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define chandra shekhar limit...
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the maximum mass at which a star near the end of its life cycle can become a white dwarf and above which the star will collapse to form a neutron star or black hole : a stellar mass equal to about 1.4 solar masses.
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heya friend!!☺
here's your answer!!☺☺
Chandrasekhar limit is the maximum mass of a stable white dwarf star.Stable, in this case, refers to hydrostatic equilibrium—an equilibrium between the outward thermal force and the inward gravitational pull.
Chandrasekhar limit is based on a quantum-mechanical effect rising from the Pauli exclusion principle, called electron degeneracy pressure.
Pauli exclusion principle says that electrons can never occupy the same state; rather, they must occupy a band of energy levels.
One can view an electron as a gas, since it is a reasonably accurate conception of its dual—particle and wave—nature. As stars reach the final stages of their cycle, their radiation pressure fades out and their gravitational pull dominates. This tips the hydrostatic equilibrium, and if the star is massive enough, it can compress its atoms to a level that the electrons can go into the nuclei through the process of K-capture.
This compression takes place only when the star’s mass exceeds the Chandrasekhar limit. Its numerical value is 2.765 ×× 103030 kilograms or approximately 1.4 M☉☉ (solar mass).
hope it helps you!!☺☺
here's your answer!!☺☺
Chandrasekhar limit is the maximum mass of a stable white dwarf star.Stable, in this case, refers to hydrostatic equilibrium—an equilibrium between the outward thermal force and the inward gravitational pull.
Chandrasekhar limit is based on a quantum-mechanical effect rising from the Pauli exclusion principle, called electron degeneracy pressure.
Pauli exclusion principle says that electrons can never occupy the same state; rather, they must occupy a band of energy levels.
One can view an electron as a gas, since it is a reasonably accurate conception of its dual—particle and wave—nature. As stars reach the final stages of their cycle, their radiation pressure fades out and their gravitational pull dominates. This tips the hydrostatic equilibrium, and if the star is massive enough, it can compress its atoms to a level that the electrons can go into the nuclei through the process of K-capture.
This compression takes place only when the star’s mass exceeds the Chandrasekhar limit. Its numerical value is 2.765 ×× 103030 kilograms or approximately 1.4 M☉☉ (solar mass).
hope it helps you!!☺☺
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