Gravitational Binding Energy
Get Gravitational Binding Energy essential facts below. View Videos or join the Gravitational Binding Energy discussion. Add Gravitational Binding Energy to your PopFlock.com topic list for future reference or share this resource on social media.
Gravitational Binding Energy
Galaxy clusters are the largest known gravitationally bound structures in the universe.[1]

A gravitational binding energy is the minimum energy that must be added to a system for the system to cease being in a gravitationally bound state. A gravitationally bound system has a lower (i.e., more negative) gravitational potential energy than the sum of its parts--this is what keeps the system aggregated in accordance with the minimum total potential energy principle.

For a spherical mass of uniform density, the gravitational binding energy U is given by the formula[2][3]

${\displaystyle U={\frac {3GM^{2}}{5R}}}$

where G is the gravitational constant, M is the mass of the sphere, and R is its radius.

Assuming that the Earth is a uniform sphere (which is not correct, but is close enough to get an order-of-magnitude estimate) with M = 5.97 x 1024 kg and r = 6.37 x 106 m, U is 2.24 x 1032 J. This is roughly equal to one week of the Sun's total energy output. It is 37.5 MJ/kg, 60% of the absolute value of the potential energy per kilogram at the surface.

The actual depth-dependence of density, inferred from seismic travel times (see Adams-Williamson equation), is given in the Preliminary Reference Earth Model (PREM).[4] Using this, the real gravitational binding energy of Earth can be calculated numerically as U = 2.487 x 1032 J.

According to the virial theorem, the gravitational binding energy of a star is about two times its internal thermal energy in order for hydrostatic equilibrium to be maintained.[2] As the gas in a star becomes more relativistic, the gravitational binding energy required for hydrostatic equilibrium approaches zero and the star becomes unstable (highly sensitive to perturbations), which may lead to a supernova in high-mass stars due to strong radiation pressure or black holes in neutron stars.

## Derivation for a uniform sphere

The gravitational binding energy of a sphere with radius ${\displaystyle R}$ is found by imagining that it is pulled apart by successively moving spherical shells to infinity, the outermost first, and finding the total energy needed for that.

Assuming a constant density ${\displaystyle \rho }$, the masses of a shell and the sphere inside it are:

${\displaystyle m_{\mathrm {shell} }=4\pi r^{2}\rho \,dr}$      and      ${\displaystyle m_{\mathrm {interior} }={\frac {4}{3}}\pi r^{3}\rho }$

The required energy for a shell is the negative of the gravitational potential energy:

${\displaystyle {\it {dU}}=-G{\frac {m_{\mathrm {shell} }m_{\mathrm {interior} }}{r}}}$

Integrating over all shells yields:

${\displaystyle U=-G\int _{0}^{R}{\frac {(4\pi r^{2}\rho )({\tfrac {4}{3}}\pi r^{3}\rho )}{r}}dr=-G{\frac {16}{3}}\pi ^{2}\rho ^{2}\int _{0}^{R}{r^{4}}dr=-G{\frac {16}{15}}{\pi }^{2}{\rho }^{2}R^{5}}$

Since ${\displaystyle \rho }$ is simply equal to the mass of the whole divided by its volume for objects with uniform density, therefore

${\displaystyle \rho ={\frac {M}{{\frac {4}{3}}\pi R^{3}}}}$

And finally, plugging this into our result leads to

${\displaystyle U=-G{\frac {16}{15}}\pi ^{2}R^{5}\left({\frac {M}{{\frac {4}{3}}\pi R^{3}}}\right)^{2}=-{\frac {3GM^{2}}{5R}}}$

## Negative mass component

Two bodies, placed at the distance R from each other, exert a gravitational force on a third body slightly smaller when R is small. This can be seen as a negative mass component of the system, equal, for uniformly spherical solutions, to:

${\displaystyle M_{\mathrm {binding} }=-{\frac {3GM^{2}}{5Rc^{2}}}}$

It can be easily demonstrated that this negative component can never exceed the positive component of a system. A negative binding energy greater than the mass of the system itself would indeed require that the radius of the system be smaller than:

${\displaystyle R\leq {\frac {3GM}{5c^{2}}}}$

which is ${\displaystyle {\frac {3}{10}}}$ smaller than its Schwarzschild radius:

${\displaystyle R\leq {\frac {3}{10}}r_{\mathrm {s} }}$

and therefore never visible to an external observer.

## Non-uniform spheres

Planets and stars have radial density gradients from their lower density surfaces to their much larger density compressed cores. Degenerate matter objects (white dwarfs; neutron star pulsars) have radial density gradients plus relativistic corrections.

Neutron star relativistic equations of state provided by Jim Lattimer include a graph of radius vs. mass for various models.[5] The most likely radii for a given neutron star mass are bracketed by models AP4 (smallest radius) and MS2 (largest radius). BE is the ratio of gravitational binding energy mass equivalent to observed neutron star gravitational mass of "M" kilograms with radius "R" meters,

${\displaystyle BE={\frac {0.60\,\beta }{1-{\frac {\beta }{2}}}}}$      ${\displaystyle \beta \ =G\,M/R\,{c}^{2}}$

Given current values

${\displaystyle G=6.6742\times 10^{-11}\,m^{3}kg^{-1}sec^{-2}}$ [6]
${\displaystyle c^{2}=8.98755\times 10^{16}\,m^{2}sec^{-2}}$
${\displaystyle M_{solar}=1.98844\times 10^{30}\,kg}$

and star masses "M" commonly reported as multiples of one solar mass,

${\displaystyle M_{x}={\frac {M}{M_{\odot }}}}$

then the relativistic fractional binding energy of a neutron star is

${\displaystyle BE={\frac {885.975\,M_{x}}{R-738.313\,M_{x}}}}$

## References

1. ^ "Spot the cluster". www.eso.org. Retrieved 2017.
2. ^ a b Chandrasekhar, S. 1939, An Introduction to the Study of Stellar Structure (Chicago: U. of Chicago; reprinted in New York: Dover), section 9, eqs. 90-92, p. 51 (Dover edition)
3. ^ Lang, K. R. 1980, Astrophysical Formulae (Berlin: Springer Verlag), p. 272
4. ^ Dziewonski, A. M.; Anderson, D. L. "Preliminary Reference Earth Model". Physics of the Earth and Planetary Interiors. 25: 297-356. Bibcode:1981PEPI...25..297D. doi:10.1016/0031-9201(81)90046-7.
5. ^ Neutron Star Masses and Radii, p. 9/20, bottom
6. ^ Measurement of Newton's Constant Using a Torsion Balance with Angular Acceleration FeedbackArchived 2011-04-19 at the Wayback Machine, Phys. Rev. Lett. 85(14) 2869 (2000)