◄ AGE of UNIVERSE ► TIME in perspective ⏱️

Imagine if 1 second were a 1mm3 How big would the rest of the time scales be? Time for a neuron in human brain to fire one impulse and return to rest Lifetime of a muon Light travels 30 cm (12 in) Mean lifetime of a bottom quark Lifetime of a tauon Shortest laser pulse The smallest time interval uncertainty in direct measurements was October 2020 Mean lifetime of a Higgs Boson A Planck time unit is the time required for light to travel a distance of 1 Planck length in a vacuum The last cold episode of the last glacial period ended about 10,000 years ago The earliest fossil evidence of early modern humans appears in Africa around 300,000 years ago Quaternary is the current and most recent of the three periods of the Cenozoic Era in the geologic time scale of the International Commission on Stratigraphy (ICS). The Cretaceous (along with the Mesozoic) ended with the Cretaceous – Paleogene extinction event.

The Mesozoic Era lasted from about 252 to 66 million years ago. It is also called the Age of Reptiles and the Age of Conifers. The Phanerozoic Eon is the current geologic eon in the geologic time scale, and the one during which abundant animal and plant life has existed.

It covers 541 million years to the present. The Proterozoic is a geological eon spanning the time from the appearance of oxygen in Earth's atmosphere to just before the proliferation of complex life on the Earth. From 2500 to 541 million years ago.

This age may represent the age of the Earth's accretion, or core formation, or of the material from which the Earth formed. The Sun was formed from the gravitational collapse of matter within a region of a large molecular cloud. In physical cosmology, the age of the universe is the time elapsed since the Big Bang.

The end of the Universe in the Big Rip scenario, assuming a model of dark energy with w = −1. 5. The estimate lifetime of low-mass stars (red dwarfs) This marks the transition from the Stelliferous Era to the Degenerate Era.

Estimated time until stellar close encounters detach all planets in star systems (including the Solar System) from their orbits. By this point, the Sun will have cooled to 5 K The radioactive half-life of bismuth-209 by alpha decay, one of the slowest-observed radioactive decay processes. Estimated time until the Earth collides with the black dwarf Sun due to the decay of its orbit via emission of gravitational radiation, if the Earth is not ejected from its orbit by a stellar encounter or engulfed by the Sun during its red giant phase.

Around this timescale most stellar remnants and other objects are ejected from the remains of their galactic cluster. Estimated time for all nucleons in the observable universe to decay, if the hypothesized proton half-life takes its smallest possible value (8. 2×10^33 years).

Estimated time for all nucleons in the observable universe to decay, if the hypothesized proton half-life takes the largest possible value, 10^41 years. By this time, if protons do decay, the Black Hole Era begins. Estimated time until a black hole of 1 solar mass decays into subatomic particles by Hawking radiation.

Estimated time until the supermassive black hole of TON 618, with a mass of 66 billion solar masses, dissipates by the emission of Hawking radiation, assuming zero angular momentum (that it does not rotate). Estimated time until a supermassive black hole with a mass of 20 trillion solar masses decays by Hawking radiation. This marks the end of the Black Hole Era.

Beyond this time, if protons do decay, the Universe enters the Dark Era. Estimated high time for all nucleons in the observable universe to decay, if they do not via the above process, through any one of many different mechanisms allowed in modern particle physics on time scales of 10^46 to 10^200 years. Assuming protons do not decay, the estimated time until all baryonic matter in stellar-mass objects has either fused together via muon-catalyzed fusion to form iron-56 or decayed from a higher mass element into iron-56 to form an iron star.

Conservative estimate for the time until all iron stars collapse via quantum tunnelling into black holes, assuming no proton decay or virtual black holes. Estimated time for a Boltzmann brain to appear in the vacuum via a spontaneous entropy decrease. High estimate for the time until all iron stars collapse into black holes, assuming no proton decay or virtual black holes, which then (on these timescales) instantaneously evaporate into subatomic particles.

Highest estimate for the time it takes for the universe to reach its final energy state, even in the presence of a false vacuum. Around this vast timeframe, quantum tunnelling in any isolated patch of the now-empty universe could generate new inflationary events, resulting in new Big Bangs giving birth to new universes.