In general relativity, the quadrupole formula describes the rate at which gravitational waves are emitted from a system of masses based on the change of the (mass) quadrupole moment. The formula reads
\bar{h}ij(t,r)=
2G | |
c4r |
\ddot{I}ij(t-r/c),
\bar{h}ij
G
c
Iij
It is useful to express the gravitational wave strain in the transverse traceless gauge, which is given by a similar formula where
T | |
I | |
ij |
T | |
{I} | |
ij |
=\int\rho(x)\left[rirj-
1 | |
3 |
r2\deltaij\right]d3r,
The total energy (luminosity) carried away by gravitational waves is
dE | |
dt |
=\sumij
G | |
5c5 |
\left(
| |||||||||||||
dt3 |
\right)2
The formula was first obtained by Albert Einstein in 1918. After a long history of debate on its physical correctness, observations of energy loss due to gravitational radiation in the Hulse–Taylor binary discovered in 1974 confirmed the result, with agreement up to 0.2 percent (by 2005).[2]