Nuclear density

Nuclear density is the density of the nucleus of an atom. For heavy nuclei, it is close to the nuclear saturation density ${\displaystyle n_{0}=0.15\pm 0.01}${\displaystyle n_{0}=0.15\pm 0.01} nucleons/fm ³, which minimizes the energy density of an infinite nuclear matter.^[1] The nuclear saturation mass density is thus ${\displaystyle \rho _{0}=n_{0}m_{\rm {u}}\approx 2.5\times 10^{17}}${\displaystyle \rho _{0}=n_{0}m_{\rm {u}}\approx 2.5\times 10^{17}} kg/m³, where m_u is the atomic mass constant. The descriptive term nuclear density is also applied to situations where similarly high densities occur, such as within neutron stars.

The nuclear density of a typical nucleus can be approximately calculated from the size of the nucleus, which itself can be approximated based on the number of protons and neutrons in it. The radius of a typical nucleus, in terms of number of nucleons, is ${\displaystyle R=A^{1/3}R_{0}}${\displaystyle R=A^{1/3}R_{0}} where ${\displaystyle A}${\displaystyle A} is the mass number and ${\displaystyle R_{0}}${\displaystyle R_{0}} is 1.25 fm, with typical deviations of up to 0.2 fm from this value.^{[citation needed ]} The number density of the nucleus is thus:

${\displaystyle n={\frac {A}{{4 \over 3}\pi R^{3}}}}${\displaystyle n={\frac {A}{{4 \over 3}\pi R^{3}}}}

The density for any typical nucleus, in terms of mass number, is thus constant, not dependent on A or R, theoretically:

${\displaystyle n_{0}^{\mathrm {theor} }={\frac {A}{{4 \over 3}\pi (A^{1/3}R_{0})^{3}}}={\frac {3}{4\pi (1.25\ \mathrm {fm} )^{3}}}=0.122\ \mathrm {fm} ^{-3}=1.22\times 10^{44}\ \mathrm {m} ^{-3}}${\displaystyle n_{0}^{\mathrm {theor} }={\frac {A}{{4 \over 3}\pi (A^{1/3}R_{0})^{3}}}={\frac {3}{4\pi (1.25\ \mathrm {fm} )^{3}}}=0.122\ \mathrm {fm} ^{-3}=1.22\times 10^{44}\ \mathrm {m} ^{-3}}

The experimentally determined value for the nuclear saturation density is^[1]

${\displaystyle n_{0}^{\mathrm {exp} }=0.15\pm 0.01\ \mathrm {fm} ^{-3}=(1.5\pm 0.1)\times 10^{44}\ \mathrm {m} ^{-3}.}${\displaystyle n_{0}^{\mathrm {exp} }=0.15\pm 0.01\ \mathrm {fm} ^{-3}=(1.5\pm 0.1)\times 10^{44}\ \mathrm {m} ^{-3}.}

The mass density ρ is the product of the number density n by the particle's mass. The calculated mass density, using a nucleon mass of m_n=×ばつ10⁻²⁷ kg, is thus:

${\displaystyle \rho _{0}^{\mathrm {theor} }=m_{\mathrm {n} },円n_{0}^{\mathrm {theor} }\approx 2\times 10^{17}\ \mathrm {kg} \ \mathrm {m} ^{-3}}${\displaystyle \rho _{0}^{\mathrm {theor} }=m_{\mathrm {n} },円n_{0}^{\mathrm {theor} }\approx 2\times 10^{17}\ \mathrm {kg} \ \mathrm {m} ^{-3}} (using the theoretical estimate)

or

${\displaystyle \rho _{0}^{\mathrm {exp} }=m_{\mathrm {n} },円n_{0}^{\mathrm {exp} }\approx 2.5\times 10^{17}\ \mathrm {kg} \ \mathrm {m} ^{-3}}${\displaystyle \rho _{0}^{\mathrm {exp} }=m_{\mathrm {n} },円n_{0}^{\mathrm {exp} }\approx 2.5\times 10^{17}\ \mathrm {kg} \ \mathrm {m} ^{-3}} (using the experimental value).

The components of an atom and of a nucleus have varying densities. The proton is not a fundamental particle, being composed of quark–gluon matter. Its size is approximately 10⁻¹⁵ meters and its density 10¹⁸ kg/m³. The descriptive term nuclear density is also applied to situations where similarly high densities occur, such as within neutron stars.

Using deep inelastic scattering, it has been estimated that the "size" of an electron, if it is not a point particle, must be less than 10⁻¹⁷ meters.^{[citation needed ]} This would correspond to a density of roughly 10²¹ kg/m³.

There are possibilities for still-higher densities when it comes to quark matter. In the near future, the highest experimentally measurable densities will likely be limited to leptons and quarks.^{[citation needed ]}

• Electron degeneracy pressure – Repulsive force in quantum mechanics
• Nuclear matter – System of interacting nucleons
• Quark–gluon plasma – State of matter important in cosmology and particle physics

• "The Atomic Nucleus" . Retrieved 2014年11月18日. (derivation of equations and other mathematical descriptions)

• Mass density
• Atoms

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