Relic High Frequency Gravitational waves from the Big Bang and How to Detect Them Andrew Beckwith [email protected] Abstract. This paper shows how entropy generation from numerical density calculations of relic gravitons can be measured via the Li-Baker high-frequency gravity wave (HFGW) detector, and suggests the implications this has for the physics of early-universe phase transitions. This paper indicates the role of Ng’s revised statistics in gravitational wave physics detection and the application of Baumann et al. (2007) formalism of reduction of rank-two tensorial contributions to density wave physics, using the HFGW approximation directly at the beginning as well as Li’s treatment of energy density explicitly. This formalism is a way to refine and add more capacity to the Li-Baker HFGW detector in reconstructing early-universe conditions at the onset of the big bang. Furthermore, we bring up how the HFGW detector can have its data sets compared and swapped with ice cube relic neutrino physics data taken at the south pole. This will enable us to begin to get criteria to falsify different inflation models as alluded to at the end of this manuscript. Keywords: High-Frequency Gravitational Waves (HFGW), Big Bang, Quantum (Infinite) Boltzmann Statistics, Phase Transitions, Gravitons,relic,inflation, relic neutrinos PACS: 98.80.Bp, 95.55.Ym, 26.35.+c INTRODUCTION At the June 2008 Dark Side meeting in Cairo, Egypt, Ng (2007) presented cogent arguments that entropy density is proportional to the number of dark matter particles per unit volume, which could also apply to gravitons. Ng’s central idea—that entropy and numerical production of “particles” can be applied to density of created gravitons per unit volume—is based on an argument Weinberg (1972) used to calculate the number of gravitons per unit volume in a frequency range between ω, ω+dω. Weinberg’s conceptualization of the creation of relic gravitons permits the development of a model entropy growth, starting from a very low level at the beginning of the universe to a much higher level right after the onset of the big bang, where the upper limit for the frequency used in deriving graviton production per unit volume was given by Grishchuk (2007) as 1010Hz, with some variance. This new model: 1) Assumes a temperature of T ~1032K, based on Weinberg’s (1972) statement that T ~1032K is the threshold for when quantum gravity dominates classical gravity, 2) Uses high-frequency gravitational waves (HFGW) explicitly of a scalar field reduction of the rank-two tensor arguments, based on the Baumann et al. (2007) use of quantum gravity operators to reduce a rank-two argument to a scalar field and then transform the entire object to a momentum space to get a scalar value for the variation of g due to gravity in momentum space, and uv 3) Uses Fourier analysis to extract relic gravitational wave signatures of the big bang, which is related to CMBR physics. Ng (2007) established a one-to-one relationship between change in entropy and change in the number of particles. Equating entropy change and graviton particle production suggests that the Li-Baker detector (Li et al., 2008) could be used to get an explicit big bang signature from HFGW data sets. That is, the Li-Baker detection methods can be used as a basis of falsifiable experimental criteria for the existence of relic gravitons from the big bang. 1 The Li-Baker detector (Li et al., 2008) uses a static magnetic field that varies under the impact of HFGWs for background detection of gravitational waves, and a fractal membrane to detect HFGW electromagnetic signatures. Researchers can use these signatures to confirm the existence of HFGWs by assuming that spin entropy density in the Li-Baker detector affects magnetic field spin and magnetism, per Rothman and Boughn (2006). Measurement of gravitons and gravitational waves is a way to establish an association between relic gravitational waves, gravitons, and entropy. This is a follow-up to a suggestion made by Yeo, et al. (2006) for how variation of spin entropy in a detector could dramatically enhance the sensitivity of existing HFGW detectors. The benefit of examining