**International Journal of Astronomy and Astrophysics**

Vol.08 No.03(2018), Article ID:87161,8 pages

10.4236/ijaa.2018.83019

Possibility of Classical Entanglement at LIGO

Partha Ghose^{1}, A. K. Rajagopal^{2 }

^{1}National Academy of Sciences, India, Allahabad, India

^{2}Inspire Institute Inc., Alexandria, USA

Copyright © 2018 by authors and Scientific Research Publishing Inc.

This work is licensed under the Creative Commons Attribution International License (CC BY 4.0).

http://creativecommons.org/licenses/by/4.0/

Received: July 11, 2018; Accepted: September 3, 2018; Published: September 6, 2018

ABSTRACT

It is now established that entanglement in the sense of local non-factorizability of two or more degrees of freedom of a system occurs in classical polarization optics. We extend the idea to weak gravitational waves which are strikingly similar to optical waves. It is shown that a linearized classical gravity wave can in principle get entangled in the sense mentioned with the vibrational modes of an array of test masses in a plane perpendicular to its direction of propagation. A Bell-CHSH inequality based on the requirement of noncontextuality for classical realism is derived, and it is shown that the putative nonfactorizable state violates this inequality. The idea is therefore empirically falsifiable.

**Keywords:**

Entanglement, Classical Optics, Gravitational Waves

1. Introduction

It is fairly well established by now that entanglement in the sense of local nonfactorizability of two or more degrees of freedom occurs in classical polarization optics [1] [2] [3] [4] [5] . Entanglement in this sense depends only on the physical existence of orthogonal Hilbert spaces, such as the polarization and propagation modes of light. Entanglement per se is not exclusive to quantum mechanics. In fact, the Schmidt decomposition theorem on which bipartite entanglement is based is pre-quantum mechanical [6] . This idea of entanglement can be extended to weak gravitational wave physics which has a striking similarity to classical polarization optics. In fact, the only difference is in the structure of polarization. Hence entanglement can, in principle, occur between the polarization modes of the gravitational wave and the vibrational modes of an array of masses which span orthogonal Hilbert spaces, and are therefore subject to the Schmidt theorem. The purpose of the paper is to point to such a possibility at LIGO, and propose how to test if it really occurs.

Section 2 gives a quick summary of gravitational wave physics relevant for our purpose. In Section 3 we show how the putative entanglement can occur at LIGO. In Section 4 we deduce a Bell-CHSH type inequality based on classical realism and noncontextuality, and show that the entangled state violates this inequality.

2. Introduction: Gravitational Waves and Polarization

For weak gravitational fields Einstein’s equation

${R}_{\mu \nu}=-8\text{\pi}G\left({T}_{\mu \nu}-\frac{1}{2}{g}_{\mu \nu}{T}_{\lambda}^{\lambda}\right)$ (1)

can be linearized by writing the metric in the form

${g}_{\mu \nu}\left(x\right)={\eta}_{\mu \nu}+{h}_{\mu \nu}\left(x\right)$ (2)

where ${\eta}_{\mu \nu}$ is the flat Minkowski metric and ${h}_{\mu \nu}\ll 1$ is a small perturbation. To the lowest order in the perturbation the vacuum equation ${R}_{\mu \nu}=0$ is then of the linearized form [7] [8] [9]

$\square {h}_{\mu \nu}-{\partial}_{\mu}{\xi}_{\nu}-{\partial}_{\nu}{\xi}_{\mu}=0$ (3)

where $\square \text{\hspace{0.17em}}={\eta}^{\alpha \beta}{\partial}_{\alpha \beta}=-{\partial}^{2}/\partial {t}^{2}+{\nabla}^{2}$ and

${\xi}_{\mu}={\partial}_{\gamma}{h}_{\mu}^{\gamma}-\frac{1}{2}{\partial}_{\mu}{h}_{\gamma}^{\gamma}.$ (4)

This equation can be written in the form

$\square {h}_{\mu \nu}=\mathrm{0,}$ (5)

