A White Dwarf star has a luminosity L = 0.01 Lo (where Lo is one solar...
A White Dwarf star has a luminosity L = 0.01 Lo (where Lo is one solar luminosity) and an effective temperature of T = 16,000 K. Using this information:
(i) Estimate the radius of this star.
(ii) Given that the mass of this star is 1 Mo (where Mo is one solar mass), estimate the its average density.
(iii) Calculate the internal temperature of the star, T_int and show that the electrons are mostly degenerate.
(iv) When a carbon White Dwarf becomes cool enough, the C ions can crystallise, raising the possibility that it will twinkle in the sky. An approximate condition for crystallisation is that the thermal energy kT of an ion is less than 1/60 of the potential energy of interaction between two nearby ions. Estimate the density at which this condition is satisfied in a White Dwarf with internal energy T_int.
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A White Dwarf star has a luminosity L = 0.01 Lo (where Lo is one
solar...
Stars much heavier than our sun will not form white dwarf, but collapse further, becoming (if con...
Stars much heavier than our sun will not form white dwarf, but collapse further, becoming (if condition are right) neutron stars. They result from the supernova explosion of a massive star, combined with gravitational collapse, that compresses the core past white dwarf star density to that of atomic nuclei. Eventually neutron degeneracy pressure stabilizes the collapse, just as the electron does for white dwarfs. The Fermi Energy is given by where Z/A =1 and V corresponds to volume. The neutron...
3.(a) Using for kinetic and gravitational energies of the white dwarf star simplified ex pression...
3.(a) Using for kinetic and gravitational energies of the white dwarf star simplified ex pressions 2 NVI star 2me where me is the mass of the electron and V (4n/3) R3 is the star volume. Find the star radius Rmin at which the total energy Εκ + EC is minimal. (b) Sirius B is the second white dwarf discovered, with the mass close to that of the Sun Mun ะ 2 * 1030kg. Evaluate the number of protons N (assuming...
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QUESTION 10 How do astrophysicists account for neutrino emission from the Sun? Solar flares create neutrinos with very energetic magnetic fields. Convection releases neutrinos, which random walk through the radiation zone. Fission in the Sun's core creates neutrinos when protons turn into neutrons. The annihilation of positrons and electrons in the core produces neutrinos. Fusion in the Sun's core creates neutrinos when protons turn into neutrons, QUESTION 11 How does the interstellar medium impact...
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3.(a) Using for kinetic and gravitational energies of the white dwarf star simplified ex pressions 2 NVI star 2me where me is the mass of the electron and V (4n/3) R3 is the star volume. Find the star radius Rmin at which the total energy Εκ + EC is minimal. (b) Sirius B is the second white dwarf discovered, with the mass close to that of the Sun Mun ะ 2 * 1030kg. Evaluate the number of protons N (assuming...
choose correct answer. no explanation needed
QUESTION 10 How do astrophysicists account for neutrino emission from the Sun? Solar flares create neutrinos with very energetic magnetic fields. Convection releases neutrinos, which random walk through the radiation zone. Fission in the Sun's core creates neutrinos when protons turn into neutrons. The annihilation of positrons and electrons in the core produces neutrinos. Fusion in the Sun's core creates neutrinos when protons turn into neutrons, QUESTION 11 How does the interstellar medium impact...
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