spin entropy density is in showing the existence of gravitons as a physically measurable datum in General Relativity, as well as the interrelationship of gravitons with HFGW from experimental data sets. Rothman and Boughn (2006) have written that the present set of existing detector systems with pre-Li-Baker detector technology (Li et al., 2008) is insufficient to accomplish meaningful detection of gravitons, suggesting that the Li-Baker detector may overcome the limits described by Rothman and Boughn: that with conventional detectors, one would need a detector mass about the size of Jupiter to detect a single graviton. Finally,we can compare how this re formulation may allow for data set swapping of information between the HFGW graviton production data and ice cube, which may improve our understanding of CMBR issues. REVIEWING JACK NG’S ARGUMENTS: HOW ENTROPY IS PROPORTIONAL TO A NUMERICAL DENSITY VALUE The fact that in both the dark matter and in the relic graviton production cases, entropy has similar quantum Boltzmann statistics will be the starting point for a derivation of the production of relic gravitons, linked to falsifiable experimental measurements. Ng (2007) used the following approximation for temperature and its variation with respect to a spatial parameter, starting with temperature T ≈R−1, where R can be thought of as a H H spatial representation of a region of space in which one can acquire statistics for the particles in question. Assume that the volume of space to be analyzed is of the form V ≈R3 . Then look at a preliminary numerical factor. Here the H proportionality argument of N ~(R l )2 is made, where l is the Planck’s length (~10−35cm) and a “wavelength” H P P parameter λ≈T−1 is also specified. That is, the value of λ≈T−1and of R are approximately within an order of H magnitude of each other. Ng (2007) changes conventional statistics by outlining how to get S≈N, which with additional arguments is defined to be S≈<n>, the numerical density of a species of particles. Ng begins with a partition function ⎛ 1 ⎞ ⎛ V ⎞N Z ~⎜ ⎟⋅⎜ ⎟ , (1) N ⎝N!⎠ ⎝λ3 ⎠ which according to Ng, leads to a limiting value of entropy of ( ) S ≈N⋅ log⎡V Nλ3⎤+5/2 , (2) ⎣ ⎦ but with V ≈R3 ≈λ3. If N is greater than one, entropy in equation (2) has a negative value. For a quantum H Boltzmann statistic calculation to obtain entropy, one does not want entropy with a negative value. The positive valued nature of entropy for physical systems calculated by Boltzmann statistics is a convention of statistical physics. Now this is where Ng introduces the removing of the N! term in equation (1). Inside the log expression, the expression of N in equation (2) is removed. This is a way to obtain what Ng refers to as Quantum Boltzmann statistics, where for a sufficiently large N , S ≈N. (3) The supposition here is that the value of N is proportional to the numerical graviton density n . It is noted that equation (3) gives credence not only to Baker et al. (2008) being applied to gravitons, but the same effort as done by Li et al. (2007) and as proposed (Beckwith 2008) in a symposium at Chongquing University in October 2008, for astrophysical applications of gravitational waves. Sensitive applications of equation (3) will help confirm the breakthrough physics of how gravitons disturb uniform magnetic fields within a HFGW detector, as remarked by Li et al. (2006).] 2 WEINBERG’S 1972 NUMERICAL ESTIMATE: THE NUMBER OF GRAVITONS PER FREQUENCY RANGE Assuming that k =1.38×10−16erg/0K, where 0K denotes Kelvin temperatures and where gravitons have two independent polarization states, the number of gravitons per unit volume with frequencies between ω and ω+dω is given by Weinberg (1972) as n(ω)dω=ω2dω⋅⎡⎢exp⎛⎜2⋅π⋅h⋅ω⎞⎟−1⎤⎥−1 (4) π2 ⎣ ⎝ kT ⎠ ⎦ The hypothesis presented here is that input thermal energy (from the prior universe) inputted into an initial cavity/region (dominated by an initially configured low temperature axion domain wall) would be thermally excited to reach the regime of temperature excitation. This would permit an order of magnitude drop of axion density ρ a from an initial temperature T ~H ≈10−33eV .