Multifrequency gravitational wave background from continuous sources

Gravitational waves have been detected in the past few years from several transient events such as merging stellar mass black holes, binary neutron stars, etc. These waves have frequencies in a band ranging from a few hundred hertz to around a kilohertz to which LIGO type instruments are sensitive. LISA would be sensitive to much lower range of frequencies from SMBH mergers. Apart from these cataclysmic burst events, there are innumerable sources of radiation which are continuously emitting gravitational waves of all frequencies. These include a whole mass range of compact binary and isolated compact objects as well as close planetary stellar entities. In this work, quantitative estimates are made of the gravitational wave background produced in typical frequency ranges from such sources emitting over a Hubble time and the fluctuations in the h values measured in the usual devices. Also estimates are made of the high frequency thermal background gravitational radiation from hot stellar interiors and newly formed compact objects.


Introduction
Gravitational waves (GW) as predicted by Einstein over a century ago, were first detected by LIGO in 2016 [1]. The waves came from two black holes circling closer and closer to each other till they finally collided and coalesced. Most of the radiation was released in the final orbit, which had a period of about a millisecond, with the wave frequency from 0.6 − 1. 2 , typical of such stellar events. About three solar masses were converted to energy of gravitational waves, i.e. ~5 × 10 54 . LIGO has detected several such events of black hole mergers since. Apart from black hole mergers, in 2017, LIGO detected gravitational waves from the collision of two neutron stars. Unlike the black hole mergers which are only detectable gravitationally, this event (GW170817) was also detected electromagnetically [2].
These are long wavelength, low frequency gravitational waves. Future gravitational wave detectors like LISA would be sensitive to much longer wavelengths and lower fluxes [3]. However compact stellar objects can generate high frequency thermal gravitational radiation, which in the case of hot neutron stars can be high. Also white dwarfs and main-sequence stars can generate such radiation from plasma-Coulomb collisions. Gamma ray bursts could also be sources of such radiation, as also the terminal stages of evaporating black holes [4,5].
Here a study is made of the thermal gravitational wave emission from all of the above sources, and the background flux is estimated. The earliest phases of the Universe close to the Planck scale would also leave remnant thermal gravitational waves. The integrated thermal gravitational flux as the Universe expands is also estimated and compared with that from all the discrete sources discussed above. Possible schemes to detect such sources of high frequency thermal gravitational radiation are discussed and the physical principles involved are elaborated.