${\partial}_{\nu}{h}_{\mu}^{\nu}\left(x\right)-\frac{1}{2}{\partial}_{\mu}{h}_{\nu}^{\nu}=\mathrm{0,}$ (6)

where the first equation is the linearized Einstein equation and the second equation is the Lorentz gauge constraint, where ${h}_{\nu}^{\gamma}\equiv {\eta}^{\gamma \delta}{h}_{\delta \nu}$ . A general solution is of the form

${h}_{\mu \nu}\left(x\right)\mathrm{=}{\alpha}_{\mu \nu}{\text{e}}^{i{k}_{\lambda}{x}^{\lambda}}+{\alpha}_{\mu \nu}^{\mathrm{*}}{\text{e}}^{-i{k}_{\lambda}{x}^{\lambda}}$ (7)

with ${k}_{\mu}^{\mu}=0$ , ${k}^{\mu}={\eta}^{\mu \nu}{k}_{\nu}$ , where ${\alpha}_{\mu \nu}$ is the polarization tensor which is symmetric in $\left(\mu \mathrm{,}\nu \right)$ and so has ten components, but this number can be reduced to two by making use of Bianchi identities and fixing the gauge.

In the transverse-traceless gauge (TT gauge) the metric perturbation is made purely spatial by requiring ${h}_{tt}={h}_{ti}=0$ and also traceless, ${h}_{i}^{\text{\hspace{0.05em}}\text{\hspace{0.05em}}i}=0$ . Then the Lorentz gauge constraint (6) becomes

${\partial}_{i}{h}_{ij}=0,$ (8)

which ensures transversality. For propagation in the z direction with a fixed frequency $\omega $ and ${k}^{\mu}=\left(\omega ,0,0,\omega \right)$ , $k\cdot x=\omega \left(z-t\right)$ and $c=1$ , the general solution can be written as

${h}_{\mu \nu}\left(z\right)=\left(\begin{array}{cccc}0& 0& 0& 0\\ 0& {\alpha}_{11}& {\alpha}_{12}& 0\\ 0& {\alpha}_{12}& -{\alpha}_{11}& 0\\ 0& 0& 0& 0\end{array}\right){\text{e}}^{i\omega \left(z-t\right)}$ (9)

which has two independent transverse polarization states and helicity ±2. The part proportional to ${\alpha}_{xx}={\alpha}_{11}$ is called the plus-polarization state and is denoted by +, and the part proportional to ${\alpha}_{xy}={\alpha}_{12}={\alpha}_{21}$ is called the cross-polarization state and is denoted by ×. It is in this sense that one usually associates spin-2 with gravity.

It will be convenient for our purpose to write the above solution in the form

$h\left(z\right)=\left[{f}_{\times}\left(t-z\right){\epsilon}_{\times}+{f}_{+}\left(t-z\right){\epsilon}_{+}\right]{\text{e}}^{i\omega \left(z-t\right)}$ (10)

$\equiv {h}_{\times}\left(z\right)+{h}_{+}\left(z\right)$ (11)

where h and $\u03f5$ are $4\times 4$ matrices with elements ${h}_{\mu \nu}\mathrm{,}{\epsilon}_{\mu \nu}$ etc, and ${h}_{\times}\left(z\right)\mathrm{,}{h}_{+}\left(z\right)$ are respectively the purely cross-polarized and purely plus-polarized gravity waves along the z axis, where

${\epsilon}_{\times}=\left(\begin{array}{cccc}0& 0& 0& 0\\ 0& 0& 1& 0\\ 0& 1& 0& 0\\ 0& 0& 0& 0\end{array}\right)$ (12)

${\epsilon}_{+}=\left(\begin{array}{cccc}0& 0& 0& 0\\ 0& 1& 0& 0\\ 0& 0& -1& 0\\ 0& 0& 0& 0\end{array}\right)$ (13)

are the unit polarization tensors. Notice that ${\u03f5}_{\times}{\u03f5}_{+}+{\u03f5}_{+}{\u03f5}_{\times}=0$ . Hence, ${h}_{\times}\left(z\right)$ and ${h}_{+}\left(z\right)$ anti-commute. The physical implications of this property need to be investigated further.