[Per Beckwith (2008), this calculation assumes that dS t≤tP 0 Egraviton ≡hωgraviton∝(volume)⋅⎡⎣energy density≡t00⎤⎦, where the energy density term is from GR formulas. GIVING FREQUENCY/ ENERGY VALUE INPUTS TO GRAVITONS FROM GR ENERGY DENSITY EQUATIONS the Li et al. (2008) derivation/formula for energy density of gravitational waves is c4k2 t0 ≡ ⋅⎡h2 +h2⎤, (5) 0 4πGa3 ⎣ ⊕ ⊗⎦ where a≈a ⋅exp(H τ) ,where H is the initial value of the Hubble expansion parameter, and τ is a initial initial initial conformal time value. This value for an exponentially expanding scale factor will be crucially important in what is calculated later. The polarization values of relic gravitational waves Let us now consider how to get appropriate h ,h values by using Baumann et al. (2007) very complete treatment of ⊕ ⊗ rank-two tensorial contributions to the evolution of the gravitational wave contributions to entropy. This will be helped by having HFGW as a template to simplify a search for appropriate h behavior, which will be simplified ij after the reduction of h to a scalar field value. The main centerpiece of the derivation is to take into account a right- ij hand-side contribution of stress and strain to the conformal time evolution of h , which in a scalar Baumann, et al. ij (2007) field contribution reduction of complexity, and leads to the fast Fourier transform (FFT) ℑh ≡hˆ with an ij equation in conformal time τ that can be written as hˆ≡ A1(k)exp(i⎡kr⋅xr−kτ⎤)+ A2(k)exp(i⎡kr⋅xr+kτ⎤) (6) a(τ) ⎣ ⎦ a(τ) ⎣ ⎦ As Li et al. (2008) writes, the expression for hˆ in equation (6) is in response to a metric is written as ⎛−a2 0 0 0 ⎞ ⎜ ⎟ 0 a2(1+h ) a2h 0 ⎜ ⎟ g ≡ ⊕ ⊗ (7) μν ⎜ 0 a2h a2(1−h ) 0 ⎟ ⎜ ⊗ ⊕ ⎟ ⎜⎝ 0 0 0 a2⎟⎠ Changes in the treatment of equation (6) have to be made in order to consider a scalar expansion at the onset of the big bang, which would entail looking at stress and strain contributions to the evolution of the scalar field contribution to gravitational radiation, starting at the onset of the big bang. This treatment of space-time geodesics is 3 modified after stress and strain processes are added to the evolution of the gravitational waves. Addition of stress and strain as presented by Baumann et al. (2007) leads to the following evolution equation of space-time deformations and gravitational wave evolution, where pressure pis a constant and Ti is a stress term. Furthermore, j k2∝ energy and a′′ a ∝ potential energy so that a′ hˆ′′+2 ⋅hˆ′+k2hˆ=16π⋅G⋅a2⋅⎡Π (τ)=ℑ(T i−pδi)⎤. (8) a ⎣ k j j ⎦ Numerous Bessel and Hankel equations, referenced in Arfken (1985), show how combined solutions of Bessel ( ) and/or Hankel equations solve the homogeneous part of equation (9) above, provided that Π τ = 0. If one k wishes to take into account stress and strain forces associated with the onset of the big bang, one would have to look at particular and general solutions that use combinations of equations (8) and (9). The solution to equation (8) is based on what Baumann et al. (2007) developed in 2007 to deal with relic inflationary contributions to gravitational waves. The particular solution of equation (8) above will involve a Greens function treatment of equation (9), as described below, as an integral solution for h. Typically, as seen in Arfken (1985), this means putting a delta function on the right-hand side of equation (8), and using the resulting solution of equation (8) as modified, times the right-hand side of equation (8) as the integrand for a particular solution, then integrating over conformal time τ. In this situation, the very convenient a(τ)⋅hˆ=μ(k) is taken advantage of to use the Greens function solution to equation (9) with a delta function on the right-hand-side of equation (9) to help construct a particular solution to equation (8). This then will be part of how a particular solution for gravitational wave amplitude evolves in space-time. HFGW in Relic Inflationary Conditions Now the homogeneous and particular solution for equation (8) above is looked at with comments on HFGW modifications that simplify matters enormously. This will be pertinent to Li, et al. (2008) and what will be discussed later in this paper about the Li-Baker HFGW detector system, with