Gravity and Fusion.
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.
In a stable star, there are primarily two opposing forces at play: gravitational force and radiation pressure. The gravitational force pulls matter inward, while radiation pressure, generated by nuclear fusion reactions in the star's core, pushes outward. These forces balance each other, allowing the star to maintain a stable state throughout most of its life cycle.
The two main forces in a star are gravity and nuclear fusion. Gravity pulls matter inward, compressing it and creating the high pressure and temperature needed for nuclear fusion to occur. Nuclear fusion releases energy as light and heat, which counteracts the force of gravity trying to collapse the star.
The two forces that result in the orbit of a planet are gravitational force, which pulls the planet towards the center of the star it is orbiting, and the planet's tangential velocity, which keeps it moving in a curved path around the star. These two forces are perfectly balanced in a stable orbit.
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.
It is possible but unlikely because the competing gravitational forces from two or more stars are very likely to make it impossible for any planet to settle into a stable orbit.
Hydrostatic and Equilibrium
In a star, the force of gravity is trying to collapse the star inward, while the pressure from nuclear fusion in the core creates an outward force, resisting the gravitational collapse. These two forces are balanced in a stable star, leading to a state of equilibrium.
Religious
Gravity and radiation pressure.
The two competing fundamental forces inside the nucleus of an atom are the strong nuclear force, which holds protons and neutrons together, and the electromagnetic force, which causes positive charges (protons) to repel each other. The strong nuclear force overcomes the electromagnetic force at close distances, keeping the nucleus stable.
Gravity pushes and pulls on a star, balancing it out so it doesn't explode.
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.
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.
leave them be...to unfold as competing forces dicate
The competing of small and large state
In a stable star, there are primarily two opposing forces at play: gravitational force and radiation pressure. The gravitational force pulls matter inward, while radiation pressure, generated by nuclear fusion reactions in the star's core, pushes outward. These forces balance each other, allowing the star to maintain a stable state throughout most of its life cycle.