Using the basis vectors $|+\rangle ={\left(\mathrm{0,1,0,0}\right)}^{\text{T}}$ , $|-\rangle ={\left(\mathrm{0,0,1,0}\right)}^{\text{T}}$ , one can construct ${\epsilon}_{\times}=|+\rangle \otimes |-\rangle +|-\rangle \otimes |+\rangle \equiv |+-\rangle +|-+\rangle $ , and ${\epsilon}_{+}=|+\rangle \otimes |+\rangle -|-\rangle \otimes |-\rangle \equiv |++\rangle -|--\rangle $ . The other two basis vectors ${\left(\mathrm{1,0,0,0}\right)}^{\text{T}}$ and ${\left(\mathrm{0,0,0,1}\right)}^{\text{T}}$ are eliminated by choosing the TT gauge which makes the metric perturbation purely spatial and transverse.

The inner product of two matrices A and B is defined by the Frobenius product

$\langle A|B\rangle =\frac{1}{2}Tr\left({A}^{\u2020}B\right).$ (14)

Hence, we have $\langle {\epsilon}_{+}|{\epsilon}_{+}\rangle =\langle {\epsilon}_{\times}|{\epsilon}_{\times}\rangle =1,\langle {\epsilon}_{+}|{\epsilon}_{\times}\rangle =\langle {\epsilon}_{\times}|{\epsilon}_{+}\rangle =0$ .

3. Entanglement and Classical Gravity

According to the Equivalence Principle the effects of gravity can be transformed away in a local enough region that tidal effects can be ignored. Therefore, the effect of gravity on a single test mass has no physical significance. But two or more test masses in different locations can be physically influenced by linearized gravity waves which can change their “proper distances”. Linearized gravity waves are transverse and can therefore change the proper distances between test masses in a plane perpendicular to their propagation direction. If, therefore, a gravity wave like $h\left(z\right)$ (Equation (11)) travelling in the z direction is incident on an array of coplanar test masses at various locations in the xy plane (as, for example, in each arm of a laser interferometer like LIGO), it can be shown [7] [9] that the proper distances between the test masses will oscillate with the wave frequency $\nu =\omega /2\text{\pi}$ in two elliptical modes, one with axes parallel to the $\left(x\mathrm{,}y\right)$ axes corresponding to the plus-polarization wave and the other with axes rotated by π/4 relative to the $\left(x\mathrm{,}y\right)$ axes, corresponding to the cross-polarization wave. This π/4 rotation is because gravity is a rank-2 tensor field.

Hence, the state of the total system (test masses + gravity wave) must be of the form

$|H\rangle =|{h}_{+}\rangle |{\left(xy\right)}_{+}\rangle +|{h}_{\times}\rangle |{\left(xy\right)}_{\times}\rangle $ (15)

where $|{h}_{+}\rangle $ and $|{h}_{\times}\rangle $ denote the two orthogonal polarization states of the classical gravity wave, and $|{\left(xy\right)}_{+}\rangle $ and $|{\left(xy\right)}_{\times}\rangle $ denote the corresponding oscillation modes of the two arms of the classical interferometer in the xy plane which span an orthogonal Hilbert space. The ${h}_{+}$ component of the wave cannot produce ${\left(xy\right)}_{\times}$ oscillation modes and the ${h}_{\times}$ component cannot produce ${\left(xy\right)}_{+}$ oscillation modes, and therefore the states $|{h}_{+}\rangle |{\left(xy\right)}_{\times}\rangle $ and $|{h}_{\times}\rangle |{\left(xy\right)}_{+}\rangle $ cannot occur. Hence, (15) is a non-factorizable, and in that sense, “entangled” state of the two gravitational polarization modes and the corresponding oscillation modes of the classical detector. This is analogous to what happens in the quantum theory of measurement in which the apparatus gets entangled with the system to be measured. Hence the entanglement is between modes of two different systems, and differs from entanglement of two modes of the same system as in classical polarization optics.

The recent detection of gravitational waves may therefore be signalling entanglement in classical gravitational physics. We now propose a possible way of testing this hypothesis.