Gravitational waves from merger of compact binary objects
Gravitational wave detectors like LIGO are hunting for waves from compact binary inspirals, which are produced by orbiting pairs of massive, compact objects like neutron stars (NS) and black holes (BH). Gravitational waves detected so far by LIGO fall in this category. These compact binary systems include binary neutron stars, binary black holes, and neutron star -black hole binary.
It is expected that there should be about a billion neutron stars in the Milky Way. Of the total of ~10 9 neutron stars in the galaxy, about half (5 × 10 8 ) will be part of NS binaries [6]. The two neutron stars orbiting each other closely emit gravitational radiation and spiral inward. Their merger leads to the formation of either a more massive neutron star, or a black hole (depending on whether the mass of the remnant exceeds the Tolman-Oppenheimer-Volkoff limit). The power radiated through GW for an equal mass binary system, each of mass , separated by a distance (circular orbit), is given by [7]: (1) where the frequency of gravitational waves is: The merger time of the equal mass binary system is given by: i.e. the merger time is related to the mass and separation as, ∝ = (≈ 4.35 × 10 17 ), we have following equation (3), 3 = × 4 . For instance, an equal mass binary, each 2 ⨀ , would merge in Hubble time, if their initial separation is ≈ 2.5 × 10 11 . The maximum initial separation ( ) of the equal mass binary of different mass range to merge within the Hubble time is given in figure 1. From this we can express the separation in terms of the mass as: From equations (4) and (2) Figure 2(a) gives the variation of frequency ( ) of GW with mass ( ) and figure 2(b) gives the variation of power ( ) emitted in GW with mass ( ). The total energy emitted over the Hubble time ( ) is = × . This will give a background flux which could affect gravitational waves measured from distant bursts. These values for varying masses of the equal mass binary black holes are tabulated in table 1. These values of frequency and power are those associated with the initial stages of the separation of the equal mass binaries. They evolve over time as the separation decreases, with both and increasing with decreasing separation. The frequency detected by gravitational wave detectors, like LIGO, is that during the merger as the separation, ≈ 2 × radius of the NS, or 2 × Schwarzschild radius in the case of BHs.  As the binary components continue to approach each other, the frequency increases, culminating with the chirp frequency as they ultimately merge which is the one measured by GW detectors. The rate of change of the frequency with decreasing distance between the binary components is given by: The variation in frequency -for binary systems with different masses -with respect to decreasing distance (as they approach) is plotted in figure 3(a). As the binary components continue to inspiral, the power emitted due to gravitational radiation increases, and the corresponding change in power is: The variation in power with respect to decreasing distance is plotted in figure 3(b), for binary systems with different mass.  The total power radiated during the merger can be obtained by integrating equation (9) from the initial separation to that at the merger (≈ 2 × radius of the NS, or 2 × Schwarzschild radius for BHs). For a 2 ⨀ NS binary, the total energy emitted in GW over the merger time is then given as: For a merger time of about a billion years, the total energy emitted is ≈ 10 51 . With one NS merger per galaxy in 10 5 years, the total number of mergers in the whole Universe (with ~10 11 galaxies) is ~10 6 per year. Then in the Hubble time, total mergers that have already taken place would be ~10 16 . Each of these mergers would release an energy of ~10 52 (= 2 ⁄ , the binding energy of the NS, where is the radius of the NS) in GW. This then implies that a total energy of ~10 68 is released in GW. This is spread over the Hubble volume of 2 2 3 ≈ 10 85 , hence the energy density is ~10 −17 / and the corresponding flux on Earth is ~10 −9 / 2 / in the frequency range of 100 − 1 (the chirp frequency detected by the GW detectors at the final stages of the merger). The flux of gravitational waves is related to the strain as: For frequency of 100 , the strain will be: ℎ ≈ 10 −24 . This is the strain due to the background flux, and it is about one order lesser than the sensitivity of LIGO, which is ≈ 10 −23 .
In the case of BHs, a 20 − 30 ⨀ BH is formed by the collapse of a 50 ⨀ progenitor star. On average a massive star collapses every second in the Universe. So in the Hubble time, total of ~10 17 such collapses will occur. The number of stars from 20 to 50 ⨀ mass range is given by (using the usual Salpeter mass function): where, ~1 /( 3 ⨀ ), this works out to be, = 0.02 /( 3 ⨀ ). Stellar mass BH mergers are estimated to occur once every 200 -300 seconds in the Universe. So the total number of such mergers in the Hubble time will be ~10 15 . The energy flux is comparable to NS Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 19 January 2021 doi:10.20944/preprints202101.0386.v1 mergers. The energy released is 10 -100 times more than that in the case of NS mergers, but the frequency is 100 times lower, hence the background strain is comparable.
In the case of mergers of SMBH, the frequency is very low, but the energies are much higher, so only LISA can detect the corresponding background strain. For example, the binary system OJ 287 consists of two orbiting supermassive black holes about a Gpc away. The mass of the primary black hole is deduced to be 18 billion solar mass, and the secondary black hole of OJ 287 has a mass of 150 million solar mass. For the orbital period of 12 years, the orbit separation is ~10 4 AU. The energy released as gravitational radiation when the merger occurs would be ~10 62 . Even at Gpc distance the strain on a gravitational wave detector would be, ℎ ≈ 10 −16 , with a typical frequency ~5 − 10 microhertz. This would be a very 'bright' signal for LISA (which has a threshold of ~10 −23 ) [8].

Thermal gravitational waves: Sources and background
Apart from mergers of binary compact objects, compact stellar objects can generate high frequency (10 16 − 10 21 ) thermal gravitational radiation. In the case of hot neutron stars, these thermal GW can be high. Main-sequence stars can generate such thermal gravitational radiation from plasma-Coulomb collisions, as also white dwarfs. Apart from these stellar and stellar remnants, gamma ray bursts could also be a source of thermal GW. Another possible source of such thermal GW are the terminal stages of evaporating black holes.

