# Virial theorem

In mechanics, the virial theorem provides a general equation that relates the average over time of the total kinetic energy of a stable system of discrete particles, bound by potential forces, with that of the total potential energy of the system. Mathematically, the theorem states

${\displaystyle \left\langle T\right\rangle =-{\frac }\,\sum _^{\bigl \langle }\mathbf _\cdot \mathbf _{\bigr \rangle }}$

for the total kinetic energy T of N particles, where Fk represents the force on the kth particle, which is located at position rk, and angle brackets represent the average over time of the enclosed quantity. The word virial for the right-hand side of the equation derives from vis, the Latin word for "force" or "energy", and was given its technical definition by Rudolf Clausius in 1870.[1]

The significance of the virial theorem is that it allows the average total kinetic energy to be calculated even for very complicated systems that defy an exact solution, such as those considered in statistical mechanics; this average total kinetic energy is related to the temperature of the system by the equipartition theorem. However, the virial theorem does not depend on the notion of temperature and holds even for systems that are not in thermal equilibrium. The virial theorem has been generalized in various ways, most notably to a tensor form.

If the force between any two particles of the system results from a potential energy V(r) = αrn that is proportional to some power n of the interparticle distance r, the virial theorem takes the simple form

${\displaystyle 2\langle T\rangle =n\langle V_{\text}\rangle .}$

Thus, twice the average total kinetic energy T equals n times the average total potential energy VTOT. Whereas V(r) represents the potential energy between two particles, VTOT represents the total potential energy of the system, i.e., the sum of the potential energy V(r) over all pairs of particles in the system. A common example of such a system is a star held together by its own gravity, where n equals −1.

Although the virial theorem depends on averaging the total kinetic and potential energies, the presentation here postpones the averaging to the last step.

## History

In 1870, Rudolf Clausius delivered the lecture "On a Mechanical Theorem Applicable to Heat" to the Association for Natural and Medical Sciences of the Lower Rhine, following a 20-year study of thermodynamics. The lecture stated that the mean vis viva of the system is equal to its virial, or that the average kinetic energy is equal to 1/2 the average potential energy. The virial theorem can be obtained directly from Lagrange's identity as applied in classical gravitational dynamics, the original form of which was included in Lagrange's "Essay on the Problem of Three Bodies" published in 1772. Karl Jacobi's generalization of the identity to N bodies and to the present form of Laplace's identity closely resembles the classical virial theorem. However, the interpretations leading to the development of the equations were very different, since at the time of development, statistical dynamics had not yet unified the separate studies of thermodynamics and classical dynamics.[2] The theorem was later utilized, popularized, generalized and further developed by James Clerk Maxwell, Lord Rayleigh, Henri Poincaré, Subrahmanyan Chandrasekhar, Enrico Fermi, Paul Ledoux and Eugene Parker. Fritz Zwicky was the first to use the virial theorem to deduce the existence of unseen matter, which is now called dark matter. As another example of its many applications, the virial theorem has been used to derive the Chandrasekhar limit for the stability of white dwarf stars.

## Statement and derivation

For a collection of N point particles, the scalar moment of inertia I about the origin is defined by the equation

${\displaystyle I=\sum _^m_\left|\mathbf _\right|^=\sum _^m_r_^}$

where mk and rk represent the mass and position of the kth particle. rk = |rk| is the position vector magnitude. The scalar G is defined by the equation

${\displaystyle G=\sum _^\mathbf _\cdot \mathbf _}$

where pk is the momentum vector of the kth particle. Assuming that the masses are constant, G is one-half the time derivative of this moment of inertia

${\displaystyle {\begin{\frac }{\frac }&={\frac }{\frac }\sum _^m_\mathbf _\cdot \mathbf _\\&=\sum _^m_\,{\frac _}}\cdot \mathbf _\\&=\sum _^\mathbf _\cdot \mathbf _=G\,.\end}}$

In turn, the time derivative of G can be written

${\displaystyle {\begin{\frac }&=\sum _^\mathbf _\cdot {\frac _}}+\sum _^{\frac _}}\cdot \mathbf _\\&=\sum _^m_{\frac _}}\cdot {\frac _}}+\sum _^\mathbf _\cdot \mathbf _\\&=2T+\sum _^\mathbf _\cdot \mathbf _\,\end}}$

where mk is the mass of the kth particle, Fk = dpk/dt is the net force on that particle, and T is the total kinetic energy of the system

