In mechanics, the virial theorem provides a general equation that relates the average over time of the total kinetic energy, , of a stable system consisting of N particles, bound by potential forces, with that of the total potential energy, , where angle brackets represent the average over time of the enclosed quantity. Mathematically, the theorem states
where Fk represents the force on the kth particle, which is located at position rk. The word "virial" derives from vis, the Latin word for "force" or "energy", and was given its technical definition by Rudolf Clausius in 1870.
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) = αr n that is proportional to some power n of the inter-particle distance r, the virial theorem takes the simple form
Thus, twice the average total kinetic energy equals n times the average total potential energy . 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.
- 1 History
- 2 Statement and derivation
- 3 In special relativity
- 4 Generalizations
- 5 Inclusion of electromagnetic fields
- 6 In astrophysics
- 7 See also
- 8 References
- 9 Further reading
- 10 External links
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. 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
Definitions of the virial and its time derivative
where mk and rk represent the mass and position of the kth particle. rk=|rk| is the position vector magnitude. The scalar virial G is defined by the equation
In turn, the time derivative of the virial G can be written
where mk is the mass of the k-th particle, is the net force on that particle, and T is the total kinetic energy of the system
Connection with the potential energy between particles
The total force on particle k is the sum of all the forces from the other particles j in the system
where is the force applied by particle j on particle k. Hence, the force term of the virial time derivative can be written
Since no particle acts on itself (i.e., whenever ), we have
where we have assumed that Newton's third law of motion holds, i.e., (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
which is clearly equal and opposite to , the force applied by particle on particle j, as may be confirmed by explicit calculation. Hence, the force term of the virial time derivative is
Thus, we have
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
where the coefficient α and the exponent n are constants. In such cases, the force term of the virial time derivative is given by the equation
where VTOT is the total potential energy of the system
Thus, we have
For gravitating systems the exponent n equals −1, giving Lagrange's identity
which was derived by Lagrange and extended by Jacobi.
The average of this derivative over a time, τ, is defined as
from which we obtain the exact equation
The virial theorem states that, if , then
There are many reasons why the average of the time derivative might vanish, i.e., . One often-cited reason applies to stably bound systems, i.e., 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 the virial, Gbound, is bounded between two extremes, Gmin and Gmax, and the average goes to zero in the limit of very long times τ
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
For gravitational attraction, n equals −1 and the average kinetic energy equals half of the average negative potential energy
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 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.
The averaging need not be taken over time; an ensemble average can also be taken, with equivalent results.
Although derived for classical mechanics, the virial theorem also holds for quantum mechanics, which was proved by Fock (the quantum equivalent of the l.h.s. vanishes for energy eigenstates).
In special relativity
For a single particle in special relativity, it is not the case that . Instead, it is true that and
The last expression can be simplified to either or .
Thus, under the conditions described in earlier sections (including Newton's third law of motion, , despite relativity), the time average for particles with a power law potential is
In particular, the ratio of kinetic energy to potential energy is no longer fixed, but necessarily falls into an interval:
where the more relativistic systems exhibit the larger ratios.
Lord Rayleigh published a generalization of the virial theorem in 1903. Henri Poincaré applied a form of the virial theorem in 1911 to the problem of determining cosmological stability. A variational form of the virial theorem was developed in 1945 by Ledoux. A tensor form of the virial theorem was developed by Parker, Chandrasekhar and Fermi. The following generalization of the virial theorem has been established by Pollard in 1964 for the case of the inverse square law: the statement is true if and only if A boundary term otherwise must be added, such as in Ref.
Inclusion of electromagnetic fields
The virial theorem can be extended to include electric and magnetic fields. The result is
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
and Tik is the electromagnetic stress tensor,
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
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.
for a mass , radius , velocity , and temperature . And the constants are Newton's constant , the Boltzmann constant , and proton mass . 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 radius" and "virial mass" respectively. Because galaxies and overdensities in continuous fluids can be highly extended (even to infinity in some models—e.g. 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 can be used in a similar way. Taking the kinetic energy (per particle) of the system as, , and the potential energy (per particle) as, U ~ (3/5)(GM/R), we can write
Here is the radius at which the velocity dispersion is being measured, and 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.
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, . Where is the Hubble parameter and is the gravitational constant. A common (although mostly arbitrary) choice for the factor is 200, in which case the virial radius is approximated as . The virial mass is then defined relative to this radius as .
- Virial coefficient
- Virial stress
- Virial mass
- Derrick's theorem (Pohozaev's identity)
- Equipartition theorem
- Clausius, RJE (1870). "On a Mechanical Theorem Applicable to Heat". Philosophical Magazine, Ser. 4 40: 122–127.
- Collins, G. W. (1978). The Virial Theorem in Stellar Astrophysics. Pachart Press. Introduction
- Proof of this equation
- Fock, V. (1930). "Bemerkung zum Virialsatz". Zeitschrift für Physik A 63 (11): 855–858. Bibcode:1930ZPhy...63..855F. doi:10.1007/BF01339281.
- Lord Rayleigh (1903). Unknown.
- Poincaré, H. Lectures on Cosmological Theories. Paris: Hermann.
- Ledoux, P. (1945). "On the Radial Pulsation of Gaseous Stars". The Astrophysical Journal 102: 143–153. Bibcode:1945ApJ...102..143L. doi:10.1086/144747. Retrieved March 24, 2012.
- Parker, E.N. (1954). "Tensor Virial Equations" (PDF). Physical Review 96 (6): 1686–1689. Bibcode:1954PhRv...96.1686P. doi:10.1103/PhysRev.96.1686. Retrieved March 24, 2012.
- Chandrasekhar, S; Lebovitz NR (1962). "The Potentials and the Superpotentials of Homogeneous Ellipsoids" (PDF). Ap. J. 136: 1037–1047. Bibcode:1962ApJ...136.1037C. doi:10.1086/147456. Retrieved March 24, 2012.
- Chandrasekhar, S; Fermi E (1953). "Problems of Gravitational Stability in the Presence of a Magnetic Field" (PDF). Ap. J. 118: 116. Bibcode:1953ApJ...118..116C. doi:10.1086/145732. Retrieved March 24, 2012.
- Pollard, H. (1964). "A sharp form of the virial theorem" (PDF). Bull. Amer. Math. Soc. LXX (5): 703–705. doi:10.1090/S0002-9904-1964-11175-7. Retrieved March 24, 2012.
- Pollard, Harry (1966). Mathematical Introduction to Celestial Mechanics. Englewood Cliffs, NJ: Prentice–Hall, Inc.
- Kolár, M.; O'Shea, S. F. (July 1996). "A high-temperature approximation for the path-integral quantum Monte Carlo method" (PDF). Journal of Physics A: Mathematical and General 29 (13): 3471–3494. Bibcode:1996JPhA...29.3471K. doi:10.1088/0305-4470/29/13/018. Retrieved March 24, 2012.
- Schmidt, George (1979). Physics of High Temperature Plasmas (Second ed.). Academic Press. p. 72.
- Goldstein, H. (1980). Classical Mechanics (2nd ed.). Addison–Wesley. ISBN 0-201-02918-9.
- Collins, G. W. (1978). The Virial Theorem in Stellar Astrophysics. Pachart Press.