Thermal gravitational waves from hot stellar cores and compact stellar remnants
Due to Coulomb collisions in the core of the stars, thermal gravitational waves can be generated. These thermal gravitational waves can arise in white dwarfs and neutron stars due to the fermion collisions in the dense degenerate Fermi gas.
If 1 , 2 are the number densities of gas particles undergoing collision with a 12 Ω differential scattering cross-section, with relative velocity 12 and reduced mass 12 , then the power per unit volume per unit frequency interval is given by the quadrupole formula as [9]: ̇= ( where, is the volume of the stellar core and = ℎ ≈ 10 17 is the frequency corresponding to the core temperature of the star of ≈ 10 7 , and the corresponding velocity of the particles, 12 ≈ 8 × 10 7 / . The typical number density, 1 = 2 = ⁄ ≈ 10 26 −3 , and volume of the stellar core, ≈ 10 33 3 . And for a main sequence star [10], These values give the power of thermal gravitational waves emitted as, ̇≈ 10 16 / , at a frequency of, ≈ 10 17 . The flux of thermal gravitational waves from the Sun, received at Earth is of the order of half a watt. Considering all the 10 11 stars in all the 200 billion galaxies, the power associated with the thermal gravitational waves from all these stars is of the order of, ̇≈ 10 38 / . The total energy emitted due to the thermal gravitational waves by these stars over their average life span of ≈ 3 × 10 17 is, ≈ 3 × 10 55 / . In the case of white dwarfs (WD), the number density is of the order of, 1 = 2 ≈ 10 31 −3 , and the velocity corresponding to the white dwarf core temperature of ≈ 10 8 , is of the order of ≈ 2 × 10 8 / , and the corresponding frequency is ≈ 10 18 . And for a white dwarf, ∑ 12 Ω 2 ≈ 10 −25 2 . The power of thermal gravitational waves emitted by the white dwarf works out to be of the order of, ̇≈ 10 19 / , at a frequency of, ≈ 10 18 . In the case of neutron stars , 1 = 2 ≈ 10 38 −3 , and the velocity corresponding to the nascent neutron star core temperature of ≈ 5 × 10 10 , is of the order of ≈ 5 × 10 9 / , and the corresponding frequency is ≈ 10 21 . And for a neutron star, ∑ 12 Ω 2 ≈ 10 −29 2 . The power of thermal gravitational waves emitted by the neutron star works out to be of the order of, ̇≈ 10 29 / , at a frequency of, ≈ 10 21 .
If one out of every 100 stars is a neutron star, then the power associated with the thermal gravitational waves from all the neutron stars is, ̇≈ 10 49 / . The total energy emitted due to the thermal gravitational waves by these NS cores over the average life span of their nascent hot-core stage of ~10 8 is, ≈ 10 57 .

Thermal Gravitational Waves from PBHs
Primordial black holes (PBHs) are hypothetical type of black holes that are formed not by the gravitational collapse of a star but by the extreme densities of matter present during early Universe [11]. As these PBHs evaporate through Hawking radiation, part of the energy could be released in the form of thermal gravitational waves [5]. In the case of spontaneous graviton emission, the quadrupole gravitational power is given by: ̇= A typical PBH, that evaporates over the Hubble time has a mass of ~10 14 and the corresponding Schwarzschild radius, ≈ 10 −13 . The power due to the gravitational waves can be written as: where is the typical velocity and is the time scale, of the underlying explosive processes giving rise to the gravitational wave emission. The term within the bracket corresponds to the power of the explosion, therefore we have, ̇= 5 2 . The total energy released in the form of gravitational waves is then, The number of quanta of gravitational waves is then given by: where, = is the energy of the explosion and ℏ⁄ is the energy of each gravitational wave quanta. For the typical PBH of mass ~10 14 , the energy of the explosion is: = 2 ≈ 10 35 (19) And the number of quanta, ≈ 10 38 . The frequency and the corresponding energy of the gravitational wave quanta are given by, = 1⁄ and = ℏ⁄ , respectively. Here = ⁄ ≈ 10 −23 . Therefore each quanta of gravitational waves has an energy of ≈ 10 −4 (100 ) with a frequency of ≈ 10 23 . The total energy associated with the thermal gravitational waves is then given as, = ≈ 10 34 . We see that 10% of the energy of PBH explosion is converted to high frequency gravitational waves, with a typical frequency of ≈ 10 23 corresponding to ~100 . According to current estimates, the number density of PBHs in the Universe could be ~1 ( ) 3 ⁄ [12]. Then the total energy associated with the gravitational waves from these PBHs over the entire volume of the Universe of (10 28 ) 3 is, ≈ 10 54 . This corresponds to a cosmic background energy density of ≈ 10 −30 / , and a flux of, ≈ 10 −20 / 2 / in high energy thermal gravitational waves at typical energies of ~100 . If the number density of PBH is higher, say, ~1 ( ) 3 ⁄ , then the flux would be ≈ 10 −10 / 2 / . The above discussion pertains to only those PBH's that evaporate over the Hubble time of 10 10 years. The integrated flux from all the PBH's over the entire Hubble time will give the background thermal gravitational flux. The number of the PBH's as a function of mass can be written as [13]: where, ℎ ( 0 ) is the present number density of PBHs, 0 is the mass of the PBH that evaporate over the Hubble time and = 3. The integrated energy of the gravitational wave emission over the entire volume of the Universe is given by: The upper limit of the integral 2 = 10 14 is the mass of the PBH that will evaporate over the Hubble time scale and the lower limit 1 = 10 13 , below which the flux is too small. Volume = 2 2 3 , where = 10 28 is the Hubble radius. With these values we get the total integrated energy as, ≈ 10 32 , and the total integrated energy flux as, ≈ 10 −24 / 2 / .

