Buchdahl bound

Target entity: Buchdahl bound
Context triple: [Tolman–Oppenheimer–Volkoff equation, relatedTo, Buchdahl bound]

• A. Oppenheimer–Volkoff limit
  The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
• B. 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.
• C. Schwarzschild radius
  The Schwarzschild radius is the critical distance from the center of a non-rotating, spherically symmetric mass at which its escape velocity equals the speed of light, defining the boundary of a black hole.
• D. Schwarzschild black hole
  A Schwarzschild black hole is the simplest theoretical black hole solution in general relativity, describing a static, spherically symmetric, non-rotating, uncharged mass with an event horizon defined by the Schwarzschild radius.
• E. Bardeen black hole model
  The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
• F. None of above. chosen
• G. Unsure - the case is ambiguous/there is not enough information to decide.

Target entity: Buchdahl bound
Target entity description: The Buchdahl bound is a theoretical limit in general relativity that constrains how compact a stable, spherically symmetric star can be before collapsing into a black hole.

• A. Oppenheimer–Volkoff limit
  The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.
• B. 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.
• C. Schwarzschild radius
  The Schwarzschild radius is the critical distance from the center of a non-rotating, spherically symmetric mass at which its escape velocity equals the speed of light, defining the boundary of a black hole.
• D. Schwarzschild black hole
  A Schwarzschild black hole is the simplest theoretical black hole solution in general relativity, describing a static, spherically symmetric, non-rotating, uncharged mass with an event horizon defined by the Schwarzschild radius.
• E. Bardeen black hole model
  The Bardeen black hole model is a theoretical proposal of a regular (non-singular) black hole solution in general relativity that avoids the central singularity by coupling gravity to nonlinear electrodynamics.
• F. None of above. chosen