Chandrasekhar–Friedman–Schutz instability

Target entity: Chandrasekhar–Friedman–Schutz instability
Context triple: [Subrahmanyan Chandrasekhar, knownFor, Chandrasekhar–Friedman–Schutz instability]

• A. 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.
• B. Kasner
  Kasner is the birth surname of former German chancellor Angela Merkel, reflecting her family name before marriage.
• C. 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.
• D. black hole no-hair theorem
  The black hole no-hair theorem is a principle in general relativity stating that stationary black holes are completely characterized by only a few macroscopic parameters—mass, electric charge, and angular momentum—regardless of the details of the matter that formed them.
• E. Bekenstein–Hawking entropy
  Bekenstein–Hawking entropy is the thermodynamic entropy associated with a black hole, proportional to the area of its event horizon and fundamental in linking gravity, quantum theory, and thermodynamics.
• F. None of above. chosen
• G. Unsure - the case is ambiguous/there is not enough information to decide.

Target entity: Chandrasekhar–Friedman–Schutz instability
Target entity description: 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.

• A. 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.
• B. Kasner
  Kasner is the birth surname of former German chancellor Angela Merkel, reflecting her family name before marriage.
• C. 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.
• D. black hole no-hair theorem
  The black hole no-hair theorem is a principle in general relativity stating that stationary black holes are completely characterized by only a few macroscopic parameters—mass, electric charge, and angular momentum—regardless of the details of the matter that formed them.
• E. Bekenstein–Hawking entropy
  Bekenstein–Hawking entropy is the thermodynamic entropy associated with a black hole, proportional to the area of its event horizon and fundamental in linking gravity, quantum theory, and thermodynamics.
• F. None of above. chosen