${\displaystyle T={\frac }\sum _^m_v_^={\frac }\sum _^m_{\frac _}}\cdot {\frac _}}.}$

### Connection with the potential energy between particles

The total force Fk on particle k is the sum of all the forces from the other particles j in the system

${\displaystyle \mathbf _=\sum _^\mathbf _}$

where Fjk is the force applied by particle j on particle k. Hence, the virial can be written

${\displaystyle -{\frac }\,\sum _^\mathbf _\cdot \mathbf _=-{\frac }\,\sum _^\sum _^\mathbf _\cdot \mathbf _\,.}$

Since no particle acts on itself (i.e., Fjj = 0 for 1 ≤ jN), we split the sum in terms below and above this diagonal (proof of this equation):

${\displaystyle {\begin\sum _^\mathbf _\cdot \mathbf _&=\sum _^\sum _^\mathbf _\cdot \mathbf _+\sum _^\sum _^\mathbf _\cdot \mathbf _\\&=\sum _^\sum _^\mathbf _\cdot \left(\mathbf _-\mathbf _\right).\end}}$

where we have assumed that Newton's third law of motion holds, i.e., Fjk = −Fkj (equal and opposite reaction).

It often happens that the forces can be derived from a potential energy V that is a function only of the distance rjk between the point particles j and k. Since the force is the negative gradient of the potential energy, we have in this case

${\displaystyle \mathbf _=-\nabla _{\mathbf _}V=-{\frac }\left({\frac {\mathbf _-\mathbf _}}}\right),}$

which is equal and opposite to Fkj = −∇rjV, the force applied by particle k on particle j, as may be confirmed by explicit calculation. Hence,

${\displaystyle {\begin\sum _^\mathbf _\cdot \mathbf _&=\sum _^\sum _^\mathbf _\cdot \left(\mathbf _-\mathbf _\right)\\&=-\sum _^\sum _^{\frac }{\frac {|\mathbf _-\mathbf _|^}}}\\&=-\sum _^\sum _^{\frac }r_.\end}}$

Thus, we have

${\displaystyle {\frac }=2T+\sum _^\mathbf _\cdot \mathbf _=2T-\sum _^\sum _^{\frac }r_.}$

### Special case of power-law forces

In a common special case, the potential energy V between two particles is proportional to a power n of their distance r

${\displaystyle V\left(r_\right)=\alpha r_^,}$

where the coefficient α and the exponent n are constants. In such cases, the virial is given by the equation

${\displaystyle {\begin-{\frac }\,\sum _^\mathbf _\cdot \mathbf _&={\frac }\,\sum _^\sum _{\frac }r_\\&={\frac }\,\sum _^\sum _n\alpha r_^r_\\&={\frac }\,\sum _^\sum _nV\left(r_\right)={\frac }\,V_{\text}\end}}$

where VTOT is the total potential energy of the system

${\displaystyle V_{\text}=\sum _^\sum _V\left(r_\right)\,.}$

Thus, we have

${\displaystyle {\frac }=2T+\sum _^\mathbf _\cdot \mathbf _=2T-nV_{\text}\,.}$

For gravitating systems the exponent n equals −1, giving Lagrange's identity

${\displaystyle {\frac }={\frac }{\frac I}}}=2T+V_{\text}}$

which was derived by Joseph-Louis Lagrange and extended by Carl Jacobi.

### Time averaging

The average of this derivative over a time, τ, is defined as

${\displaystyle \left\langle {\frac }\right\rangle _{\tau }={\frac {\tau }}\int _^{\tau }{\frac }\,dt={\frac {\tau }}\int _^\,dG={\frac {\tau }},}$

from which we obtain the exact equation

${\displaystyle \left\langle {\frac }\right\rangle _{\tau }=2\left\langle T\right\rangle _{\tau }+\sum _^\left\langle \mathbf _\cdot \mathbf _\right\rangle _{\tau }.}$

The virial theorem states that if dG/dtτ = 0, then

${\displaystyle 2\left\langle T\right\rangle _{\tau }=-\sum _^\left\langle \mathbf _\cdot \mathbf _\right\rangle _{\tau }.}$

There are many reasons why the average of the time derivative might vanish, dG/dtτ = 0. One often-cited reason applies to stably-bound systems, that is to say systems that hang together forever and whose parameters are finite. In that case, velocities and coordinates of the particles of the system have upper and lower limits so that Gbound, is bounded between two extremes, Gmin and Gmax, and the average goes to zero in the limit of very long times τ:

${\displaystyle \lim _{\tau \rightarrow \infty }\left|\left\langle {\frac }}}\right\rangle _{\tau }\right|=\lim _{\tau \rightarrow \infty }\left|{\frac {\tau }}\right|\leq \lim _{\tau \rightarrow \infty }{\frac -G_{\min }}{\tau }}=0.}$

Even if the average of the time derivative of G is only approximately zero, the virial theorem holds to the same degree of approximation.

