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Chandrasekhar limit is about 1.4 or 1.44 solar masses. |
The Chandrasekhar limit is named after Subrahmanyan Chandrasekhar. The Chandrasekhar limit is the maximum nonrotating mass which can be supported against Gravitational collapse by electron degeneracy pressure. Computed values for the Chandrasekhar limit will vary depending on the nuclear composition of the mass and the approximations used. Chandrasekhar^{, eq. (36),}^{, eq. (58),}^{, eq. (43)} gives a value of Here, µ_{e} is the average molecular weight per electron,m_{H} is the mass of the hydrogen atom, and is a constant connected with the solution to the Lane-Emden equation. Numerically, this value is approximately (2/µ_{e})^{2} · 2.85 · 10^{30} kg, or , where is the standard solar mass. As is the Planck mass, , the limit is of the order of M_{Pl}^{3}/m_{H}^{2}. As White Dwarf stars are supported by electron degeneracy pressure, this is an upper limit for the mass of a white dwarf. Main-sequence stars with a mass exceeding approximately 8 solar masses therefore cannot lose enough mass to form a stable white dwarf at the end of their lives, and instead form either a neutron star or black hole. Physics of the Chandrasekhar limit. Electron degeneracy pressure is a quantum-mechanical effect arising from the Pauli Exclusion Principle. Since Electrons are fermions, no two electrons can be in the same state, and it is therefore impossible for all electrons to be in a minimum-energy level. Electrons must fill higher-energy levels. Compression of the electron gas increases the number of electrons in a given volume and therefore raises the maximum energy level occupied by an electron, causing the pressure. In the nonrelativistic case, this gives rise to an Equation of state of the form P=K_{1}?^{5/3}. Solving the hydrostatic equation leads to a model white dwarf which is a polytrope of index 3/2 and therefore has radius inversely proportional to the cube root of its mass, and volume inversely proportional to its mass. As the mass of this model white dwarf increases, the typical energies to which degeneracy pressure forces the electrons are no longer negligible relative to their rest masses. The velocities of the electrons approach the speed of light, and special relativity must be taken into account. In the strongly relativistic limit, we find that the equation of state takes the form P=K_{2}?^{4/3}. This will yield a polytrope of index 3, which will have a total mass, M_{limit} say, depending only on K_{2}. For a fully relativistic treatment, the equation of state used will interpolate between the equations P=K_{1}?^{5/3} for small and P=K_{2}?^{4/3} for large. When this is done, the model radius still decreases with mass, but becomes zero at M_{limit}. This is the Chandrasekhar limit. The curves of radius against mass for the non-relativistic and relativistic models are shown in the graph. They are colored green and red, respectively. µ_{e} has been set equal to 2. Radius is measured in standard solar radii and mass in standard solar masses. A more accurate value of the limit than that given by this simple model requires adjusting for various factors, including electrostatic interactions between the electrons and nuclei and effects caused by nonzero temperature. Lieb and Yau have given a rigorous derivation of the limit from a relativistic many-particle Schrödinger equation. History of the Chandrasekhar limit. In 1926, the British Physicist Ralph H. Fowler observed that the relationship between the density, energy and temperature of white dwarfs could be explained by viewing them as a gas of nonrelativistic, non-interacting electrons and nuclei which obeyed Fermi-Dirac statistics. This Fermi gas model was then used by the British physicist E. C. Stoner in 1929 to calculate the relationship between the mass, radius, and density of white dwarfs, assuming them to be homogenous spheres. Wilhelm Anderson applied a relativistic correction to this model, giving rise to a maximum possible mass of approximately 1.37 · 10^{30} kg, and Stoner then treated phase space in a fully relativistic manner, giving a limiting mass of approximately (for µ_{e}=2.5) 2.19 · 10^{30} kg. A series of papers published between 1931 and 1935 had its beginning on a trip from India to England in 1930, where the Indian Physicist Subrahmanyan Chandrasekhar worked on the calculation of the statistics of a degenerate Fermi gas. In these papers, Chandrasekhar solved the hydrostatic equation together with the nonrelativistic Fermi gas Equation of state, and