its uniform magnetic field impinged upon by incident HFGW. This leads to a experimentally falsifiable claim that before the onset of the CMBR formation 280,000 to 300,000 years after the big bang, data sets are signatures of phase transitions that modeled appropriately with the following formalism. After making the substitution of a(τ)⋅hˆ=μ(k), equation (8) leads to a non-homogeneous perturbed Schrodinger- like equation, which can be written as ⎛ a′′⎞ μ′′+⎜⎝k2 − a ⎟⎠μ=a⋅⎡⎣16π⋅a2⋅Πk(τ)⎤⎦, (9) where the particular solution to equation (8) becomes 1 hˆ = ⋅∫dτ%⋅g (τ,τ%)⋅(16π⋅G⋅Π (τ%)) (10) Particular a(τ) k k The kernel in equation (10), g (τ,τ%), obeys the following equation if a′′ a<<k2, so for k ⎛ a′′⎞ g′′+⎜k2 − ⎟⋅g ≡δ(τ−τ%), (11) k ⎝ a ⎠ k where 1 g (τ,τ%)= [sin(kτ)⋅cos(kτ%)−sin(kτ%)⋅cos(kτ)]. (12) k k Given the above, a particular solution may be written as 1 hˆ = ⋅∫dτ%⋅[sin(kτ)cos(kτ%)−sin(kτ%)cos(kτ)]⋅(16π⋅G⋅Π (τ%)) (13) Particular a(τ)k k Details for the 16π⋅G⋅Π (τ%) part of this particular solution will be presented in the next section; for now, the k general solution is presented. The main dynamics of the 16π⋅G⋅Π (τ%) terms are that they are in part linked to k 4 quantum fluctuation. That is, the stress and strain are initially nucleated from a vacuum template of space-time itself in the beginning of a new universe, allowing for the following homogeneous part of evolution equation (8), with ( ) Π τ = 0, where the homogeneous solution to equation (8) is based on Izquierdo (2006) k a′ hˆ′′+2 ⋅hˆ′+k2hˆ=0. (14) a In the initial phases of nucleation of a new universe, equation (15) can be simplified as hˆ′′+2H ⋅hˆ′+k2hˆ=0. (15) initial Traditional treatments of both equations (14) and (15) make use of a dynamical, changing value of a′ a, in many cases leading to Bessel/Hankel equation solutions. By setting a′ a~H , to obtain Initial hˆ =hˆ ⋅⎡exp(−H τ)⎤⋅cos(kτ+c )+hˆ (16) Total Initial−Value ⎣ Initial ⎦ 1 Particular implies that in later times the dynamics are largely dominated by the particular, specialized solution. Stress and strain contributions to space time due to early universe production of HFGW The following analysis will deal with the HFGW contribution to forming the 16π⋅G⋅Π (τ%) stress and strain k contribution, using much of what Baumann et al. (2007) set for the simplest case of how to evaluate 16π⋅G⋅Π (τ%). k This takes into account a simplified treatment of the Bardeen and Wagoner (1971) potential for times τ<τ ; Threshold effectively confining τ<τ to within with two orders of magnitude of the Planck’s time interval after big bang Threshold nucleation of the present universe. This means working with the following template for the stress-strain-vacuum nucleation problem (16π⋅G⋅Π (τ%))≡S (source)=∫d3k%⋅e(k,k%)⋅ f (k,k%,τ)⋅ψ ⋅ψ (17) k k k−k% k% where ψ is a quantum fluctuation (offering a simplified model) and the term e(k,k%) is equal to k%2⋅(1−(kr⋅kr%) kk%). k% The main result of this section will be to present f(k,k%,τ), where w∝1/3 is used to obtain ⎧ 2⋅(5+3w) 1 ⎫ ⎪( 2 )⋅( 2 ) ⎪ ⎪ 1+ k−k% τ2 1+ k% τ2 ⎪ ( ) 4 ⎪ ⎪ f k,k%,τ ≡ ⎨ ⎬ (18) 3⋅(1+w) ⎡ ⎛ ⎞⎤ ⎛ ⎞ ⎪⎪+4⋅⎢ 2τ +τ2⋅ ∂ ⎜ 1 ⎟⎥⋅ ∂ ⎜ 1 ⎟⎪⎪ ⎪ ⎢1+ k−k%2τ2 ∂τ⎜⎜1+ k−k%2τ2 ⎟⎟⎥ ∂τ⎜⎜1+ k%2τ2 ⎟⎟⎪ ⎩ ⎣⎢ ⎝ ⎠⎥⎦ ⎝ ⎠⎭ Note that this uses the Bardeen and Wagoner (1971) potential in early times, which is 1 Φ= (19) 1+k2τ2 [Note that the derived quantity of hˆ, which is a FFT, with quantum raising and lowering operator considerations added, will require an inverse FFT used in the h2 +h2 expression of t0 for the Li-Baker detector.] ⊕ ⊗ 0 A Simplified Quantum Fluctuation Model Here, the ideas of Mukhanov and Wintizki (2007) are used, where they give a quantum fluctuation in k space along the lines of: ψ′′+(k2 +m2)ψ ≅0 (20) k k In the limit of low mass, this will lead to ψ ~exp(ikτ) (21) k 5 The assumption is made that with additional data acquisition, the nucleation quantum fluctuation formula as outlined in equation (21) will be given considerably more structure. TIES TO THE LI-BAKER HFGW DETECTOR With reference to Beckwith (2008), a power law relationship, first presented by Fontana (2005) using Park’s (1955) earlier derivation, is presented as ) m 2⋅L4⋅ω 6 P(power)=2⋅ graviton net (22) 45⋅(c5⋅G) With the effective energy E ≡ n(ω) ⋅ω≡ω , where graviton production is connected to equation (22), eff eff with ω ≈ω or ω →ω . eff net net eff This expression in power should be compared with the one presented by Giovannini (2008), averaging the energy- momentum pseudo tensor to get his version of a gravitational power energy density expression 27 ⎛ H ⎞2 ⎡ ⎛ H4 ⎞⎤ ρ(3) (τ,τ )≅ H2⋅⎜ ⎟ ⋅⎢1+ϑ⋅⎜ ⎟⎥ (23) GW 0 256⋅π2 ⎝M ⎠ ⎣ ⎝M4 ⎠⎦ This led Giovannini to state that “should the mass scale be picked such that M ~m >>m , and if the above Planck graviton formula were true, there are doubts that there could be inflation.” It is clear that gravitational wave density is faint, even if one makes the approximation that H ≡a& a≅mφ 6 as stated by Linde (2008). So H ≡a& a≅mφ 6and φ&=−m 2 3 makes it appropriate to use different procedures to come up with relic gravitational wave detection schemes to get quantifiable experimental measurements of relic gravitational waves. Equation (22) , and Equation (24) below imply a very short lived, but extreme energy flux as the starting point for graviton production, and also implies a large requisite value for M =V1/4, where V would be unusually large as a requisite inflationary potential. This is to be expected if there is an input from a universe prior to our own, as outlined by Beckwith (2008a and 2008b). It also is related to the following argument as given by Linde (2008) for gravitational wave amplitude. If one makes use of the present day gravitational radiation as M =V1/4 (Kofman, 2008), the energy scale with potential V and frequency (M =V1/4) f ≅ Hz, (24) 107GeV implies that f ~1010Hz. However, using equation (24) assumes that the temperature of thermally induced vacuum energy is rising to a maximum value 5T∗≈1032 0K , which is a huge energy flux. Beckwith (2008) asserted that midway during the thermal/vacuum energy transfer from a prior to the present universe, a relic gravition burst would have occurred. As shown in Table 1, this is consistent with a wormhole introduction of vacuum energy from a prior universe to the present, with a thermal buildup from near-zero vacuum energy values. The threshold burst is then consistent with a buildup of temperature from a prior universe, which introduces a relic graviton energy burst. 6 TABLE 1. Graviton burst Numerical values of Scaled graviton Temp Power production values N1=1.794×10−6 T∗ 0 N2=1.133×10−4 2T∗ 0 N3=7.872×1021 3T∗ 1.058×1016 N4=3.612×1016 4T∗ ~1 N5=4.205×10−3 5T∗ 0 By way of explanation (Beckwith, 2008), the above table assumes a rapid buildup of temperature resulting from energy-matter transfer from a prior universe. The Wheeler-De Witt wormhole equation, as given by Crowell (2005), contains a pseudo time component. The wormhole model of energy transfer uses Crowell’s treatment of the Wheeler-De Witt equation to model a bridge from a prior universe to our present universe. At the time the temperature reaches a maximum value of 5T∗ (1032degrees Kelvin), a graviton burst has already happened within 10−35seconds, and the frequency has gone up to 1010Hz, as given by π2 ⎛ v ⎞2 Ω (v)= h2(v)⎜ ⎟ (25) gw 3 ⎝vH ⎠ in Grishchuk (2007) and charted in Figure 1. FIGURE 1. Where HFGWs come from: Grishchuk (2007) found the maximum energy density (at a peak frequency) of relic gravitational waves. Comparing results of numerical production Smoot (2007) alluded to the following information theory regarding the number of information bits transferred between a prior and present universe: 7 1) Holographic principle allowed states in the evolution/development of the Universe - 10120 2) Initially available states given to us to work with at the onset of the inflationary era- 1010 3) Observable bits of information present due to quantum/statistical fluctuations -108 The relationship of bits to actual entropy, per Lloyd (2002), is that 10120bits correspond to an entropy reading of 1090. Arguments by Carroll (2005) suggest that black holes in the center of galaxies have entropy readings of 1088, whereas the jump in entropy from about 108 to 1090 is due to the jump in<n>, where <n>~ΔS ∝1021. graviton−production In a meeting in Bad