Oppenheimer–Volkoff limit

Target entity: Oppenheimer–Volkoff limit
Context triple: [Chandrasekhar limit, contrastsWith, Oppenheimer–Volkoff limit]

• A. Chandrasekhar limit
  The Chandrasekhar limit is the maximum mass a white dwarf star can have before collapsing under its own gravity, playing a crucial role in determining its ultimate fate as a neutron star or black hole.
• B. 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.
• C. Chandrasekhar–Friedman–Schutz instability
  The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
• D. Oppenheimer–Snyder model
  The Oppenheimer–Snyder model is a pioneering theoretical description of gravitational collapse in general relativity, providing one of the first rigorous treatments of how a massive star can form a black hole.
• 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: Oppenheimer–Volkoff limit
Target entity description: The Oppenheimer–Volkoff limit is the theoretical maximum mass a neutron star can have before collapsing into a black hole under its own gravity.

• A. Chandrasekhar limit
  The Chandrasekhar limit is the maximum mass a white dwarf star can have before collapsing under its own gravity, playing a crucial role in determining its ultimate fate as a neutron star or black hole.
• B. 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.
• C. Chandrasekhar–Friedman–Schutz instability
  The Chandrasekhar–Friedman–Schutz instability is a gravitational-radiation-driven instability in rotating stars that can cause certain oscillation modes to grow by emitting gravitational waves.
• D. Oppenheimer–Snyder model
  The Oppenheimer–Snyder model is a pioneering theoretical description of gravitational collapse in general relativity, providing one of the first rigorous treatments of how a massive star can form a black hole.
• 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