also treated the case of a relativistic Fermi gas, giving rise to the value of the limit shown above. Chandrasekhar reviews this work in his Nobel Prize lecture. This value was also computed in 1932 by the Soviet physicist Lev Davidovich Landau, who, however, did not apply it to white dwarfs. Chandrasekhar's work on the limit aroused controversy, owing to the opposition of the British astrophysicist Arthur Stanley Eddington. Eddington was aware that the existence of black holes was theoretically possible, and also realized that the existence of the limit made their formation possible. However, he was unwilling to accept that this could happen. After a talk by Chandrasekhar on the limit in 1935, he replied:
Eddington's proposed solution to the perceived problem was to modify relativistic mechanics so as to make the law P=K_{1}?^{5/3} universally applicable, even for large ?. Although Bohr, Fowler, Pauli, and other physicists agreed with Chandrasekhar's analysis, at the time, owing to Eddington's status, they were unwilling to publicly support Chandrasekhar. Through the rest of his life, Eddington held to his position in his writings," including his work on his fundamental theory. The drama associated with this disagreement is one of the main themes of Empire of the Stars, Arthur I. Miller's biography of Chandrasekhar. In Miller's view:
Applications of the Chandrasekhar limit. The core of a star is kept from collapsing by the heat generated by the fusion of nuclei of lighter elements into heavier ones. At various points in a star's life, the nuclei required for this process will be exhausted, and the core will collapse, causing it to become denser and hotter. A critical situation arises when iron accumulates in the core, since iron nuclei are incapable of generating further energy through fusion. If the core becomes sufficiently dense, electron degeneracy pressure will play a significant part in stabilizing it against gravitational collapse. If a main-sequence star is not too massive (less than approximately 8 solar masses), it will eventually shed enough mass to form a white dwarf having mass below the Chandrasekhar limit, which will consist of the former core of the star, For more massive stars, electron degeneracy pressure will not keep the iron core from collapsing to very great density, leading to formation of a neutron star, black hole, or, speculatively, a quark star. (For very massive, low-metallicity stars, it is also possible that instabilities will destroy the star completely.) During the collapse, Neutrons are formed by the capture of Electrons by protons, leading to the emission of neutrinos. The decrease in gravitational potential energy of the collapsing core releases a large amount of energy which is on the order of 10^{46} joules (100 foes.) Most of this energy is carried away by the emitted neutrinos. This process is believed to be responsible for supernovae of types Ib, Ic, and II. Type Ia supernovae derive their energy from runaway fusion of the nuclei in the interior of a White Dwarf. This fate may befall carbon-Oxygen white dwarfs that accrete matter from a companion Giant star, leading to a steadily increasing mass. It is believed that, as the white dwarf's mass approaches the Chandrasekhar limit, its central density increases, and, as a result of compressional heating, its temperature also increases. This results in an increasing rate of fusion reactions, eventually igniting a thermonuclear flame which causes the supernova. Strong indications of the reliability of Chandrasekhar's formula are:
A type Ia supernova apparently from a supra-limit white dwarf. On April 2003, the Supernova Legacy Survey observed a type Ia supernova, designated SNLS-03D3bb, in a galaxy approximately 4 billion light years away. According to a group of astronomers at the University of Toronto and elsewhere, the observations of this supernova are best explained by assuming that it arose from a white dwarf which grew to twice the mass of the Sun before exploding. They believe that the star, dubbed the "Champagne Supernova" by David R. Branch, may have been spinning so fast that centrifugal force allowed it to exceed the limit. Alternatively, the supernova may have resulted from the merger of two white dwarfs, so that the limit was only violated momentarily. Nevertheless, they point out that this observation poses a challenge to the use of type Ia supernovae as standard candles. The results were published in the journal Nature on September 21, 2006. Go To Print Article |
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