From the early universe to human history.

The observable universe begins in an extremely hot, dense state.

A very early phase of rapid expansion explains large-scale cosmic uniformity.

Quarks combine into protons and neutrons as the early plasma cools.

Light atomic nuclei, especially hydrogen and helium, form in the early universe.

Neutral atoms form and light begins traveling freely through space.

Gas collapses inside early dark-matter structures and ignites the first stars.

Early galaxies assemble within growing cosmic structure.

Stars and stellar explosions forge heavier elements needed for planets and life.

Dark energy becomes dominant and the expansion of the universe accelerates.

The Sun and surrounding planetary disk form from interstellar gas and dust.

Planet Earth forms from material orbiting the young Sun.

A giant impact likely produces the debris that becomes the Moon.

The first known organisms appear on Earth.

The human lineage separates from the lineage leading to chimpanzees.

The genus Homo evolves in Africa and early stone tools appear.

Early humans spread from Africa into Eurasia as several human species coexist.

Neanderthals evolve in Europe and western Asia.

Homo sapiens evolves in Africa.

Symbolic language, shared myths, and flexible cooperation become central to Sapiens history.

Humans reach Australia and begin major ecological transformations.

Neanderthals disappear, leaving traces in many modern human genomes.

Domestication transforms settlement, labor, disease, hierarchy, and social organization.

Large-scale political, economic, and symbolic systems become increasingly stable.

Modern science, global exploration, capitalism, and technological power reshape human history.

Energy, machines, markets, states, and mass production transform human life and planetary ecology.

Humanity becomes a planetary force while future evolution may involve biotechnology and AI.

The aging Sun expands dramatically as it exhausts hydrogen in its core.

The Sun burns helium and passes through late stellar evolutionary stages.

The Sun sheds its outer layers and leaves a dense stellar remnant.

Accelerating expansion carries most galaxies beyond observable reach.

Star formation dwindles as galaxies run out of usable gas.

Over immense timescales, orbital systems decay around stellar remnants.

Close gravitational encounters eject many objects into intergalactic space.

If protons decay, ordinary matter slowly dissolves into lighter particles.

Hawking radiation causes smaller astrophysical black holes to vanish.

The most massive black holes eventually evaporate through Hawking radiation.

Dark energy could tear apart galaxies, stars, planets, and matter itself.

Cosmic expansion could reverse and collapse the universe into a hot dense state.

The universe could pass through repeated phases of contraction and expansion.

A lower-energy vacuum state could spread through space and rewrite physical conditions.

Rare thermal fluctuations could produce isolated observer-like states in a vast future.

Our observable universe could be one region within a much larger cosmic ensemble.