Stars begin in nebulae, vast clouds of dust and gas, where gravity pulls material together.
As the cloud collapses, it fragments into clumps, each potentially birthing a new star.
The core of these clumps heats up, creating a protostar that glows from the heat.
Protostars spin, flattening into disks with materials that may form planets.
Nuclear fusion ignites once the core's temperature exceeds 10 million degrees Celsius.
The star reaches equilibrium, balancing gravity's pull with fusion's outward pressure.
Stars spend most of their life in the stable phase, known as the main sequence.
A star's mass determines its lifespan, color, and eventual end, from white dwarf to supernova.
Massive stars may collapse into black holes or neutron stars after a supernova.
New stars are born from the remnants, continuing the cosmic cycle of star formation.