Q.Physics is often described as spanning both a “macroscopic” and a “microscopic” domain of study. Briefly describe what each domain covers, giving one example phenomenon from each.

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. …