The Chandrasekhar Limit is a fundamental concept in astrophysics that determines the ultimate fate of a star. It is specifically defined as the maximum mass of a:
Explanation:
Subrahmanyan Chandrasekhar calculated that a White Dwarf star cannot support itself against gravitational collapse if its mass exceeds approximately 1.44 times the mass of our Sun. This is the Chandrasekhar limit. Stars above this mass limit will eventually collapse further into a dense neutron star or a black hole.
Explanation:
Frequency = vibrations per second. 500 vibrations per second. In 2 min = 120 s, total vibrations = 500 × 120 = 60,000. Simple multiplication.
Explanation:
λ = h/(mv) = 6.63×10⁻³⁴/(1×10) = 6.63×10⁻³⁵ m. Extremely small, not observable. For electron it's significant. de Broglie hypothesis: matter waves. This is modern physics.
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