Honnef in April 2008, brane theorists suggested that the huge entropy reading of black holes in the center of galaxies is excusable, since most of the purported entropy would be hidden by the event horizon of black holes. From this and discussions with others, it is apparent that the event horizon of a black hole is equivalent to the escape velocity of a black hole, trapping huge amounts of information/entropy, since the escape velocity of a black hole is greater than the speed of light. However, to measure entropy requires an entropy datum that can be measured. By definition, the black hole trapping of much of entropy in the universe leads to non-measurable data. Furthermore, it is assumed that the increase in entropy due to identification of a change of a relic graviton particle <n>~ΔS ∝1021 is within the ability graviton−production of the Li- Baker HFGW detector (Li et al., 2008) to obtain data sets. Identifying this relic graviton burst would allow for understanding how entropy increased in the first place and would permit astrophysicists to model different phase transitions in the problem of how the universe traversed through the “graceful exit problem” in inflationary cosmology. Gasperini et al. (1996) modeled graceful exit from inflation in terms of the Wheeler-De Witt equation and phase transitions. So far, little new progress has been made in getting the data sets needed to ascertain if their suggestion is true, but the Li-Baker detector should be able to identify falsifiable data collection procedures to confirm or falsify Gaperini’s suggestion of graceful exit from inflation. CONTRIBUTION OF THE LI-BAKER DETECTOR According to Li et al. (2008), the Li-Baker detector (Li, et al., 2008) is able to measure the interaction of HFGWs with a static magnetic field Bˆ(0), allowing researchers to get data on relic HFGWs created from relic big bang y conditions. . The electric and magnetic fields are generated by the HFGWs which, when A ≈A ≈A(k ) a(t), ⊗ ⊕ g and ω ≤1010Hz give the following values of electric and magnetic fields: g i 1 E%1 = A Bˆ(0)k c⋅(z+l )exp⎡i(k z−ωt)⎤+ A Bˆ(0)cexp⎡i(k z+ωt)⎤ x 2 ⊕ y g 1 ⎣ g g ⎦ 4 ⊕ y ⎣ g g ⎦ i 1 B%(1) = A Bˆ(0)k (z+l )exp⎡i(k z−ωt)⎤− A Bˆ(0)exp⎡i(k z+ωt)⎤ y 2 ⊕ y g 1 ⎣ g g ⎦ 4 ⊕ y ⎣ g g ⎦ (26) 1 i E%(1) =− A Bˆ(0)k c⋅(z+l )exp⎡i(k z−ωt)⎤+ A Bˆ(0)exp⎡i(k z+ωt)⎤ y 2 ⊗ y g 1 ⎣ g g ⎦ 4 ⊗ y ⎣ g g ⎦ 1 i B%(1) = A Bˆ(0)k (z+l )exp⎡i(k z−ωt)⎤+ A Bˆ(0)exp⎡i(k z+ωt)⎤ z 2 ⊗ y g 1 ⎣ g g ⎦ 4 ⊗ y ⎣ g g ⎦ a frequency value of ω ≤1010Hz is a base line for measurement in the Li- Baker detector in hopefully soon to be g available data sets. Li et al., (2008) numerically simulated incident relic graviton flux detected by the Li-Baker detector, with a value of N ≅2.89×1014/sec at a detector site. Beckwith (2008) has also created a model that g simulates graviton flux, for all gravitons produced by the big bang, of<n> ~7.872×10+21/sec (not just the gravitons g detected by the Li-Baker detector) 8 Quantum Entanglement Based on the same numerical simulation done by Dr. Li and reported in , Li et al., (2008), Dr. Li made a prediction (see equation 27) about the number of HFGW/ gravitons produced by the big bang, as compared to the general number of HFGW/ gravitons which the Li- Baker detector can access at the site of the detector. The difference in the numerator and denominator of equation (27) makes the case for the use of quantum entanglement detectors.There is a gap , i.e. a difference in the number of HFGW gravitons that are detectable by the Li-Baker detector (for all time from the big bang up to the present) and those relic HFGW gravitons from the onset of the big bang. The difference between gravitons producted at the onset of the big bang and those which are generally accessible for all times , from the big bang to the present is given in equation (27) below. The ratio of 10−2 appearing in the square root of equation (27) means that one out of a incoming HFGW gravitons detected by the Li-Baker detector would be relic in origin—directly due to the big bang—whereas the other 99 gravitons are due to astrophysical processes occurring after the big bang. The significance of the 8.76×10−2 value in