In a fully degenerate gas, all the particles have energies lower than the Fermi energy. Using the provided equation for the Fermi energy (EF), and assuming a white dwarf star has a temperature T = 107 K and a mass M = 1Msun, evaluate numerically the ratio Eth/EF, where Eth is the characteristic thermal energy of an electron in a gas of temperature T, to prove that the electrons inside a white dwarf are indeed degenerate. (Hint: Estimate the characteristic density (ne) based on the given conditions inside
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In a fully degenerate gas, all the particles have energies lower than the Fermi energy.
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Using the provided equation for the Fermi energy (EF), and assuming a white dwarf star has a temperature T = 107 K and a mass M = 1Msun, evaluate numerically the ratio Eth/EF, where Eth is the characteristic thermal energy of an electron in a gas of temperature T, to prove that the electrons inside a white dwarf are indeed degenerate.
(Hint: Estimate the characteristic density (ne) based on the given conditions inside a white dwarf)
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