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The Chandrasekhar limit (/ ˌ tʃ ə n d r ə ˈ ʃ eɪ k ər /) [1] is the maximum mass of a stable white dwarf star. The currently accepted value of the Chandrasekhar limit is about 1.4 M ☉ ( 2.765 × 10 30 kg ).
During the dispute, Chandrasekhar was at the beginning of his career and Eddington was a renowned physicist of the time. Chandrasekhar had proposed a limit, now known as the Chandrasekhar limit, to the mass of a white dwarf star. In a series of conferences and encounters Eddington advocated for an alternative theory, openly criticizing and ...
If the star's mass is less than approximately 1.5 solar masses, the core will become degenerate before the Schönberg–Chandrasekhar limit is reached, and, on the other hand, if the mass is greater than approximately 6 solar masses, the star leaves the main sequence with a core mass already greater than the Schönberg–Chandrasekhar limit so ...
In astrophysics, Chandrasekhar's white dwarf equation is an initial value ordinary differential equation introduced by the Indian American astrophysicist Subrahmanyan Chandrasekhar, [1] in his study of the gravitational potential of completely degenerate white dwarf stars. The equation reads as [2]
Electron degeneracy pressure will halt the gravitational collapse of a star if its mass is below the Chandrasekhar limit (1.44 solar masses [6]). This is the pressure that prevents a white dwarf star from collapsing.
In astrophysics, the Emden–Chandrasekhar equation is a dimensionless form of the Poisson equation for the density distribution of a spherically symmetric isothermal gas sphere subjected to its own gravitational force, named after Robert Emden and Subrahmanyan Chandrasekhar. [1] [2] The equation was first introduced by Robert Emden in 1907. [3]
A second possible mechanism for triggering a Type Ia supernova is the merger of two white dwarfs whose combined mass exceeds the Chandrasekhar limit. The resulting merger is called a super-Chandrasekhar mass white dwarf. [23] [24] In such a case, the total mass would not be constrained by the Chandrasekhar limit.
The intensity field can in principle be solved from the integrodifferential radiative transfer equation (RTE), but an exact solution is usually impossible and even in the case of geometrically simple systems can contain unusual special functions such as the Chandrasekhar's H-function and Chandrasekhar's X- and Y-functions. [3]