For power-law forces with an exponent n, the general equation holds:

${\displaystyle {\begin\langle T\rangle _{\tau }&=-{\frac }\sum _^\langle \mathbf _\cdot \mathbf _\rangle _{\tau }\\&={\frac }\langle V_{\text}\rangle _{\tau }.\end}}$

For gravitational attraction, n equals −1 and the average kinetic energy equals half of the average negative potential energy

${\displaystyle \langle T\rangle _{\tau }=-{\frac }\langle V_{\text}\rangle _{\tau }.}$

This general result is useful for complex gravitating systems such as solar systems or galaxies.

A simple application of the virial theorem concerns galaxy clusters. If a region of space is unusually full of galaxies, it is safe to assume that they have been together for a long time, and the virial theorem can be applied. Doppler effect measurements give lower bounds for their relative velocities, and the virial theorem gives a lower bound for the total mass of the cluster, including any dark matter.

If the ergodic hypothesis holds for the system under consideration, the averaging need not be taken over time; an ensemble average can also be taken, with equivalent results.

## In quantum mechanics

Although originally derived for classical mechanics, the virial theorem also holds for quantum mechanics, as first shown by Fock[3] using the Ehrenfest theorem.

Evaluate the commutator of the Hamiltonian

${\displaystyle H=V{\bigl (}\\}{\bigr )}+\sum _{\frac ^}}}$

with the position operator Xn and the momentum operator

${\displaystyle P_=-i\hbar {\frac }}}$

of particle n,

${\displaystyle [H,X_P_]=X_[H,P_]+[H,X_]P_=i\hbar X_{\frac }}-i\hbar {\frac ^}}~.}$

Summing over all particles, one finds for

${\displaystyle Q=\sum _X_P_}$

the commutator amounts to

${\displaystyle {\frac {\hbar }}[H,Q]=2T-\sum _X_{\frac }}}$

where ${\displaystyle T=\sum _{\frac ^}}}$ is the kinetic energy. The left-hand side of this equation is just dQ/dt, according to the Heisenberg equation of motion. The expectation value dQ/dt of this time derivative vanishes in a stationary state, leading to the quantum virial theorem,

${\displaystyle 2\langle T\rangle =\sum _\left\langle X_{\frac }}\right\rangle ~.}$

## Pokhozhaev's identity

Another form of the virial theorem Quantum Mechanics, applicable to localized solutions to the stationary nonlinear Schrödinger equation or Klein–Gordon equation, is Pokhozhaev's identity, also known as Derrick's theorem. Let ${\displaystyle g(s)}$ be continuous and real-valued, with ${\displaystyle g(0)=0}$. Denote ${\displaystyle G(s)=\int _^g(t)\,dt}$. Let

${\displaystyle u\in L_{\mathrm }^{\infty }(\mathbb ^),\qquad \nabla u\in L^(\mathbb ^),\qquad G(u(\cdot ))\in L^(\mathbb ^),\qquad n\in \mathbb ,}$

be a solution to the equation

${\displaystyle -\nabla ^u=g(u)}$,

in the sense of distributions. Then ${\displaystyle u}$ satisfies the relation

${\displaystyle (n-2)\int _{\mathbb ^}|\nabla u(x)|^\,dx=n\int _{\mathbb ^}G(u(x))\,dx.}$

## In special relativity

For a single particle in special relativity, it is not the case that T = 1/2p · v. Instead, it is true that T = (γ − 1) mc2, where γ is the Lorentz factor

${\displaystyle \gamma ={\frac {\sqrt }}}}}}}$

and β = v/c. We have,

${\displaystyle {\begin{\frac }\mathbf \cdot \mathbf &={\frac }{\boldsymbol {\beta }}\gamma mc\cdot {\boldsymbol {\beta }}c\\&={\frac }\gamma \beta ^mc^\\&=\left({\frac {\gamma \beta ^}}\right)T\,.\end}}$

The last expression can be simplified to

${\displaystyle \left({\frac }}}}\right)T\qquad {\text}\qquad \left({\frac {\gamma +1}}\right)T}$.

