After a nebula contracts and its temperature increases, the gravitational forces cause the gas and dust to clump together, leading to the formation of a protostar. As the protostar continues to accumulate mass, its core temperature rises further, eventually reaching the point where nuclear fusion ignites. This marks the birth of a new star, which then begins to shine and can eventually evolve into different types of stars depending on its mass. The surrounding material may form a protoplanetary disk, potentially leading to the creation of planets.
As a nebula contracts and its temperature increases to millions of Kelvin, it initiates nuclear fusion processes, primarily converting hydrogen into helium. This marks the birth of a new star, as the immense pressure and heat overcome gravitational forces, leading to the ignition of fusion reactions in the core. The newly formed star enters the main sequence phase of its life cycle, where it will spend the majority of its existence. Over time, the star will evolve and eventually exhaust its nuclear fuel, leading to further stages in its life, such as becoming a red giant or supernova, depending on its mass.
When the pressure and temperature of a nebula increase, it can lead to the formation of protostars. As gravity causes the nebula to contract and heat up, eventually nuclear fusion can begin at the core of the protostar, leading to the formation of a new star.
A nebula begins to contract due to gravitational forces overcoming the pressure from its internal gas and dust. As the material within the nebula begins to clump together, the gravitational attraction increases, leading to further contraction. This process can be triggered by external factors such as shock waves from nearby supernovae or collisions with other clouds, which can compress the nebula and initiate star formation. As the nebula contracts, it can lead to the formation of stars and planetary systems.
During the third stage, a star expands and becomes a red giant as it runs out of hydrogen fuel in its core. The core contracts and heats up, causing the outer layers to expand. Eventually, the star will shed its outer layers to form a planetary nebula, leaving behind a dense core called a white dwarf.
Under the influence of its own gravity, a nebula contracts, spinning faster and faster as it does. This is called is called conservation of angular momentum. Because of the spinning, the nebula flattens out to form a disk. As it continues to flatten and spin, it becomes denser and hotter, particularly in the center. This dense, hot center eventually forms into a star, the sun. The swirling mass destined to become a solar system is usually referred to as the solar nebula.
A supernova occurs.
After a nebula contracts and its temperature increases to 10 million K, it can start nuclear fusion in its core, becoming a protostar. The increase in temperature and pressure triggers the fusion of hydrogen atoms into helium atoms, releasing energy in the form of light and heat. The protostar will continue to evolve and eventually become a full-fledged star.
A supernova occurs.
If there is sufficient mass and material it will contract due to gravity it may then become a star. The type of star depends on how much mass was present
When the pressure and temperature of a nebula increase, it can lead to the formation of protostars. As gravity causes the nebula to contract and heat up, eventually nuclear fusion can begin at the core of the protostar, leading to the formation of a new star.
A nebula.
A nebula begins to contract due to gravitational forces overcoming the pressure from its internal gas and dust. As the material within the nebula begins to clump together, the gravitational attraction increases, leading to further contraction. This process can be triggered by external factors such as shock waves from nearby supernovae or collisions with other clouds, which can compress the nebula and initiate star formation. As the nebula contracts, it can lead to the formation of stars and planetary systems.
During the third stage, a star expands and becomes a red giant as it runs out of hydrogen fuel in its core. The core contracts and heats up, causing the outer layers to expand. Eventually, the star will shed its outer layers to form a planetary nebula, leaving behind a dense core called a white dwarf.
Under the influence of its own gravity, a nebula contracts, spinning faster and faster as it does. This is called is called conservation of angular momentum. Because of the spinning, the nebula flattens out to form a disk. As it continues to flatten and spin, it becomes denser and hotter, particularly in the center. This dense, hot center eventually forms into a star, the sun. The swirling mass destined to become a solar system is usually referred to as the solar nebula.
A supernova occurs.
Gravity is the force that holds matter in a nebula together. As the nebula contracts under its own gravity, the particles begin to clump together, eventually forming stars and other celestial bodies.
it contracts together to were it can't hold any more.