# Physics/Essays/Fedosin/Gravitational characteristic impedance of free space

Gravitational characteristic impedance of free space, $\rho _{g0}\$ is a physical constant that according to Maxwell-like gravitational equations relates magnitudes of gravitational field strength $\mathbf {\Gamma }$ and gravitational torsion field $\mathbf {\Omega }$ in gravitational radiation travelling through free space:
    $\rho _{g0}={\sqrt {\frac {\mu _{g0}}{\varepsilon _{g}}}}={\frac {4\pi G}{c}}={\frac {\mu _{g0}\Gamma }{\Omega }}=2.796696\cdot 10^{-18}\mathrm {m^{2}/(s\cdot kg)} .\$
where $~\varepsilon _{g}={\frac {1}{4\pi G}}=1.192708\cdot 10^{9}\mathrm {kg\cdot s^{2}\cdot m^{-3}}$ is gravitoelectric gravitational constant in the set of selfconsistent gravitational constants, $~G$ is gravitational constant, c is speed of light, $\mu _{g0}={\frac {4\pi G}{c^{2}}}=9.328772\cdot 10^{-27}\mathrm {m/kg} \$ is gravitomagnetic gravitational constant.
As in electromagnetism, the characteristic impedance of free space plays a central role in all radiation problems, such as in a comparison of the radiation resistance of gravity-wave antennas to the value of this impedance in order to estimate the coupling efficiency of these antennas to free space. The numerical value of this impedance is extremely small, but the impedance of all material objects must be “impedance matched” to this extremely small quantity before significant power can be transferred efficiently from gravitational waves to these detectors.
The gravitational characteristic impedance of free space may be connected with other constants:
    $\rho _{g0}=2\alpha \cdot {\frac {h}{m_{S}^{2}}},\$
where $h\$ is the Planck constant, $\alpha ={\frac {e^{2}}{2\varepsilon _{0}hc}}$ is the fine structure constant for the elementary charge $e\$, $\varepsilon _{0}$ is the electric constant, $m_{S}=e{\sqrt {\frac {\varepsilon _{g}}{\varepsilon _{0}}}}={\frac {e}{\sqrt {4\pi G\varepsilon _{0}}}}\$ is the Stoney mass.
The gravitational characteristic impedance of free space for the atoms and nucleons level of matter is:
    $\rho _{s}={\frac {4\pi G_{s}}{c}}=6.346\cdot 10^{21}\mathrm {m^{2}/(s\cdot kg)} ,\$
where $G_{s}={\frac {e^{2}}{4\pi \varepsilon _{0}m_{p}m_{e}}}$ is the strong gravitational constant, $m_{p}$ and $m_{e}$ are the masses of proton and electron.

## History

Due to McDonald first who used Maxwell equations to describe gravity was Oliver Heaviside. The point is that in the weak gravitational field the standard theory of gravity could be written in the form of Maxwell-like gravitational equations.
In the 80-ties Maxwell-like equations were considered in the Wald book of general relativity. In the 90-ties Kraus first introduced the gravitational characteristic impedance of free space, which was detailed later by Kiefer, and now by Raymond Y. Chiao, who is developing the ways of experimental determination of the gravitational waves.

## Typical gravitational impedance at the megascopic scale

In the general case only planets (with their sattelites) and stars could be considered "as free, as possible" to be used as some "antenna" to the gravitational waves detection. Spherical megascopic bodies have the folloving characteristic impedance:
    $\rho _{gs}\approx {\frac {vr}{3m}},\$
where
    $v\$ is the equatorial velocity,
    $r\$ is the spherical body radius and
    $m\$ is the body mass.

### Solar planetary system

Planetary data were taken from the textbook. As could be seen from the Table, only the Mercury has characteristic impedance close to the free space value.

### Planet's satellites

Satellites' data were taken from the textbook. As could be seen from the Table, only the Moon has the closest value of characteristic impedance about 12-times greater then for free space.

### Stars

In this table designations "O5" and "F5" define stellar types. As it is seen from the Table, some stars could have characteristic impedance value about the same as the impedance of free space.