert Wilson noted a constant low level noise disrupting their reception. They discovered a 2.725 degree Kelvin (-454.765 degree Fahrenheit, -270.425 degree Celsius) Cosmic Microwave Background radiation (CMB).
The Universe’s light-element abundance is another important criterion by which the Big Bang hypothesis is verified. Light elements (namely deuterium, helium, and lithium) were produced in the first few minutes of the Big Bang, while elements heavier than helium are thought to have their origins in the interiors of stars which formed much later in the history of the Universe. It is observed that upwards of 25% the Universe’s total matter consists of helium. The Big Bang Nucleosynthesis theory predicts that 25% the mass of the Universe consists of Helium. It also predicts about 0.01% deuterium, and even smaller quantities of lithium. The important point is that the prediction depends critically on the density of baryons (ie neutrons and protons) at the time of nucleosynthesis. Measurements of the baryon density in the Universe using the cosmic microwave background spectrum and primordial nucleosynthesis constrain the baryon density to a value less than 0,05.
There are a number of free parameters in the Big Bang model must be fixed by observations of our universe: the geometry of the universe (open, flat or closed); the present expansion rate (the Hubble constant); the overall course of expansion, which is determined by the fractional density of the different types of matter in the universe.