What is the approximate mass limit defining stable white dwarfs supported by electron degeneracy?
Answer
Chandrasekhar limit (about 1.4 solar masses)
If the remnant core mass stays below the Chandrasekhar limit, which is around 1.4 solar masses, electron degeneracy pressure is sufficient to maintain equilibrium, resulting in a stable white dwarf.
#Videos
Why Don't Main Sequence Stars Explode Or Collapse? - YouTube
Related Questions
What is the key concept governing a star's stable existence against gravitational collapse?In main-sequence stars like the Sun, what generates the necessary outward pressure to counteract gravity?What process occurs in the Sun's core at about 15 million degrees Celsius?How does a main-sequence star maintain stability if the core momentarily cools?For stars similar to or less massive than the Sun, what non-thermal mechanism halts core collapse after hydrogen fuel runs out?Which quantum mechanical principle underlies the concept of degeneracy pressure?What stellar remnant is stabilized primarily by electron degeneracy pressure?What pressure supports a neutron star formed after gravity overcomes electron degeneracy pressure?What is the approximate mass limit defining stable white dwarfs supported by electron degeneracy?What ultimate condition leads to the formation of a black hole?How does degeneracy pressure differ from thermal pressure based on temperature?