B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
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and
g
k ( B Superficial deviations from perfect equilibrium, such as peaks, valleys, craters, and other irregularities of the crust which are small in scale compared to the body as a whole, are not considered significant for these definitions.
= -equation, which now reads.
of the cluster and is given by, where This qualification typically means that the object is ).
To put it simply, hydrostatic equilibrium is the balance struck between pressure-gradient force and gravity. ( ) An example of this is Beta Lyrae. {\displaystyle r^{2}/\rho _{B}(r)} A rotating star in hydrostatic equilibrium is an oblate spheroid up to a certain (critical) angular velocity. Hydrostatic equilibrium happens when the pull of gravity is balanced by a pressure gradient which creates a pressure-gradient force in the other direction.
θ − {\displaystyle \sigma _{D}^{2}} Using the ideal gas law , the index i runs for the coordinates r and is Boltzmann's constant and
σ (That is, the body as a whole can be considered to be in hydrostatic equilibrium even if the crust is not.
t M(r) is a foliation of spheres weighted by the mass density ρ(r), with the largest sphere having radius r: Per standard procedure in taking the nonrelativistic limit, we let c→∞, so that the factor. Dividing by A. Ptop − Pbottom is a change in pressure, and h is the height of the volume element—a change in the distance above the ground. Density changes with pressure, and gravity changes with height, so the equation would be: Note finally that this last equation can be derived by solving the three-dimensional Navier–Stokes equations for the equilibrium situation where, Then the only non-trivial equation is the z Thus, hydrostatic balance can be regarded as a particularly simple equilibrium solution of the Navier–Stokes equations. n. A state of balance by which the This occurs when external forces such as gravity are balanced by a pressure-gradient. {\displaystyle r} r is a characteristic mass of the baryonic gas particles) and rearranging, we arrive at, Multiplying by X {\displaystyle {\mathcal {L}}_{X}=\Lambda (T_{B})\rho _{B}^{2}} Hydrostatic equilibrium happens when the pull of gravity is balanced by a pressure gradient which creates a pressure-gradient force in the other direction. B B = B In addition to the Sun, there are a dozen or so equilibrium objects confirmed to exist in the Solar System, with others possible. Hydrostatic Equilibrium For the majority of the life of a star, the gravitational force (due to the mass of the star) and the gas pressure (due to energy generation in the core of the star) balance, and the star is said to be in ‘ hydrostatic equilibrium ’. Hydrostatic equilibrium is the distinguishing criterion between dwarf planets and small Solar System bodies, and has other roles in astrophysics and planetary geology. {\displaystyle dP=-\rho gdr} Finally, the weight of the volume element causes a force downwards. Only baryonic matter (or, rather, the collisions thereof) emits X-ray radiation.
Thus, there cannot be two different hydrostatic pressures at a certain depth. r This force balance is called a hydrostatic equilibrium. This page was last edited on 26 September 2017, at 12:56. B m − It flattens the surface of undisturbed liquids. 2 p ) ρ {\displaystyle z} satisfies the non-linear differential equation, With perfect X-ray and distance data, we could calculate the baryon density at each point in the cluster and thus the dark matter density. r Under planetary conditions, "solid" rock and ice are actually fluid, and will lapse into hydrostatic equilibrium if the body is massive or warm enough. (
ρ
B {\displaystyle \rho _{B}(0)/\rho _{M}(0)} ( d Values for the ratio range from .11 to .14 for various surveys.[6]. the proper distance to the cluster. is the angular width of the cluster and
However, Mimas is not actually in hydrostatic equilibrium for its current rotation. https://en.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=979865432, Articles needing additional references from May 2010, All articles needing additional references, Creative Commons Attribution-ShareAlike License, This page was last edited on 23 September 2020, at 06:54. =
However, in the cases of moons in synchronous orbit, nearly unidirectional tidal forces create a scalene ellipsoid. being the proper distance to the center of the cluster. The force of gravity balances this out, keeping the atmosphere bound to Earth and maintaining pressure differences with altitude. T The smallest body confirmed to be in hydrostatic equilibrium is the dwarf planet Ceres, which is icy, at 945 km, whereas the largest body known body to have a noticeable deviation from hydrostatic equilibrium is Iapetus (moon) being made of mostly permeable ice and almost no rock [7]. {\displaystyle m_{B}} d Λ Strobel, Nick. ) The hydrostatic equilibrium pertains to hydrostatics and the principles of equilibrium of fluids. s Therefore, in the nonrelativistic limit the Tolman–Oppenheimer–Volkoff equation reduces to Newton's hydrostatic equilibrium: (we have made the trivial notation change h=r and have used f(Ρ,ρ)=0 to express ρ in terms of P). If the density is ρ, the volume is V and g the standard gravity, then: The volume of this cuboid is equal to the area of the top or bottom, times the height — the formula for finding the volume of a cube. T Icy objects were previously believed to need less mass to attain hydrostatic equilibrium than rocky objects. If the star has a massive nearby companion object then tidal forces come into play as well, distorting the star into a scalene shape when rotation alone would make it a spheroid. The balance of these two forces is known as the hydrostatic balance. A star with an angular velocity above the critical angular velocity becomes a Jacobi (scalene) ellipsoid, and at still faster rotation it is no longer ellipsoidal but piriform or oviform, with yet other shapes beyond that, though shapes beyond scalene are not stable.[5].
This means the sum of the forces in a given direction must be opposed by an equal sum of forces in the opposite direction. r ρ of the dark matter, which is given by, The central density ratio ρ yields, If we make the assumption that cold dark matter particles have an isotropic velocity distribution, then the same derivation applies to these particles, and their density An extreme example of this phenomenon is the star Vega, which has a rotation period of 12.5 hours. Often the equilibrium shape is an oblate spheroid, as is the case with Earth. In any given layer of a star, there is a hydrostatic equilibrium between the outward thermal pressure from below and the weight of the material above pressing inward. This equilibrium is strictly applicable when an ideal fluid is in steady horizontal laminar flow, and when any fluid is at rest or in vertical motion at constant speed. From Simple English Wikipedia, the free encyclopedia, https://simple.wikipedia.org/w/index.php?title=Hydrostatic_equilibrium&oldid=5695854, Creative Commons Attribution/Share-Alike License. θ z By balancing these forces, the total force on the fluid is. {\displaystyle z} 2 ( Hydrostatic-equilibrium definitions A state of balance by which the internal pressure of a gaseous body, such as a star, exactly balances its gravitational pressure. where
The fluid can be split into a large number of cuboid volume elements; by considering a single element, the action of the fluid can be derived.
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