4. Contextuality in Classical Gravity: A Bell-CHSH Test

Let us consider a LIGO set up with the two arms of the laser interferometer in the xy plane, and a gravitational wave incident on it along the z direction. As we have seen from Equation (9), in the TT gauge there are two independent degrees of freedom and two amplitudes ${\alpha}_{xx}=-{\alpha}_{yy}$ and ${\alpha}_{xy}={\alpha}_{yx}$ . A wave with ${\alpha}_{xy}=0$ produces a metric

$\text{d}{s}^{2}=-\text{d}{t}^{2}+\left(1+{h}_{+}\right)\text{d}{x}^{2}+\left(1-{h}_{+}\right)\text{d}{y}^{2}+\text{d}{z}^{2}$ (16)

where ${h}_{+}={\alpha}_{xx}\mathrm{exp}\left(i\omega \left(z-t\right)\right)$ . This produces opposite effects on the proper distance on the two axes, contracting one and expanding the other. On the other hand, if ${\alpha}_{xx}=0$ , only the off-diagonal terms ${h}_{xy}={h}_{yx}={h}_{\times}$ in the metric are non-zero, and that corresponds to a π/4 rotation relative to the previous case. A general wave is a linear superposition of these two, and depending on the phase relation, a circular or elliptical polarization is produced. Consequently, the proper distances between the test masses in the interferometer are stretched and compressed along the x and y directions periodically in two modes, one parallel to the (xy) axes (the plus mode) and the other rotated by π/4 relative to the (xy) axes (the cross mode). An interferometer in the (xy) plane can measure the difference in the return times of light along the two arms in the x and y directions due to these changes in the proper distances through the phase changes they produce, resulting in fringe shifts in the interference pattern. Hence, the normalized state of the gravitational wave plus the oscillatory interferometer paths can be written in the form

$|\stackrel{^}{H}\rangle =\frac{1}{\sqrt{2}}\left(|{h}_{+}\rangle |{\left(xy\right)}_{+}\rangle +|{h}_{\times}\rangle |{\left(xy\right)}_{\times}\rangle \right)$ (17)

where $|{\left(xy\right)}_{+}\rangle $ and $|{\left(xy\right)}_{\times}\rangle $ denote the two oscillation modes of the arms of the interferometer.

To derive a Bell-CHSH inequality based on noncontextuality, let us first consider an arbitrary general state

$|H\rangle =\left(\mathrm{cos}\alpha |{h}_{+}\rangle +{\text{e}}^{i\beta}\mathrm{sin}\alpha |{h}_{\times}\rangle \right)\left(\mathrm{cos}\gamma |{\left(xy\right)}_{+}\rangle +{\text{e}}^{i\delta}\mathrm{sin}\gamma |{\left(xy\right)}_{\times}\rangle \right)$ (18)

$\equiv |{\psi}_{h}\rangle |{\psi}_{xy}\rangle $ (19)

where $\alpha \mathrm{,}\beta \mathrm{,}\gamma \mathrm{,}\delta $ are arbitrary parameters. Next, let us define the correlation

$E\left(\theta \mathrm{,}\varphi \right)=\langle H|{\sigma}_{\theta}\cdot {\sigma}_{\varphi}|H\rangle $ (20)

where $|H\rangle $ is an arbitrary normalized state of the apparatus + gravity, and

${\sigma}_{\theta}={\sigma}_{\theta ,0}-{\sigma}_{\theta ,\pi},$ (21)

${\sigma}_{\varphi}={\sigma}_{\varphi ,0}-{\sigma}_{\varphi ,\pi},$ (22)

with

${\sigma}_{\theta ,0}=\frac{1}{2}\left(|{h}_{+}\rangle +{\text{e}}^{i\theta}|{h}_{\times}\rangle \right)\left(\langle {h}_{+}|+{\text{e}}^{-i\theta}\langle {h}_{\times}|\right)\otimes {\mathbb{I}}_{xy},$

${\sigma}_{\theta ,\pi}=\frac{1}{2}\left(|{h}_{+}\rangle -{\text{e}}^{i\theta}|{h}_{\times}\rangle \right)\left(\langle {h}_{+}|-{\text{e}}^{-i\theta}\langle {h}_{\times}|\right)\otimes {\mathbb{I}}_{xy},$

${\sigma}_{\varphi ,0}={\mathbb{I}}_{h}\otimes \frac{1}{2}\left(|{\left(xy\right)}_{+}\rangle +{\text{e}}^{i\varphi}|{\left(xy\right)}_{\times}\rangle \right)\left(\langle {\left(xy\right)}_{+}|+{e}^{-i\varphi}\langle {\left(xy\right)}_{\times}|\right),$

