Here is a brief 'potted' history of how the Universe was developed from the so-called 'Big Bang' according to most accepted current theories.
By studying the origins of the Universe, ESA Science can help provide answers about how the Universe will end - whether it will expand forever or collapse in on itself, thousands of millions of years from now.
During this period, a very quick 'inflation' process takes place, and in an infinitesimal fraction of a second the cosmos becomes extremely large. All the matter and energy, concentrated in a region smaller than a coin, begins to expand at a very rapid rate. Once inflation is over, the Universe continues
the expansion at a much slower pace. As it expands, it also cools.
When it is at a temperature of 1000 GeV (about 10 million million degrees),
the forces of nature assume their present properties (such as gravity,
electromagnetism, and the strong and weak forces) and the 'quarks', the
elementary particles that are the building blocks of matter, wander freely.
This is the most accepted theory. For many scientists, this period is
'speculative'. There are no observations to confirm or disprove the theories.
A millionth of a second after the Big Bang
The Universe is roughly the size of our Solar System today, and the
temperature drops to 1 GeV (10 thousand million degrees). It is cool enough
for quarks to combine and make the particles in the atomic nucleus, protons
and neutrons. These particles are called hadrons, so this period is often
called the 'quark-hadron transition'.
From one second to three minutes after the Big
Bang
At one second, the Universe grows to about a thousand times the size of our
Solar System today and the temperature drops to 1 MeV, equivalent to 10 000
million degrees. Neutrons and protons combine to form the first nuclei: first
deuterium, then helium and other elements. This is called 'primordial
nucleosynthesis' and it lasts several minutes.
From three minutes to 300 000 years after the Big Bang
The Universe keeps expanding. It is too hot yet for electrons to be captured by the atomic nuclei. Electrons wander freely and are therefore able to interact with the photons (light 'particles') as a result, light is trapped and cannot propagate more than a very short distance before encountering an electron. Therefore the Universe is opaque.
But about 300 000 years later, the Universe has cooled enough (to some 3000°C) to allow
protons to capture electrons, and form neutral hydrogen atoms (in a phenomenon
called 'recombination' or 'decoupling').
The Universe is about 1000 times smaller than its present size. Light can
propagate without hindrance: the Universe suddenly becomes transparent. The
Cosmic Microwave Background radiation that we detect today is that 'first
light'.
Soon after recombination (The Dark Age)
The matter is now cool and luminous. Initial 'clots' of matter start to grow
by gravitational attraction. This process is still unknown, but involves both
the matter that we can see ('baryons') and so-called 'Dark Matter'.
The first stars form when the lumps of matter grow to about 10 million times
the mass of our Sun, when the Universe is about one thirtieth of its current
size. The lumps of matter (containing stars) coalesce to form galaxies and
clusters of galaxies.
The first stars produce lots of ultraviolet radiation which ionises most of
the neutral hydrogen (that is, liberating the electrons from the protons),
thereby ending the so-called ‘Dark age’ of the Universe.
1000 million years after the Big Bang
The Universe is a fifth of its present size. Observations indicate that there
are already fully formed galaxies. Therefore galaxy formation must have
started much earlier. When the Universe is half its present size, the nuclear
reactions inside the stars have already produced most of the chemical elements
that are needed to make Earth-like planets.
10 000 million years after the Big Bang
About 5000 million years ago, our Sun was formed from the collapse of a cloud
of dust and gas, producing a very average- looking star.
The remnants from the formation of the Sun, swirling in a disk around our
infant star, gradually coalesce into the planets that form part of our Solar
System. 4500 million years ago, the Earth and the inner planets form with
rocky mantles and molten interiors, while more distant planets become gaseous
giants.
Around 700 million years later, life begins on Earth. The oldest fossils of
living organisms (bacteria) found on Earth are 3800 million years old.
ESA
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