In order for a star to form, gas from an interstellar cloud has to be gravitationally attracted toward a center of gravity. The strength of the gravitational attraction depends upon the amount of mass (and its density, which of course increases as the star is in the process of being formed). It takes a certain amount of mass to create a star, otherwise all you will have is an interstellar gas cloud.
The maximum mass of a star is around 150 times the mass of our sun. Stars more massive than this are unable to achieve hydrostatic equilibrium and will undergo rapid mass loss through stellar winds or explode in supernova events.
Hydrostatic equilibrium is the balance between the inward force of gravity and the outward pressure gradient in a fluid, like in a star or planet. This equilibrium prevents further collapse or expansion by ensuring that the pressure within the fluid supports the weight of the overlying material. In stars, this balance between gravity and pressure helps maintain their stable size and shape.
binary star systems
Massive stars get hotter, burn their fuel faster, and therefore live shorter.With respect to their "death": Stars of "normal" mass become white dwarves; more massive stars become neutron stars, and the most massive stars become black holes.
Yes, a planet's mass can be determined by observing its transit across a star. By measuring the dip in the star's brightness during the transit, astronomers can calculate the size of the planet and its gravitational effect on the star, which provides information on the planet's mass.
Hydrostatic and Equilibrium
Hydrostatic equilibrium occurs when compression due to gravity is balanced by a pressure gradient which creates a pressure gradient force in the opposite direction. The balance of these two forces is known as the hydrostatic balance.
achieved through the process of hydrostatic equilibrium. This balance helps maintain the stability and structure of the star by ensuring that the inward gravitational force is counteracted by the outward pressure force generated by the internal energy of the star.
The four fundamental laws of stellar structure are: 1) Hydrostatic equilibrium - balance between pressure and gravity within the star, 2) Energy transport - mechanism by which energy is transported from the core to the surface, 3) Energy generation - fusion reactions that produce energy within the core of the star, and 4) Mass continuity - conservation of mass within the star.
The maximum mass of a star is around 150 times the mass of our sun. Stars more massive than this are unable to achieve hydrostatic equilibrium and will undergo rapid mass loss through stellar winds or explode in supernova events.
The properties of a main-sequence star can be understood by considering the various physical processes occurring in the interior. First is the hydrostatic balance, also called hydrostatic equilibrium. This determines the density structure of the star as the internal pressure gradient balances against the force of gravity.
hydrostatic 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.
Hydrostatic equilibrium [See related question]
Any star is going to be in hydrostatic equilibrium, so "shape" is not really a factor.
Hydrostatic equilibrium is the balance between the inward force of gravity and the outward pressure gradient in a fluid, like in a star or planet. This equilibrium prevents further collapse or expansion by ensuring that the pressure within the fluid supports the weight of the overlying material. In stars, this balance between gravity and pressure helps maintain their stable size and shape.
They weigh each star with a scale