${\sigma}_{\varphi ,\pi}={\mathbb{I}}_{h}\otimes \frac{1}{2}\left(|{\left(xy\right)}_{+}\rangle -{\text{e}}^{i\varphi}|{\left(xy\right)}_{\times}\rangle \right)\left(\langle {\left(xy\right)}_{+}|-{\text{e}}^{-i\varphi}\langle {\left(xy\right)}_{\times}|\right),$ (23)

where $\theta $ and $\varphi $ are phase shifts between the two polarization modes and the two path oscillation modes respectively, and ${\mathbb{I}}_{xy}$ and ${\mathbb{I}}_{h}$ are the identity operators in the Hilbert space ${\mathcal{H}}_{xy}$ spanned by the oscillating interferometer paths and the Hilbert space ${\mathcal{H}}_{h}$ spanned by the gravity wave polarizations respectively. Hence,

${\sigma}_{\theta}=\left({\text{e}}^{-i\theta}|{h}_{+}\rangle \langle {h}_{\times}|+{\text{e}}^{i\theta}|{h}_{\times}\rangle \langle {h}_{+}|\right)\otimes {\mathbb{I}}_{xy},$ (24)

${\sigma}_{\varphi}={\mathbb{I}}_{h}\otimes \left({\text{e}}^{-i\varphi}|{\left(xy\right)}_{+}\rangle \langle {\left(xy\right)}_{\times}|+{\text{e}}^{i\varphi}|{\left(xy\right)}_{\times}\rangle \langle {\left(xy\right)}_{+}|\right).$ (25)

It should be noted that ${\sigma}_{\theta}$ and ${\sigma}_{\varphi}$ act upon different Hilbert spaces altogether, and hence they commute with each other. This property is necessary for noncontextuality of the apparatus + gravity wave system. It has always been a tenet of classical physics that whatever exists in the physical world is independent of observations which only serve to reveal them. Put more technically, this means that the result of a measurement is predetermined and is not affected by how the value is measured, i.e. not affected by previous or simultaneous measurement of any other compatible or co-measureable observable. Hence the need for commuting observables to test noncontextuality.

For the general product state (19),

$E\left(\theta \mathrm{,}\varphi \right)=\langle {\psi}_{h}|{\sigma}_{\theta}|{\psi}_{h}\rangle \langle {\psi}_{xy}|{\sigma}_{\varphi}|{\psi}_{xy}\rangle ={E}_{h}\left(\theta \right){E}_{xy}\left(\varphi \right)\mathrm{,}$ (26)

with

${E}_{h}\left(\theta \right)=sin2\alpha cos\left(\beta -\theta \right)\mathrm{,}$ (27)

${E}_{xy}\left(\varphi \right)=sin2\gamma cos\left(\delta -\varphi \right)\mathrm{.}$ (28)

Thus, the expectation value $E\left(\theta \mathrm{,}\varphi \right)$ is the product of the expectation values of the polarization and proper distance (or path) projections. Hence, the path and polarization measurements for product states in classical gravity are independent of one another in all contexts. This is the content of noncontextuality. This may, at first sight, look obvious and trivial, but on closer inspection, one finds that it implies the inequality

$-1\le E\left(\theta \mathrm{,}\varphi \right)\le 1$ (29)

for the correlation.

Now, define a quantity S as

$S\left({\theta}_{1}\mathrm{,}{\varphi}_{1}\mathrm{;}{\theta}_{2}\mathrm{,}{\varphi}_{2}\right)=E\left({\theta}_{1}\mathrm{,}{\varphi}_{1}\right)+E\left({\theta}_{1}\mathrm{,}{\varphi}_{2}\right)-E\left({\theta}_{2}\mathrm{,}{\varphi}_{1}\right)+E\left({\theta}_{2}\mathrm{,}{\varphi}_{2}\right)\mathrm{.}$ (30)

It follows from (29) that

$\left|S\right|\le 2.$ (31)

All that is required to derive this bound for product states is that the correlations lie between −1 and +1, which is guaranteed by the results (27) and (28).

