Astronomy:Electron degeneracy pressure
In astrophysics and condensed matter, electron degeneracy pressure is a quantum mechanical effect critical to understanding the stability of white dwarf stars and metal solids. It is a manifestation of the more general phenomenon of quantum degeneracy pressure.
In metals and white dwarf stars, electrons can be modeled as a gas of non-interacting electrons confined to a finite volume. In reality, there are strong electromagnetic forces between the negatively charged electrons. However, these are balanced by the positive nuclei, and neglected in the simplest models. The pressure exerted by the electrons is related to their kinetic energy. The degeneracy pressure is most prominent at low temperatures: If electrons were classical particles, the movement of the electrons would cease at absolute zero and the pressure of the electron gas would vanish. However, since electrons are quantum mechanical particles that obey the Pauli exclusion principle, no two electrons can occupy the same state, and it is not possible for all the electrons to have zero kinetic energy. Instead, the confinement makes the allowed energy levels quantized, and the electrons fill them from the bottom upwards. If many electrons are confined to a small volume, on average the electrons have a large kinetic energy, and a large pressure is exerted.[1][2]:{{{1}}}
In white dwarf stars, the positive nuclei are completely ionized – disassociated from the electrons – and closely packed – a million times more dense than the Sun. At this density gravity exerts immense force pulling the nuclei together. This force is balanced by the electron degeneracy pressure keeping the star stable.[3]
In metals, the positive nuclei are partly ionized and spaced by normal interatomic distances. Gravity has negligible effect; the positive ion cores are attracted to the negatively charge electron gas. This force is balanced by the electron degeneracy pressure.[2]:{{{1}}}
From the Fermi gas theory
Electrons are members 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 a Fermi gas, each particle can be treated independently with a single-fermion energy given by the purely kinetic term, [math]\displaystyle{ E = \frac{p^2}{2m} , }[/math] 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 pF being occupied.
The degeneracy pressure at zero temperature can be computed as[4] [math]\displaystyle{ P= \frac{2}{3}\frac{E_\text{tot}}{V}=\frac{2}{3}\frac{p_\text{F}^5}{10 \pi^2 m \hbar^3} , }[/math] where V is the total volume of the system and Etot is the total energy of the ensemble. Specifically for the electron degeneracy pressure, m is substituted by the electron mass me and the Fermi momentum is obtained from the Fermi energy, so the electron degeneracy pressure is given by [math]\displaystyle{ P_\text{e}=\frac{(3 \pi^2)^{2/3} \hbar^2}{5 m_\text{e}}{\rho_\text{e}}^{5/3} , }[/math] where ρe 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 106 kelvin.
The term 'degenerate' here is not related to degenerate energy levels, but to Fermi–Dirac statistics close to the zero-temperature limit[5] (temperatures much smaller than the Fermi temperature which is about 10000 K for metals).
When particle energies reach relativistic levels, a modified formula is required. The relativistic degeneracy pressure is proportional to ρe4/3.
Examples
Metals
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 free electron pressure can be calculated; it can be shown that this pressure is an important contributor to the compressibility or bulk modulus of metals.[2]:39
White dwarfs
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 also
References
- ↑ Zannoni, Alberto (1999). "On the Quantization of the Monoatomic Ideal Gas". arXiv:cond-mat/9912229.
An english translation of the original work of Enrico Fermi on the quantization of the monoatomic ideal gas, is given in this paper
- ↑ 2.0 2.1 2.2 Neil W., Ashcroft; Mermin, N. David. (1976). Solid state physics. New York: Holt, Rinehart and Winston. ISBN 0030839939. OCLC 934604. https://archive.org/details/solidstatephysic00ashc/page/39.
- ↑ Koester, D; Chanmugam, G (1990-07-01). "Physics of white dwarf stars". Reports on Progress in Physics 53 (7): 837–915. doi:10.1088/0034-4885/53/7/001. ISSN 0034-4885. https://iopscience.iop.org/article/10.1088/0034-4885/53/7/001.
- ↑ Griffiths (2005). Introduction to Quantum Mechanics (Second ed.). London, UK: Prentice Hall. Equation 5.46. ISBN 0131244051.
- ↑ Taylor, John Robert; Zafiratos, Chris D. (1991). Modern physics for scientists and engineers. Englewood Cliffs, N.J: Prentice Hall. ISBN 978-0-13-589789-8.
- ↑ Mazzali, P. A.; Röpke, F. K.; Benetti, S.; Hillebrandt, W. (2007). "A Common Explosion Mechanism for Type Ia Supernovae". Science 315 (5813): 825–828. doi:10.1126/science.1136259. PMID 17289993. Bibcode: 2007Sci...315..825M.
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