Newtonian hydrostatic equilibrium equation

Target entity: Newtonian hydrostatic equilibrium equation
Context triple: [Tolman–Oppenheimer–Volkoff equation, generalizationOf, Newtonian hydrostatic equilibrium equation]

• A. Maclaurin spheroid
  A Maclaurin spheroid is an oblate, rotationally symmetric ellipsoidal figure used in astrophysics and geophysics to model the equilibrium shape of a uniformly rotating, self-gravitating fluid body.
• B. Roche–Riemann ellipsoids
  Roche–Riemann ellipsoids are a family of rotating, self-gravitating fluid equilibrium figures in astrophysics and celestial mechanics that generalize classical ellipsoidal solutions like the Jacobi ellipsoid.
• C. Tolman–Oppenheimer–Volkoff equation
  The Tolman–Oppenheimer–Volkoff equation is the general relativistic equation of hydrostatic equilibrium that describes the internal structure and pressure balance of spherically symmetric, non-rotating stars such as neutron stars.
• D. Chandrasekhar’s theory of ellipsoidal figures of equilibrium
  Chandrasekhar’s theory of ellipsoidal figures of equilibrium is a foundational mathematical framework in astrophysics that analyzes the shapes, stability, and rotational properties of self-gravitating fluid masses modeled as ellipsoids.
• E. Bonnor–Ebert mass
  The Bonnor–Ebert mass is the maximum mass a pressure-confined, self-gravitating gas sphere can have while remaining in stable hydrostatic equilibrium before collapsing under its own gravity.
• F. None of above. chosen
• G. Unsure - the case is ambiguous/there is not enough information to decide.

Target entity: Newtonian hydrostatic equilibrium equation
Target entity description: The Newtonian hydrostatic equilibrium equation is the classical relation in stellar structure that balances the inward pull of gravity with the outward pressure gradient in a spherically symmetric, non-relativistic fluid.

• A. Maclaurin spheroid
  A Maclaurin spheroid is an oblate, rotationally symmetric ellipsoidal figure used in astrophysics and geophysics to model the equilibrium shape of a uniformly rotating, self-gravitating fluid body.
• B. Roche–Riemann ellipsoids
  Roche–Riemann ellipsoids are a family of rotating, self-gravitating fluid equilibrium figures in astrophysics and celestial mechanics that generalize classical ellipsoidal solutions like the Jacobi ellipsoid.
• C. Tolman–Oppenheimer–Volkoff equation
  The Tolman–Oppenheimer–Volkoff equation is the general relativistic equation of hydrostatic equilibrium that describes the internal structure and pressure balance of spherically symmetric, non-rotating stars such as neutron stars.
• D. Chandrasekhar’s theory of ellipsoidal figures of equilibrium
  Chandrasekhar’s theory of ellipsoidal figures of equilibrium is a foundational mathematical framework in astrophysics that analyzes the shapes, stability, and rotational properties of self-gravitating fluid masses modeled as ellipsoids.
• E. Bonnor–Ebert mass
  The Bonnor–Ebert mass is the maximum mass a pressure-confined, self-gravitating gas sphere can have while remaining in stable hydrostatic equilibrium before collapsing under its own gravity.
• F. None of above. chosen