Thus, under the conditions described in earlier sections (including Newton's third law of motion, Fjk = −Fkj, despite relativity), the time average for N particles with a power law potential is

${\displaystyle {\frac }\left\langle V_{\mathrm }\right\rangle _{\tau }=\left\langle \sum _^\left({\frac ^}}}}\right)T_\right\rangle _{\tau }=\left\langle \sum _^\left({\frac {\gamma _+1}}}\right)T_\right\rangle _{\tau }\,.}$

In particular, the ratio of kinetic energy to potential energy is no longer fixed, but necessarily falls into an interval:

${\displaystyle {\frac }\rangle } }\rangle }}\in \left[1,2\right]\,,}$

where the more relativistic systems exhibit the larger ratios.

## Generalizations

Lord Rayleigh published a generalization of the virial theorem in 1903.[4] Henri Poincaré applied a form of the virial theorem in 1911 to the problem of determining cosmological stability.[5] A variational form of the virial theorem was developed in 1945 by Ledoux.[6] A tensor form of the virial theorem was developed by Parker,[7] Chandrasekhar[8] and Fermi.[9] The following generalization of the virial theorem has been established by Pollard in 1964 for the case of the inverse square law:[10][11]

${\displaystyle 2\lim \limits _{\tau \rightarrow +\infty }\langle T\rangle _{\tau }=\lim \limits _{\tau \rightarrow +\infty }\langle U\rangle _{\tau }\qquad {\text}\quad \lim \limits _{\tau \rightarrow +\infty }{\tau }^{-2}I(\tau )=0\,.}$

A boundary term otherwise must be added.[12]

## Inclusion of electromagnetic fields

The virial theorem can be extended to include electric and magnetic fields. The result is[13]

${\displaystyle {\frac }{\frac I}}}+\int _x_{\frac {\partial G_}{\partial t}}\,d^r=2(T+U)+W^{\mathrm }+W^{\mathrm }-\int x_(p_+T_)\,dS_,}$

where I is the moment of inertia, G is the momentum density of the electromagnetic field, T is the kinetic energy of the "fluid", U is the random "thermal" energy of the particles, WE and WM are the electric and magnetic energy content of the volume considered. Finally, pik is the fluid-pressure tensor expressed in the local moving coordinate system

${\displaystyle p_=\Sigma n^{\sigma }m^{\sigma }\langle v_v_\rangle ^{\sigma }-V_V_\Sigma m^{\sigma }n^{\sigma },}$

and Tik is the electromagnetic stress tensor,

${\displaystyle T_=\left({\frac {\varepsilon _E^}}+{\frac }}}\right)\delta _-\left(\varepsilon _E_E_+{\frac B_}{\mu _}}\right).}$

A plasmoid is a finite configuration of magnetic fields and plasma. With the virial theorem it is easy to see that any such configuration will expand if not contained by external forces. In a finite configuration without pressure-bearing walls or magnetic coils, the surface integral will vanish. Since all the other terms on the right hand side are positive, the acceleration of the moment of inertia will also be positive. It is also easy to estimate the expansion time τ. If a total mass M is confined within a radius R, then the moment of inertia is roughly MR2, and the left hand side of the virial theorem is MR2/τ2. The terms on the right hand side add up to about pR3, where p is the larger of the plasma pressure or the magnetic pressure. Equating these two terms and solving for τ, we find

${\displaystyle \tau \,\sim {\frac }}},}$

where cs is the speed of the ion acoustic wave (or the Alfvén wave, if the magnetic pressure is higher than the plasma pressure). Thus the lifetime of a plasmoid is expected to be on the order of the acoustic (or Alfvén) transit time.

## Relativistic uniform system

In case when in the physical system the pressure field, the electromagnetic and gravitational fields are taken into account, as well as the field of particles’ acceleration, the virial theorem is written in the relativistic form as follows:[14]

${\displaystyle \left\langle W_\right\rangle \approx -0.6\sum _^\langle \mathbf _\cdot \mathbf _\rangle ,}$

where the value WkγcT exceeds the kinetic energy of the particles T by a factor equal to the Lorentz factor γc of the particles at the center of the system. Under normal conditions we can assume that γc ≈ 1, then we can see that in the virial theorem the kinetic energy is related to the potential energy not by the coefficient 1/2, but rather by the coefficient close to 0.6. The difference from the classical case arises due to considering the pressure field and the field of particles’ acceleration inside the system, while the derivative of the scalar G is not equal to zero and should be considered as the material derivative.

