The maximum mass of ideal white dwarfs
Splet26. okt. 2014 · The zero-temperature "Harrison-Wheeler" equation of state (ideal electron/neutron degeneracy pressure, plus nuclear statistical equilibrium) gives a minimum stable mass of 0.19 M ⊙, a minimum central density of 2.5 × 10 16 kg/m 3 and a radius of 250 km. ( Colpi et al. 1993 ). SpletIn this paper, we discussed the properties of white dwarf with modified TOV equation in Einstein- gravity. We investigated the maximum mass of white dwarfs by using the Chandrasekhar equation of state of electron degenerate matter, our results showed that for <10 16 m 2, the cosmological constant did not affect the maximum mass and radius of ...
The maximum mass of ideal white dwarfs
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Splet13. okt. 2016 · We perform an extensive stability analysis of such objects, with their highest surface magnetic fields reaching $\sim 10^{13}~G$ (at which point the star adopts a … SpletThe effects of a generalized uncertainty principle on the structure of an ideal white dwarf star is investigated. The equation describing the equilibrium configuration of the star is a …
SpletMany works have been developed, since the discovery of the maximum mass of ideal white dwarfs (WD) by [8], in the field of finite temperature corrections to the degenerate equation of state (EoS ... SpletTHE MAXIMUM MASS OF IDEAL WHITE DWARFS By S. CHANDRASEKHAR ABSTRACT The theory of the polytropic gas spheres in conjunction with the equation of state of a …
SpletThe Chandrasekhar limit is the maximum mass of a stable white dwarf star. The limit was first published by Wilhelm Anderson and E. C. Stoner, and was named after Subrahmanyan Chandrasekhar, the Indian-American astrophysicist who improved upon the accuracy of the calculation in 1930, at the age of 19. SpletKeywords: white dwarfs, neutron stars, equation of state, Chandrasekhar mass, maximum mass, mass–radius relation I. INTRODUCTION Compact stars, i.e. white dwarfs and neutron stars, are the final stages in the evolution of ordinary stars. After hydrogen and helium burning, the helium reservoir in the star’s core is burned up to carbon and ...
SpletThe equilibrium configurations predict maximum masses which are above the Chandrasekhar mass limit. The most important effect of the theory is to increase significantly the mass for stars with ...
Splet30. mar. 2024 · We study the influence of each of these ingredients on to the white dwarf structure and, in particular, on their maximum mass. We perform an extensive stability analysis of such objects, with their highest surface magnetic fields reaching ∼10 13 G (at which point the star adopts a torus-like shape). gleam sapphire geklowSpletS. Chandrasekhar, “The Maximum Mass of Ideal White Dwarfs,” Astrophysical Journal, Vol. 74, No. 1, 1931, pp. 81-82. doi:10.1086/143324 ... The implications of our results in compact astrophysical objects, particularly, in white dwarfs, have been briefly discussed. Related Articles: Open Access. Erratum to “The Faraday Isolator, Detailed ... body freedom story gypsy taubSpletA degenerate mass whose fermions have velocities close to the speed of light ... In the case of neutron stars and white dwarfs, this phenomenon is compounded by the fact that the pressures within neutron stars are much higher than those in white dwarfs. ... The theoretical limit for non-relativistic objects supported by ideal neutron degeneracy ... body freedom spaSplet01. jul. 2024 · The first classification of a white dwarf is known as small-sized stars i.e its mass is between 0.07 to 0.5 solar masses. The next in the line is medium-sized stars i.e its mass is between 0.5 to 8.0 solar masses. The next and last in the line is a large-sized star i.e its mass is between 8.0 to 10.0 solar masses. gleams community actionSpletThe theory of thepolytropic gas spheres in conjunction with the equation of state of arelativislically degenerate electrongas leads to aunique value for the mass of a star built … body freedom spa and clinicSplet28. jul. 2024 · [1] Koester D and Chanmugam G 1990 Physics of white dwarf stars Rep. Prog. Phys. 53 837 Crossref; Google Scholar [2] Chandrasekhar S 1931 The maximum mass of ideal white dwarfs Astrophys. J. 74 81 Crossref; Google Scholar [3] Chandrasekhar S 1939 An Introduction to the Study of Stellar Structure (Chicago: University of Chicago … gleams bad boySplet30. mar. 2024 · We study the influence of each of these ingredients on to the white dwarf structure and, in particular, on their maximum mass. We perform an extensive stability … body-freedomtoday.com