
Process by which gravitational collapse of matter forms galaxies and larger structures.Cosmic structure formation is the process by which the initially nearly uniform matter in the early universe evolved into the rich hierarchy of structures we observe today: stars, galaxies, galaxy clusters, and the vast cosmic web of filaments and voids. It begins with tiny density fluctuations imprinted in the primordial plasma, which are amplified by gravity over billions of years. Dark matter plays a crucial role, providing the gravitational scaffolding that attracts ordinary matter, which then cools and collapses to form luminous objects.
The modern theory was developed in the 1960s and 1970s, with key contributions from Yakov Zeldovich, Jim Peebles, and others, building on earlier ideas from the 1940s by George Gamow and collaborators.
The mechanism is gravitational instability. Regions with slightly higher density exert a stronger gravitational pull, attracting surrounding matter and becoming even denser. This runaway growth continues until pressure, radiation, or angular momentum halts collapse at various scales. Dark matter, which interacts only gravitationally, collapses into halos first; ordinary gas then falls into these halos, shocks, cools, and forms stars and galaxies. On large scales, the distribution of matter is shaped by the expansion of the universe, producing a web-like pattern of filaments and nodes.
Cosmological simulations of structure formation are used to interpret galaxy surveys and cosmic microwave background observations, constraining the nature of dark matter and dark energy.
The largest structures in the universe, such as galaxy filaments, are so massive that they are still collapsing today, even though the universe's overall expansion is accelerating.
















