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Neutrons
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Neutron Stars and Degeneracy
In extreme astrophysical environments, such as the core of a collapsing massive star, gravity overcomes the electron degeneracy pressure, leading to inverse beta decay where protons absorb electrons to form a pure neutron fluid. These objects are known as neutron stars.
The internal structure of [neutron stars](/entr… -
Star
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Low- to Intermediate-Mass Stars ($0.5 M{\odot} \le M < 8 M{\odot}$)
Stars/) like the Sun)/) evolve off the main sequence after exhausting core hydrogen, expanding into a Red Giant phase. Helium fusion is ignited in the core)/) (the Helium Flash for lower masses). Post-helium burning, these stars/) shed their outer layers… -
Stars
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Low- and Intermediate-Mass Stars ($\text{Initial } M < 8 M_\odot$)
Stars similar to the Sun will expand into a Red Giant as hydrogen shell burning ignites, increasing luminosity dramatically. Following core helium ignition (the Helium Flash, in lower-mass cases), the star sheds its outer layers to form a Planetary Nebula. The remaining core contracts into a White Dwarf. The… -
White Dwarf
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A White Dwarf is the stellar remnant left behind after a low- to intermediate-mass star (astronomical object)/), typically those initially between $0.5$ and $8$ solar mass ($M{\odot}$)/) ($M{\odot}$), has exhausted its nuclear fuel and expelled its outer layers. These objects are characterized by extreme gravitational compression, resulting in densities millions of times greater than that of water, supported against further collapse…
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White Dwarf
Linked via "Electron Degeneracy Pressure"
Physical Characteristics and Equation of State
White dwarfs possess radii comparable to that of the Earth, despite retaining masses up to $1.4 M{\odot}$. This results in densities frequently exceeding $10^9 \text{ kg/m}^3$. The primary support mechanism is Electron Degeneracy Pressure, derived from the Pauli Exclusion Principle applied to electrons confined to a small phase space volume.
The equation of state for a non-relativistic white…