Non-relativistic gravitational fields explained

Within general relativity (GR), Einstein's relativistic gravity, the gravitational field is described by the 10-component metric tensor. However, in Newtonian gravity, which is a limit of GR, the gravitational field is described by a single component Newtonian gravitational potential. This raises the question to identify the Newtonian potential within the metric, and to identify the physical interpretation of the remaining 9 fields.

The definition of the non-relativistic gravitational fields provides the answer to this question, and thereby describes the image of the metric tensor in Newtonian physics. These fields are not strictly non-relativistic. Rather, they apply to the non-relativistic (or post-Newtonian) limit of GR.

\phi ^{EM} and the magnetic vector potential \vec{A}{} ^{EM} . Together, they combine into the 4-vector potential A ^{EM} _{\mu} \leftrightarrow (\phi ^{EM,} \vec{A}{} ^{EM)} , which is compatible with relativity. This relation can be thought to represent the non-relativistic decomposition of the electromagnetic 4-vector potential. Indeed, a system of point-particle charges moving slowly with respect to the speed of light may be studied in an expansion in v ^{2/c} ^{2} , where v is a typical velocity and c is the speed of light. This expansion is known as the post-Coulombic expansion. Within this expansion, \phi ^{EM} contributes to the two-body potential already at 0th order, while \vec{A} ^{EM} contributes only from the 1st order and onward, since it couples to electric currents and hence the associated potential is proportional to v ^{2/c} ^{2} .

Definition

In the non-relativistic limit, of weak gravity and non-relativistic velocities, general relativity reduces to Newtonian gravity. Going beyond the strict limit, corrections can be organized into a perturbation theory known as the post-Newtonian expansion. As part of that, the metric gravitational field

g _{\mu\nu} , \mu, \nu = 0 , 1 , 2 , 3 , is redefined and decomposed into the non-relativistic gravitational (NRG) fields g _{\mu\nu} \leftrightarrow ( \phi, \vec{A}, \sigma _{ij} ) : \phi is the Newtonian potential, \vec{A} is known as the gravito-magnetic vector potential, and finally \sigma _{ij} is a 3d symmetric tensor known as the spatial metric perturbation. The field redefinition is given by^[1] $$ds^2\backslash equiv\; g\_dx^\backslash mu\; dx^\backslash nu\; =\; e^(dt-2\backslash ,\; \backslash vec\; \backslash cdot\; d\backslash vec)^2-e^(\backslash delta\_\; +\; \backslash sigma\_)\backslash ,\; dx^i\backslash ,\; dx^j.$$In components, this is equivalent towhere i, j = 1 , 2 , 3 .

Counting components,

g _{\mu\nu} has 10, while \phi has 1, \vec{A} has 3 and finally \sigma _{ij} has 6. Hence, in terms of components, the decomposition reads 10 = 1 + 3 + 6 .

Motivation for definition

In the post-Newtonian limit, bodies move slowly compared with the speed of light, and hence the gravitational field is also slowly changing. Approximating the fields to be time independent, the Kaluza-Klein reduction (KK) was adapted to apply to the time direction. Recall that in its original context, the KK reduction applies to fields which are independent of a compact spatial fourth direction. In short, the NRG decomposition is a Kaluza-Klein reduction over time.

The definition was essentially introduced in, interpreted in the context of the post-Newtonian expansion in,^[2] and finally the normalization of

\vec{A} was changed in ^[3] to improve the analogy between a spinning object and a magnetic dipole.

Relation with standard approximations

By definition, the post-Newtonian expansion assumes a weak field approximation. Within the first order perturbation to the metric

g _{\mu} = η _{\mu} + h _{\mu} , where η _{\mu} is the Minkowski metric, we find the standard weak field decomposition into a scalar, vector and tensor h _{\mu\nu} \to \left( h _{00} , h _{0i} , h _{ij} \right) , which is similar to the non-relativistic gravitational (NRG) fields. The importance of the NRG fields is that they provide a non-linear extension, thereby facilitating computation at higher orders in the weak field / post-Newtonian expansion. Summarizing, the NRG fields are adapted for higher order post-Newtonian expansion.

