宇宙演化历史

Time: <10^−43 s

Temperature: >10^32 K

Energy: >10^19 Gev

Description: The Planck scale is the scale beyond which current physical theories do not have predictive value. The Planck epoch is the time during which physics is assumed to have been dominated by quantum effects of gravity.

Time: <10^−36 s

Energy: >10^16 Gev

Description: The three forces of the Standard Model are unified (assuming that nature is described by a Grand unification theory).

Time: <10^−32 s

Temperature: 10^28K--10^22k

Energy: >10^19 Gev

Description: Cosmic inflation expands space by a factor of the order of 1026 over a time of the order of 10−33 to 10−32 seconds. The universe is supercooled from about 1027 down to 1022 kelvins.[3] The Strong Nuclear Force becomes distinct from the Electroweak Force.

Time: 10^−12s--10^-6s

Temperature: >10^12 K

Energy: 100Mev

Description: The forces of the Standard Model have separated, but energies are too high for quarks to coalesce into hadrons, instead forming a quark-gluon plasma. These are the highest energies directly observable in experiment in the Large Hadron Collider.

Time: 10^−6s--1s

Temperature: >10^10 K

Description: Quarks are bound into hadrons. A slight matter-antimatter-asymmetry from the earlier phases (baryon asymmetry) results in an elimination of anti-hadrons.

Time: 1s

Temperature: 10^10 K

Energy: 1Mev

Description: Neutrinos cease interacting with baryonic matter. The spherical volume of space which will become the Observable universe is approximately 10 light-years in radius at this time.

Time: 1s--10s

Temperature: >10^10 K

Description: Leptons and anti-leptons remain in thermal equilibrium.

Time: 10s--10^3s

Temperature: 10^9K--10^7K

Energy: 100Kev--1Kev

Description: Protons and neutrons are bound into primordial atomic nuclei, hydrogen and helium-4. Small amounts of deuterium, helium-3, and lithium-7 are also synthesized.

Time: 10s--1.2*10^13s

Temperature: 10^K--4000K

Description: The universe consists of a plasma of nuclei, electrons and photons; temperatures remain too high for the binding of electrons to nuclei.

Time: 380 ka

Redshift: 1100

Temperature: 4000K

Description: Electrons and atomic nuclei first become bound to form neutral atoms. Photons are no longer in thermal equilibrium with matter and the Universe first becomes transparent. Recombination lasts for about 100 ka, during which Universe is becoming more and more transparent to photons. The photons of the cosmic microwave background radiation originate at this time. The spherical volume of space which will become the observable universe is 42 million light-years in radius at this time.

Time: 380ka...150Ma

Redshift: 1100--20

Temperature: 4000K--60K

Description: The time between recombination and the formation of the first stars. During this time, the only source of photons was hydrogen emitting radio waves at hydrogen line. Freely propagating CMB photons quickly (within ~500 ka) red-shifted to infrared, and Universe was devoid of visible light.

Time: 150Ma--1Ga

Redshift: 20--6

Temperature: 60K-19K

Description: The most distant astronomical objects observable with telescopes date to this period; as of 2016, the most remote galaxy observed is GN-z11, at a redshift of 11.09. The earliest "modern" Population III stars are formed in this period.

Time: 47Ka--10Ga

Redshift: 3600--0.4

Temperature: 10^4K--4K

Description: During this time, the energy density of matter dominates both radiation density and dark energy, resulting in a decelerated metric expansion of space.

Time: 1Ga--10Ga

Redshift: 6--0.4

Temperature: 19K-4K

Description: Galaxies coalesce into "proto-clusters" from about 1 Ga (z = 6) and into Galaxy clusters beginning at 3 Gy (z = 2.1), and into superclusters from about 5 Gy (z = 1.2), see list of galaxy groups and clusters, list of superclusters.

Time: >10Ga

Redshift: <0.4

Temperature: <4K

Description: Matter density falls below dark energy density (vacuum energy), and expansion of space begins to accelerate. This time happens to correspond roughly to the time of the formation of the Solar System and the evolutionary history of life.

Time: 150Ma--100Ga

Redshift: 20---0.99

Temperature: 60K-0.003K

Description: The time between the first formation of Population III stars until the cessation of star formation, leaving all stars in the form of degenerate remnants.

Time: 13.8Ga

Redshift: 0

Temperature: 2.7K

Description: Farthest observable photons at this moment are CMB photons. They arrive from a sphere with the radius of 46 billion light-years. The spherical volume inside it is commonly referred to as Observable universe.

Time: >100Ga

Redshift: <-0.99

Temperature: 0.1K

Description: The Stelliferous Era will end as stars eventually die and fewer are born to replace them, leading to a darkening universe. Various theories suggest a number of subsequent possibilities. Assuming proton decay, matter may eventually evaporate into a Dark Era (heat death). Alternatively the universe may collapse in a Big Crunch. Alternative suggestions include a false vacuum catastrophe or a Big Rip as possible ends to the universe.