Thermal gravitational waves from gamma ray bursts
Similar to stellar cores, in GRBs also, Coulomb collisions can result in the emission of high frequency gravitational waves. The power of the thermal gravitational waves is given by the same expression as that for the stars, but the bulk properties will be altered by factors of Γ (Lorentz factor), due to the relativistic velocities encountered in GRBs. The number density will be increased by a factor of gamma and the volume associated with the GRB, will be given by the deceleration volume. In gamma ray bursts, due to the general relativistic effects, the shock wave (from a spherical shell around the blast) propagated from the burst will be decelerated.
With the Lorentz factor taken into consideration, the power of the thermal gravitational waves emitted from a GRB will be [4]: where ≈ 10 51 , is the energy of the GRB. For = 10 2 −3 , we have the power, ̇≈ Γ 4 × 3.5 × 10 15 / . For a gamma ray burst corresponding to a Γ = 100, the power works out to be of the order of 3.5 × 10 23 / at the frequency of ≈ 10 22 .

Thermal gravitational waves from short duration GRB
Short duration gamma ray bursts have a shorter duration (< 0.2 − 2 ) and a harder spectrum as compared to the duration of 2 -200 s for long GRBs. Short GRBs are due to the merger of two neutron stars, whereas, the long GRBs are due to the collapse of very massive stars. The spectrum observed is harder because the objects merging to produce the GRB are more compact.
The time taken for the merging of two NS is given by, = 2 ⁄ . For two neutron stars of mass 1.5 ⨀ the merger time typically works out to be of the order of 10 9 years. Due to the longer merger time of the NS, the short GRBs are found in older population elliptical galaxies [14].
In the case of the merger of two neutron stars, the number density as well as the temperature is substantially high compared to the long duration GRB, with temperature of the order of 10 13 and ≈ 10 40 −3 . Considering all the gamma factors associated with the GRB [15,16], as in the previous case, the gravitational power is given by, ̇≈ Γ 4 × 4 × 10 43 , at a frequency of ≈ Γ × 10 23 . During the short duration burst, the two neutron stars undergo collision. During the tidal breakup of the neutron stars, its binding energy is released, which for a pair of neutron stars each of mass 1.5 ⨀ and radius of about 10 6 , is For a gamma factor of about 100, the power radiated due to the thermal gravitational wave emission is of the order of ̇≈ 4 × 10 51 / . This implies that about 1% of the energy released in the short duration gamma ray burst could be in the form of thermal gravitational waves. For a GRB at a typical distance of 100 , the flux is given by: Since the event occurs over a time scale of one second, the flux is equivalent to the fluence.