An analysis of the integral theorem of generalized virial makes it possible to find, on the basis of field theory, a formula for the root-mean-square speed of typical particles of a system without using the notion of temperature:[15]

${\displaystyle v_{\mathrm }=c{\sqrt r^}\gamma _^\sin ^{\left({\frac }{\sqrt }}\right)}}}}},}$

where ${\displaystyle ~c}$ is the speed of light, ${\displaystyle ~\eta }$ is the acceleration field constant, ${\displaystyle ~\rho _}$ is the mass density of particles, ${\displaystyle ~r}$ is the current radius.

Unlike the virial theorem for particles, for the electromagnetic field the virial theorem is written as follows:[16]

${\displaystyle ~E_+2W_=0,}$

where the energy ${\displaystyle ~E_=\int j^{\alpha }{\sqrt {-g}}dx^dx^dx^}}$ considered as the kinetic field energy associated with four-current ${\displaystyle ~j^{\alpha }}$, and

${\displaystyle ~W_={\frac }}\int F^{\alpha \beta }{\sqrt {-g}}dx^dx^dx^}}$

sets the potential field energy found through the components of the electromagnetic tensor.

## In astrophysics

The virial theorem is frequently applied in astrophysics, especially relating the gravitational potential energy of a system to its kinetic or thermal energy. Some common virial relations are[citation needed]

${\displaystyle {\frac }{\frac }={\frac }{\frac }T} }}}={\frac }v^}$

for a mass M, radius R, velocity v, and temperature T. The constants are Newton's constant G, the Boltzmann constant kB, and proton mass mp. Note that these relations are only approximate, and often the leading numerical factors (e.g. 3/5 or 1/2) are neglected entirely.

### Galaxies and cosmology (virial mass and radius)

In astronomy, the mass and size of a galaxy (or general overdensity) is often defined in terms of the "virial mass" and "virial radius" respectively. Because galaxies and overdensities in continuous fluids can be highly extended (even to infinity in some models, such as an isothermal sphere), it can be hard to define specific, finite measures of their mass and size. The virial theorem, and related concepts, provide an often convenient means by which to quantify these properties.

In galaxy dynamics, the mass of a galaxy is often inferred by measuring the rotation velocity of its gas and stars, assuming circular Keplerian orbits. Using the virial theorem, the dispersion velocity σ can be used in a similar way. Taking the kinetic energy (per particle) of the system as T = 1/2v2 ~ 3/2σ2, and the potential energy (per particle) as U ~ 3/5 GM/R we can write

${\displaystyle {\frac }\approx \sigma ^.}$

Here ${\displaystyle R}$ is the radius at which the velocity dispersion is being measured, and M is the mass within that radius. The virial mass and radius are generally defined for the radius at which the velocity dispersion is a maximum, i.e.

${\displaystyle {\frac }}}}}\approx \sigma _{\max }^.}$

As numerous approximations have been made, in addition to the approximate nature of these definitions, order-unity proportionality constants are often omitted (as in the above equations). These relations are thus only accurate in an order of magnitude sense, or when used self-consistently.

An alternate definition of the virial mass and radius is often used in cosmology where it is used to refer to the radius of a sphere, centered on a galaxy or a galaxy cluster, within which virial equilibrium holds. Since this radius is difficult to determine observationally, it is often approximated as the radius within which the average density is greater, by a specified factor, than the critical density

${\displaystyle \rho _{\text}={\frac }}}$

where H is the Hubble parameter and G is the gravitational constant. A common choice for the factor is 200, which corresponds roughly to the typical over-density in spherical top-hat collapse (see Virial mass), in which case the virial radius is approximated as

${\displaystyle r_{\text}\approx r_=r,\qquad \rho =200\cdot \rho _{\text}.}$

The virial mass is then defined relative to this radius as

${\displaystyle M_{\text}\approx M_={\frac }\pi r_^\cdot 200\rho _{\text}.}$

### In stars

The virial theorem is applicable to the cores of stars, by establishing a relation between gravitational potential energy and thermal kinetic energy (i.e. temperature). As stars on the main sequence convert hydrogen into helium in their cores, the mean molecular weight of the core increases and it must contract to maintain enough pressure to supports its own weight. This contraction decreases its potential energy and, the virial theorem states, increases its thermal energy. The core temperature increases even as energy is lost, effectively a negative specific heat.[17] This continues beyond the main sequence, unless the core becomes degenerate since that causes the pressure to become independent of temperature and the virial relation with n equals −1 no longer holds.[18]