Physical interpretation

The scalar field

\phi is interpreted as the Newtonian gravitational potential.

The vector field

\vec{A} is interpreted as the gravito-magnetic vector potential. It is magnetic-like, or analogous to the magnetic vector potential in electromagnetism (EM). In particular, it is sourced by massive currents (the analogue of charge currents in EM), namely by momentum.

As a result, the gravito-magnetic vector potential is responsible for current-current interaction, which appears at the 1st post-Newtonian order. In particular, it generates a repulsive contribution to the force between parallel massive currents. However, this repulsion is overturned by the standard Newtonian gravitational attraction, since in gravity a current "wire" must always be massive (charged) -- unlike EM.

A spinning object is the analogue of an electromagnetic current loop, which forms as magnetic dipole, and as such it creates a magnetic-like dipole field in

\vec{A} .

The symmetric tensor

\sigma _{ij} is known as the spatial metric perturbation. From the 2nd post-Newtonian order and onward, it must be accounted for. If one restricts to the 1st post-Newtonian order, \sigma _{ij} can be ignored, and relativistic gravity is described by the \phi , \vec{A} fields. Hence it becomes a strong analogue of electromagnetism, an analogy known as gravitoelectromagnetism.

Applications and generalizations

The two body problem in general relativity holds both intrinsic interest and observational, astrophysical interest. In particular, it is used to describe the motion of binary compact objects, which are the sources for gravitational waves. As such, the study of this problem is essential for both detection and interpretation of gravitational waves.

Within this two body problem, the effects of GR are captured by the two body effective potential, which is expanded within the post-Newtonian approximation. Non-relativistic gravitational fields were found to economize the determination of this two body effective potential.^{[4] [5] [6]}

Generalizations

In higher dimensions, with an arbitrary spacetime dimension

d , the definition of non-relativistic gravitational fields generalizes into

$$ds^2\; =\; e^(dt-2\backslash ,\; \backslash vec\; \backslash cdot\; d\backslash vec)^2-e^(\backslash delta\_\; +\; \backslash sigma\_)\; dx^i\; dx^j$$Substituting

d =4 reproduces the standard 4d definition above.

See also

• Non-relativistic spacetime

References

1. Kol . Barak . Smolkin . Michael . 2008-03-28 . eq. (2.6) . Classical Effective Field Theory and Caged Black Holes . Physical Review D . 77 . 6 . 064033 . 0712.2822 . 10.1103/PhysRevD.77.064033 . 2008PhRvD..77f4033K . 16299713 . 1550-7998.
2. Kol . Barak . Smolkin . Michael . 2008-07-21 . Non-Relativistic Gravitation: From Newton to Einstein and Back . Classical and Quantum Gravity . 25 . 14 . 145011 . 0712.4116 . 10.1088/0264-9381/25/14/145011 . 2008CQGra..25n5011K . 119216835 . 0264-9381.
3. Birnholtz . Ofek . Hadar . Shahar . Kol . Barak . 2013 . eq. (A.10) . Theory of post-Newtonian radiation and reaction . Phys. Rev. D . 88 . 10 . 104037 . 1305.6930 . 10.1103/PhysRevD.88.104037. 2013PhRvD..88j4037B . 119170985 .
4. Gilmore . James B. . Ross . Andreas . 2008-12-30 . Effective field theory calculation of second post-Newtonian binary dynamics . Physical Review D . 78 . 12 . 124021 . 0810.1328 . 10.1103/PhysRevD.78.124021 . 2008PhRvD..78l4021G . 119271832 . 1550-7998.
5. Foffa . S. . Sturani . R. . 2011-08-09 . Effective field theory calculation of conservative binary dynamics at third post-Newtonian order . Physical Review D . 84 . 4 . 044031 . 10.1103/PhysRevD.84.044031 . 1104.1122 . 2011PhRvD..84d4031F . 119234031 . 1550-7998.
6. Blanchet . Luc . 2014 . Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries . Living Reviews in Relativity . 17 . 1 . 2 . 1310.1528 . 10.12942/lrr-2014-2 . free . 28179846 . 5256563 . 2014LRR....17....2B . 2367-3613.