Cosmic background thermal gravitational radiation
At the Planck epoch in the early Universe, with ≈ 10 −43 , all the interactions were of equal strength so that thermal equilibrium was maintained between gravitons and other particles. As the Universe expanded, the gravitational interaction weakened and gravitons decoupled from other Preprints (www.preprints.org) | NOT PEER-REVIEWED | Posted: 19 January 2021 doi:10.20944/preprints202101.0386.v1 particles [9]. If is the number of particles that were coupled with the graviton, then the temperature of the background thermal gravitational radiation is given by: where, is the background radiation temperature. And for the present cosmic radiation temperature of 2.7 and with ≈ 30, we have the temperature of the background thermal gravitational radiation of about 1 . This result has consequences for the inflationary model of the Universe. At the time of inflation, the expansion of the Universe occurred at an exponential rate where the expansion was increased by a factor of 10 28 , when the Universe was 10 −36 old [17]. The radiation temperature at this epoch is given by: The temperature of the background thermal gravitational radiation corresponding to this radiation temperature is given by, 1 3 ⁄ ≈ 8 × 10 27 (27) and the corresponding wavelength is, = ℏ ≈ 10 −28 (28) At the end of the inflation phase, the wavelength of the gravitational radiation background is 1 . However, in order not to interfere with nucleosynthesis in the hot dense phase, its energy density would have to be < 1% of the radiation energy density. This would give an ℎ of the order of . Now the wave would be stretched by a further factor of 10 19 (at the present epoch). This would give a wavelength of 10 19 at present. Detection of such waves through fluctuations in the cosmic microwave background radiation could verify the existence of such a phase in the early Universe [18]. If inflation had not taken place, we would be left with a thermal gravitational wave background with a temperature of ~1 . If at all this can be detected, it would provide evidence against inflation [7].
Also the detection of these thermal background gravitational waves provides a basis to verify the validity of the big bang model itself. There are claims that the most convincing evidences of the big bang, the microwave background and abundance of helium, can be accounted for without invoking the big bang. But these thermal gravitational waves cannot be generated without the Universe passing through the super-hot, super-dense Planck epoch [19].

Integrated background thermal gravitational radiation
Thermal gravitational waves continue to be generated in the early Universe as it expands, as the temperature and particle densities continue to be high. We can estimate the integrated power emitted in thermal gravitational waves as the Universe cools from say 10 13 − 10 5 [20]. This is similar to what was done for stellar core (in section 3.1) but now all the quantities are time dependant. The time range, corresponding to the above temperatures is 10 −6 − 10 10 . The power per unit volume per unit frequency interval is given by the same expression as in equation (13).
The initial values corresponding to time 10 −6 is given by: This is the integrated energy radiated by the background thermal gravitational radiation in the early Universe as the temperature cooled from 10 13 − 10 5 , and this is spread over the Hubble volume.
As the Universe expanded, this energy is red shifted by a factor given by, 10 5 ≈ 10 5 . Therefore the present energy associated with the integrated background thermal gravitational radiation is of the order of 10 62 . The flux associated with this integrated background thermal gravitational radiation (IBTGR) is given by, ≈ 2 × 10 −14 / / 2 . The energy density associated with the cosmic microwave background radiation is of the order of 10 −13 / 3 , and the corresponding flux is, ≈ 10 −3 / / 2 . We see that the flux associated with integrated background thermal gravitational radiation is about 10 orders less than that of the CMB radiation.
The contribution of the microwave background radiation to the normalised critical density of the Universe is Ω ≈ 4 × 10 −5 . Since the flux associated with IBTGR is about 10 orders less the contribution to Ω due to this will be Ω ≈ 10 −15 . The overall energy associated with the emission of thermal gravitational waves from stellar sources is of the order of 10 57 , which is still about 5 orders less than that associated with IBTGR (10 62 ) as arrived at earlier. As for the PBH's, we need something like 10 30 of them to match the thermal gravitational wave background. This would need a density of such objects much more than what is implied by the gamma ray background.

