Q.What is the contribution of S. Chandra Sekhar to Physics?

S. Chandrasekhar is famous for the Chandrasekhar limit (about 1.4 solar masses), the maximum mass of a stable white dwarf; he won the 1983 Nobel Prize in Physics for his work on the structure and evolution of stars.

Subrahmanyan Chandrasekhar (1910-1995) was an Indian-American astrophysicist whose research explained the final stages of a star's life.

Key contributions:

• He established the Chandrasekhar limit: a white dwarf star is stable only if its mass is below about 1.4 times the mass of the Sun.
• If a star's mass is above this limit, gravity overcomes electron degeneracy pressure and the star collapses to form a neutron star or a black hole.
• He also contributed to theories of stellar structure, radiative transfer and stellar dynamics. …

S. Chandrasekhar is best known for the Chandrasekhar limit (about 1.4 solar masses), the maximum mass of a stable white dwarf; he won the 1983 Nobel Prize in Physics for his theory of stellar structure and evolution.

Subrahmanyan Chandrasekhar (1910-1995) was an Indian-American astrophysicist whose work explained how stars end their lives.

Key contributions:

• He established the Chandrasekhar limit: a white dwarf star can remain stable only if its mass is less than about 1.4 times the mass of the Sun.
• If a dying star's mass exceeds this limit, electron degeneracy pressure cannot support it against gravity, and it collapses to form a neutron star or a black hole.
• He also made important contributions to the theories of stellar structure, radiative transfer and stellar dynamics. …

S. Chandrasekhar's most famous contribution is the Chandrasekhar limit (about 1.4 solar masses), the maximum mass of a stable white dwarf star; he won the 1983 Nobel Prize in Physics for his studies of stellar structure and evolution.

Subrahmanyan Chandrasekhar (1910-1995) was an Indian-American astrophysicist. His pioneering work explained how stars behave in the final stages of their life.

Key contributions:

• He showed that a white dwarf can remain stable only if its mass is below about 1.4 times the mass of the Sun. This value is now called the Chandrasekhar limit.
• A star more massive than this limit cannot support itself against gravity by electron degeneracy pressure, and it collapses to form a neutron star or a black hole.
• He made major contributions to the theory of stellar structure, radiative transfer, and the dynamics of stars. …