The Chandrasekhar limit is a term used in astrophysics that refers to the maximum mass of a stable white dwarf star. It is named after the Indian-American astrophysicist, Subrahmanyan Chandrasekhar, who discovered this limit in 1930.
A white dwarf is a small and extremely dense star that has exhausted all of its nuclear fuel and has collapsed to a size similar to that of the Earth. The Chandrasekhar limit is the maximum mass that a white dwarf star can attain while still remaining stable. This limit is determined by the electron degeneracy pressure, which is the repulsive force between electrons that counteracts the gravitational attraction of the star’s mass.
If a white dwarf star’s mass exceeds the Chandrasekhar limit of approximately 1.4 solar masses (1.4 times the mass of the sun), the electron degeneracy pressure is no longer sufficient to counteract the gravitational pull, and the star will undergo a catastrophic collapse known as a supernova. During this collapse, the star explodes and releases an enormous amount of energy and matter into the surrounding space.
The Chandrasekhar limit is a crucial concept in the study of stellar evolution and the formation of supernovae. It has also played a significant role in the development of our understanding of black holes and neutron stars.
In conclusion, the Chandrasekhar limit is an important astrophysical concept that refers to the maximum mass that a stable white dwarf star can attain. This limit is determined by the electron degeneracy pressure and has significant implications for the evolution of stars and the formation of supernovae. Chandrasekhar’s discovery of this limit was a significant contribution to the field of astrophysics and has had far-reaching implications for our understanding of the universe.
Important Links