Detection of thermal gravitational waves
When a weak gravitational wave passes through a system of particles along a line perpendicular to the plane of the particles then the particles will oscillate. The area enclosed by the particles does not change, and there is no motion along the direction of propagation. Passing of gravitational waves through a system of masses sets it into harmonic oscillations, hence causing a strain h.
However, current devices in operation like LIGO are expected to detect an ℎ ≈ 10 −22 . But what about the detection of thermal gravitational waves. So far there have been few attempts to conceive detection of such waves. The flux of thermal gravitational wave from the Sun (around frequency of ≈ 10 16 ) at earth is about 0.5 (5 × 10 6 ). How can we detect this kind of high frequency gravitational wave radiation? For example, in magnetised plasma, gravitational waves can be coupled to electromagnetic waves and can get damped. The damping time is given by: For a magnetic field of 10 15 and ≈ 10 12 , the damping time is of the order of 10 2 . If two particles in the gas is separated by a distance of , and the passing of gravitational wave causes a strain ℎ, then the change in the distance between the particles is given by, ∆ = ℎ . The distance of separation is given by, = ⁄ where, is the frequency and = √ ⁄ is the particle velocity. The change in velocity due to the passing of the gravitational wave is given by, ∆ = ℏ , and the energy change per collision is given by, = 1 2 ( ∆ ) 2 . If the number density of particles is and is the mean free path, the total power radiated over the volume is given as: The energy density of the wave is of the order of, The quantity has the same dimensions as 2 , hence √ can be interpreted as the gravitational plasma frequency associated with the particles undergoing oscillations due to the passing of the gravitational waves.
In the case of neutron stars with temperature of the order of ≈ 10 11 we have ≈ . The damping time will be of the order of 10 −18 and hence waves may be trapped within the NS. The trajectories of charged particles may be affected by passage of gravitational waves, which involves generation of electric current in the magnetised plasma.
The high frequency gravitational waves can also be detected through the atomic transitions induced by them at a very slow rate [7]. The quadrupole transition of hydrogen from 3 → 1 state with emission of a graviton occurs at a frequency of ≈ 10 15 . The quantum mechanical transition rate is given by [21]: = ℏ , where, is the power emitted by a dipole. For the case of spontaneous graviton emission, the quadrupole gravitational power is given by, = The frequency of this transition is of the order of 10 16 , which is within the range of thermal gravitons emitted from the Sun. About 10 3 gravitons fall per square metre per second on the Earth from the Sun at this frequency. Thus there is a finite probability of detecting induced emission with a sufficiently large detector. This radiation will be very penetrating.
By coincidence, the lifetime for this transition to take place is the same as the proton decay time (10 38 ). Proton decay is a major prediction of GUTs and despite the long lifetime is being tested by several experiments. So it may not altogether be impossible to also observe the effects of high frequency thermal gravitational radiation, which can also induce transitions with a lifetime comparable to that of proton decay.
The absorption rate of these high frequency gravitons can be estimated as ≈ 10 −27 , for terrestrial detectors, so one requires a detector of several hundred square kilometres to detect a few transitions in some decades [22].
Another way of detecting these thermal GW is to convert them into electromagnetic waves of same frequency. When an electromagnetic wave of amplitude propagates through a constant magnetic field 0 , as it produces a quadrupole stress term given by: = 0 ( − ) (37) This stress term gives rise to gravitational waves given by the linear Einstein equation [20]: Alternatively, a weak gravitational wave ℎ propagating through a magnetic field 0 gives rise to a magnetic field perturbation given by [23]:  = 2 ℎ 0 (39) The fraction of the gravitational wave energy converted into electromagnetic waves of frequency is given by [24,25]: = 0 2 2 , where, is the spatial extent of the uniform magnetic field.

Conclusions
The gravitational waves detected so far by the LIGO and Virgo collaboration are from transient events, such as the final stages of mergers of black holes and neutron stars. These waves have frequencies in a band ranging from a few hundred hertz to around a kilohertz to which LIGO type instruments are sensitive. Here we study various sources of continuous background gravitational waves. The frequency and background flux for a whole mass range of compact binary and isolated compact objects are estimated. As shown, these gravitational wave backgrounds are produced in typical frequency ranges, over a Hubble time. The fluctuations in the strain due to these background GW fall within the sensitivity range of either existing or proposed GW detectors.
Such gravitational waves are also associated with close planetary stellar entities. For instance the total power emitted in GW by Jupiter as it orbits the Sun is about a few kilowatts. For a system of a hot Jupiter (10 ) orbiting a solar mass star with a period of a day (at a distance of ≈ 0.02 ) the power emitted in GW is ≈ 7 × 10 24 / , at a frequency of 10 −5 . There could also be new class of planetary dark matter objects that could emit gravitational radiation [26].
We have also given detailed estimates of the high frequency thermal gravitational radiation flux emitted from a variety of high energy sources including nascent neutron stars, gamma ray bursts, evaporating primordial black holes, etc. We have also estimated the integrated thermal gravitational wave flux produced in the expanding early universe. This integrated cosmic thermal gravitational wave background has a present energy density about five orders of magnitude higher than that from all other discrete sources. Gravitational waves also provides a testing tool for various theories of gravity, i.e. general relativity and extended theories of gravity, and will be the definitive test for general relativity [27].