## References

1. ^ Clausius, RJE (1870). "On a Mechanical Theorem Applicable to Heat". Philosophical Magazine. Series 4. 40: 122–127. doi:10.1080/14786447008640370.
2. ^ Collins, G. W. (1978). "Introduction". The Virial Theorem in Stellar Astrophysics. Pachart Press. Bibcode:1978vtsa.book.....C. ISBN 978-0-912918-13-6.
3. ^ Fock, V. (1930). "Bemerkung zum Virialsatz". Zeitschrift für Physik A. 63 (11): 855–858. Bibcode:1930ZPhy...63..855F. doi:10.1007/BF01339281.
4. ^ Lord Rayleigh (1903). "Unknown". Cite journal requires |journal= (help)
5. ^ Poincaré, Henri. Lectures on Cosmological Theories. Paris: Hermann.
6. ^ Ledoux, P. (1945). "On the Radial Pulsation of Gaseous Stars". The Astrophysical Journal. 102: 143–153. Bibcode:1945ApJ...102..143L. doi:10.1086/144747.
7. ^ Parker, E.N. (1954). "Tensor Virial Equations". Physical Review. 96 (6): 1686–1689. Bibcode:1954PhRv...96.1686P. doi:10.1103/PhysRev.96.1686.
8. ^ Chandrasekhar, S; Lebovitz NR (1962). "The Potentials and the Superpotentials of Homogeneous Ellipsoids". Astrophys. J. 136: 1037–1047. Bibcode:1962ApJ...136.1037C. doi:10.1086/147456.
9. ^ Chandrasekhar, S; Fermi E (1953). "Problems of Gravitational Stability in the Presence of a Magnetic Field". Astrophys. J. 118: 116. Bibcode:1953ApJ...118..116C. doi:10.1086/145732.
10. ^ Pollard, H. (1964). "A sharp form of the virial theorem". Bull. Amer. Math. Soc. LXX (5): 703–705. doi:10.1090/S0002-9904-1964-11175-7.
11. ^ Pollard, Harry (1966). Mathematical Introduction to Celestial Mechanics. Englewood Cliffs, NJ: Prentice–Hall, Inc. ISBN 978-0-13-561068-8.
12. ^ Kolár, M.; O'Shea, S. F. (July 1996). "A high-temperature approximation for the path-integral quantum Monte Carlo method". Journal of Physics A: Mathematical and General. 29 (13): 3471–3494. Bibcode:1996JPhA...29.3471K. doi:10.1088/0305-4470/29/13/018.
13. ^ Schmidt, George (1979). Physics of High Temperature Plasmas (Second ed.). Academic Press. p. 72.
14. ^ Fedosin, S. G. (2016). "The virial theorem and the kinetic energy of particles of a macroscopic system in the general field concept". Continuum Mechanics and Thermodynamics. 29 (2): 361–371. arXiv:1801.06453. Bibcode:2017CMT....29..361F. doi:10.1007/s00161-016-0536-8.
15. ^ Fedosin, Sergey G. (2018-09-24). "The integral theorem of generalized virial in the relativistic uniform model". Continuum Mechanics and Thermodynamics. 31 (3): 627–638. Bibcode:2018CMT...tmp..140F. doi:10.1007/s00161-018-0715-x. ISSN 1432-0959 – via Springer Nature SharedIt.
16. ^ Fedosin S.G. The Integral Theorem of the Field Energy. Gazi University Journal of Science. Vol. 32, No. 2, pp. 686-703 (2019). https://doi.org/10.5281/zenodo.3252783.
17. ^ BAIDYANATH BASU; TANUKA CHATTOPADHYAY; SUDHINDRA NATH BISWAS (1 January 2010). AN INTRODUCTION TO ASTROPHYSICS. PHI Learning Pvt. Ltd. pp. 365–. ISBN 978-81-203-4071-8.
18. ^ William K. Rose (16 April 1998). Advanced Stellar Astrophysics. Cambridge University Press. pp. 242–. ISBN 978-0-521-58833-1.