Now consider the correlation calculated for the normalized state (17), namely

$E\left(\theta \mathrm{,}\varphi \right)=\langle \stackrel{^}{H}|{\sigma}_{\theta}\cdot {\sigma}_{\varphi}|\stackrel{^}{H}\rangle $

$=\langle \stackrel{^}{H}|\left[(+){\sigma}_{\theta ,0}+(-){\sigma}_{\theta ,\pi}\right]\cdot \left[(+){\sigma}_{\varphi ,0}+(-){\sigma}_{\varphi ,\pi}\right]|\stackrel{^}{H}\rangle $ (32)

$=\langle \stackrel{^}{H}|\left[{\sigma}_{\theta ,0}\cdot {\sigma}_{\varphi ,0}+{\sigma}_{\theta ,\pi}\cdot {\sigma}_{\varphi ,\pi}-{\sigma}_{\theta ,0}\cdot {\sigma}_{\varphi ,\pi}-{\sigma}_{\theta ,\pi}\cdot {\sigma}_{\varphi ,0}\right]|\stackrel{^}{H}\rangle $ (33)

The intensities corresponding to the four possible orientations are given by

$I\left(\theta ,\varphi \right)=\langle \stackrel{^}{H}|{\sigma}_{\theta ,0}\cdot {\sigma}_{\varphi ,0}|\stackrel{^}{H}\rangle ,$

$I\left(\theta +\pi ,\varphi +\pi \right)=\langle \stackrel{^}{H}|{\sigma}_{\theta ,\pi}\cdot {\sigma}_{\varphi ,\pi}|\stackrel{^}{H}\rangle ,$

$I\left(\theta +\pi ,\varphi \right)=\langle \stackrel{^}{H}|{\sigma}_{\theta ,\pi}\cdot {\sigma}_{\varphi ,0}|\stackrel{^}{H}\rangle ,$ (34)

$I\left(\theta ,\varphi +\pi \right)=\langle \stackrel{^}{H}|{\sigma}_{\theta ,0}\cdot {\sigma}_{\varphi ,\pi}|\stackrel{^}{H}\rangle ,$

where clearly $I\left(\theta ,\varphi \right)=\frac{1}{2}\left[1+\mathrm{cos}\left(\theta +\varphi \right)\right]$ from (17) and the definitions (23).

We can write $E\left(\theta \mathrm{,}\varphi \right)$ in terms of the normalized intensities as

$E\left(\theta ,\varphi \right)=\frac{I\left(\theta ,\varphi \right)+I\left(\theta +\pi ,\varphi +\pi \right)-I\left(\theta +\pi ,\varphi \right)-I\left(\theta ,\varphi +\pi \right)}{I\left(\theta ,\varphi \right)+I\left(\theta +\pi ,\varphi +\pi \right)+I\left(\theta +\pi ,\varphi \right)+I\left(\theta ,\varphi +\pi \right)}=\mathrm{cos}\left(\theta +\varphi \right).$ (35)

It is clear from this that the noncontextuality bound (31) is violated by the state (17) for the set of parameters ${\theta}_{1}=0,{\theta}_{2}=\pi /2,{\varphi}_{1}=\pi /4,{\varphi}_{2}=-\pi /4$ for which $\left|S\right|=2\sqrt{2}$ . Since the distance and polarization changes occur in the same path, there is no violation of locality in this result. It is hoped that these predictions can one day be verified at facilities like LIGO.

Since we have used purely classical physics throughout, it is clear that entanglement and contextuality which are widely regarded as exclusively quantum mechanical, occur in classical gravity too.

Acknowledgements

The authors thank the S. N. Bose National Centre for Basic Sciences, Kolkata for inviting them to the International Symposium on New Frontiers in Quantum Correlations, Jan 29-Feb 2, 2018, where the basic ideas were developed. PG also thanks the National Academy of Sciences, India for a grant.

Conflicts of Interest

The authors declare no conflicts of interest regarding the publication of this paper.

Cite this paper

Ghose, P. and Rajagopal, A.K. (2018) Possibility of Classical Entanglement at LIGO. International Journal of Astronomy and Astrophysics, 8, 267-274. https://doi.org/10.4236/ijaa.2018.83019

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