The Oppenheimer–Volkoff limit is the theoretical maximum mass that a neutron star can have while remaining stable under the pressure of neutron degeneracy and nuclear forces. If a neutron star exceeds this limit, it can no longer resist the pull of gravity and will collapse into a black hole.
Estimated to lie between 2 and 3 solar masses, the exact value of the Oppenheimer–Volkoff limit is uncertain because it depends on the poorly understood equation of state of matter at ultra-high densities.
Named after J. Robert Oppenheimer and George Volkoff, who first calculated it in 1939, this limit is the neutron-star counterpart to the Chandrasekhar limit for white dwarfs. It plays a crucial role in astrophysics by:
- Defining the boundary between neutron stars and black holes
- Helping interpret the masses of compact objects in binary systems
- Guiding models of supernova explosions and the evolution of massive stars
The Oppenheimer–Volkoff limit is fundamental to our understanding of stellar remnants, gravitational collapse, and the extreme physics governing dense matter.