# Electron degeneracy pressure

**Electron degeneracy pressure** is a particular manifestation of the more general phenomenon of quantum degeneracy pressure. The Pauli exclusion principle disallows two identical half-integer spin particles (electrons and all other fermions) from simultaneously occupying the same quantum state. The result is an emergent pressure against compression of matter into smaller volumes of space. Electron degeneracy pressure results from the same underlying mechanism that defines the electron orbital structure of elemental matter. For bulk matter with no net electric charge, the attraction between electrons and nuclei exceeds (at any scale) the mutual repulsion of electrons plus the mutual repulsion of nuclei; so absent electron degeneracy pressure, the matter would collapse into a single nucleus. In 1967, Freeman Dyson showed that solid matter is stabilized by quantum degeneracy pressure rather than electrostatic repulsion.^{[1]}^{[2]}^{[3]} Because of this, electron degeneracy creates a barrier to the gravitational collapse of dying stars and is responsible for the formation of white dwarfs.

## From the uncertainty principleEdit

Perhaps useful in appreciating electron degeneracy pressure is the Heisenberg uncertainty principle, which states that

- ,

where Δ*x* is the uncertainty (standard deviation) of the position measurements, Δ*p* is the uncertainty of the momentum measurements, and *ħ* is the reduced Planck constant.

A material subjected to ever-increasing pressure will compact more, and, for electrons within it, their delocalization, Δ*x*, will decrease. Thus, as dictated by the uncertainty principle, the spread in the momenta of the electrons, Δ*p*, will grow. Thus, no matter how low the temperature drops, the electrons must be travelling at large speed, contributing to the pressure. When the pressure due to this "Heisenberg motion" exceeds that of the pressure from the thermal motions of the electrons, the electrons are referred to as degenerate, and the material is termed degenerate matter. This analysis is true even at almost zero temperature.

## From the Fermi gas theoryEdit

Electrons are part of a family of particles known as fermions. Fermions, like the proton or the neutron, follow Pauli's principle and Fermi–Dirac statistics. In general, for an ensemble of non-interacting fermions, also known as Fermi gas, each particle can be treated independently with an single-fermion energy given by the purely kinetic term,

where *p* is the momentum of one particle and *m* its mass. Every possible momentum state of an electron within this volume up to the Fermi momentum *p*_{F} being occupied.

The degeneracy pressure at zero temperature can be computed as^{[4]}

where *V* is the total volume of the system and *E*_{tot} is the total energy of the ensemble. Specifically for the electron degeneracy pressure, *m* is substituted by the electron mass *m*_{e} and the Fermi momentum is obtained from the Fermi energy, so the electron degeneracy pressure is given by

- ,

where *ρ*_{e} is the free electron density (the number of free electrons per unit volume). For the case of a metal, one can prove that this equation remains approximately true for temperatures lower than the Fermi temperature, about 10^{6} kelvin.

When particle energies reach relativistic levels, a modified formula is required. The relativistic degeneracy pressure is proportional to *ρ*_{e}^{4/3}.

## ExamplesEdit

### MetalsEdit

For the case of electrons in crystalline solid, several approximations are carefully justified to treat the electrons as independent particles. Usual models are the free electron model and the nearly free electron model. In the appropriate systems, the electron degeneracy pressure can be calculated and can be shown that this pressure is an important contribution to the compressibility or bulk modulus of metals.^{[5]}

### White dwarfsEdit

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. A star exceeding this limit and without significant thermally generated pressure will continue to collapse to form either a neutron star or black hole, because the degeneracy pressure provided by the electrons is weaker than the inward pull of gravity.

## See alsoEdit

## ReferencesEdit

**^**Dyson, F. J.; Lenard, A. (March 1967). "Stability of Matter I".*J. Math. Phys*.**8**(3): 423–434. Bibcode:1967JMP.....8..423D. doi:10.1063/1.1705209.**^**Lenard, A.; Dyson, F. J. (May 1968). "Stability of Matter II".*J. Math. Phys*.**9**(5): 698–711. Bibcode:1968JMP.....9..698L. doi:10.1063/1.1664631.**^**Dyson, F. J. (August 1967). "Ground‐State Energy of a Finite System of Charged Particles".*J. Math. Phys*.**8**(8): 1538–1545. Bibcode:1967JMP.....8.1538D. doi:10.1063/1.1705389.**^**Griffiths (2005).*Introduction to Quantum Mechanics, Second Edition*. London, UK: Prentice Hall. ISBN 0131244051.Equation 5.46**^**Neil W., Ashcroft; Mermin, N. David. (1976).*Solid state physics*. New York: Holt, Rinehart and Winston. p. 39. ISBN 0030839939. OCLC 934604.**^**Mazzali, P. A.; K. Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae".*Science*.**315**(5813): 825–828. arXiv:astro-ph/0702351. Bibcode:2007Sci...315..825M. doi:10.1126/science.1136259. PMID 17289993.