hydrostatic
Dynamic equilibrium.
The balance of forces that keeps a star from collapsing is called hydrostatic equilibrium. This equilibrium occurs when the outward pressure generated by nuclear fusion in the star's core balances the inward gravitational force trying to collapse the star. If these forces are not balanced, the star may either contract under gravity or expand until a new equilibrium is reached.
The two competing forces in a star are gravity, which tries to collapse the star under its own weight, and nuclear fusion, which generates energy and causes the star to expand outward. These forces balance each other to maintain a stable, long-lived star.
A star is primarily affected by two opposing forces: gravitational force and radiation pressure. Gravitational force pulls the star's mass inward, trying to collapse it, while radiation pressure, generated by nuclear fusion reactions in the star's core, pushes outward. The balance between these forces determines the star's stability and lifecycle. If the balance is disrupted, it can lead to various evolutionary stages, including expansion into a red giant or collapse into a supernova.
hydrostatic
Dynamic equilibrium.
The balance of forces that keep a star from collapsing is called hydrostatic equilibrium. This equilibrium is maintained between the inward force of gravity and the outward force generated by gas pressure within the star.
The balance of forces that keeps a star from collapsing is called hydrostatic equilibrium. This equilibrium occurs when the outward pressure generated by nuclear fusion in the star's core balances the inward gravitational force trying to collapse the star. If these forces are not balanced, the star may either contract under gravity or expand until a new equilibrium is reached.
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The two competing forces in a star are gravity, which tries to collapse the star under its own weight, and nuclear fusion, which generates energy and causes the star to expand outward. These forces balance each other to maintain a stable, long-lived star.
Star balance, often referred to in the context of astronomy, pertains to the equilibrium between the gravitational forces pulling inward on a star and the outward pressure generated by nuclear fusion in its core. This balance is crucial for a star's stability and longevity, allowing it to maintain its size and shape over time. If the balance is disrupted, either by the depletion of nuclear fuel or external forces, the star may undergo changes such as expansion into a red giant or collapse into a different stellar state.
A star is primarily affected by two opposing forces: gravitational force and radiation pressure. Gravitational force pulls the star's mass inward, trying to collapse it, while radiation pressure, generated by nuclear fusion reactions in the star's core, pushes outward. The balance between these forces determines the star's stability and lifecycle. If the balance is disrupted, it can lead to various evolutionary stages, including expansion into a red giant or collapse into a supernova.
Equilibrium.
Inside a star, there are two opposing forces at play: gravity tries to pull the stellar material inward, compressing it, while the force of nuclear fusion in the star's core pushes outward, generating energy and counteracting gravity to maintain the star's stability. These forces must balance each other for the star to remain in a state of equilibrium.
The outward forces on a star, primarily generated by nuclear fusion in its core, counterbalance the inward gravitational forces trying to collapse the star. The balance between these forces determines the star's size and stability; if the outward pressure increases (e.g., from increased fusion due to higher core temperatures), the star expands. Conversely, if the inward gravitational force becomes stronger (e.g., from a depletion of nuclear fuel), the star contracts. Thus, the interplay of these forces is crucial in defining a star's size and evolutionary state.
The two opposing forces are gravity, pulling the star in and the outward force from the ongoing nuclear fusion reactions. As the star approaches the end of it's life, changes in the reactions occur, which cause the forces to balance out in different ways, changing the size of the star.