equation (27) below in Li, et al (2008) is that this number refers to the ratio of the strength of the amplitude of the different gravitational wave contributions. I.e. the amplitude of the gravitational waves from the big bang are ~10−1 weaker at the Li Baker detector than general HFGW detected at the detector itself. What Li refers to as the strength, overall magnitude, of a PPF is the square root of numerical graviton flux, N . So equation (27) refers to the overall magnitude , amplitude g difference in value in the process of graviton production in the origins of the universe, to what is seen today. The values of 10−1 and 10−2 come directly from Dr. Li et al(2008) discussions of what is their equation (62) in their article written in 2008. N 2.89×1014 g−relic−GW ≡ ≈8.76×10−2 (27) N 3.77×1016 g−plane−GW This rarity of relic big bang gravitons means that for a next-generation refinement of sensitivity, the Li-Baker detector would need to use a variant of quantum entanglement to obtain a better data set of relic HFGW originating in the big bang. Yeo et al. (2006) presented calculations showing that a passing gravitational wave could influence the spin entropy and spin negativity of a system of N massive spin-(1/2) particles, in a way that is characteristic of the radiation. This implies entanglement, as Yeo et al. (2006) suggested. This suggests that what is now needed is to develop an actual entanglement entropy-based device that could complement and give additional refinement to the prediction given by equation (27). That would then help to analyze HFGWs to determine relic ω values. gravitation Thoughts and commentary upon swapping HFGW data with relic neutrinos As a convenience, this paper uses estimates from previous work (Beckwith, 2008) for high frequency gravitational wave (HFGW) upper frequency of detectable gravitational waves of approximately 1010Hz. Furthermore, arguments for an upper limit for the mass of neutrinos will be reviewed, and a mean temperature of T ~1032K is assumed as a starting point for neutrino and graviton production. Valev (2006) benchmarks upper limits for gravitational mass, as traditionally calculated, by claiming that observations lead to upper-bound values of m ~1.2×10−37eV /c2 (28) g And m ~ 0.0002eV /c2 (29) ve− Furthermore, the ratio of about 105 neutrinos to each graviton (most likely due to relic production of both ;neutrinos and gravitons) and the Li-Baker predictions (Li et al., 2008; Baker, Stephenson and Li, 2008; Stephenson, 2009) for 9 electric and magnetic field production suggests a connection between graviton/gravitational wave detection and neutrino data sets generated by the IceCube South Pole detector. The key to comparing these two data sets is the the ratio of 1 graviton to 10 5th neutrinos. That is, the presence of very low, but existent masses for both of them, plus some specifics as to how the IceCubeIceCube detector works, as far as obtaining data sets will be employed to make the point. The HFGW planar wave approximation as given by Eqn (26) is due to first order perturbative photon flux (PPF). The PPF is generated by the interaction of HFGWs with a static magnetic field Bˆ(0) (the inverse Gertsenshtein effect) and the synchro-resonance effect between the y HFGWs and the background Gaussian beam. Because the transverse PPF (signal) and the background photon flux (BPF) have very different behaviors (e.g. propagating direction, distribution, phase, polarization, decay, etc.) in some special regions, such properties provide a new way to distinguish and display the perturbative effects of HFGWs. Li et al. (2008) and Baker, Stephenson and Li (2008) give the transverse PPF form as follows, with ω=ω set as boundary conditions in the time-averaged brackets below. Equation (30) E and M fields are e g electromagnetic terms used to define F0(0) and F%1α(1). α c (1) c ~ ~ n1 = ⋅ T01 = − ⋅ F0(0)F1α(1) + F0(1)F1α(0) (30) hωe ω=ω μ0hωe α α ωe=ωg e g The F0(0) and the F%1α(1) terms represent the background and perturbative EM fields respectively in HFGWs, and α the angular brackets denote physical quantities averaged over time. Doing so will lead to detection of relic HFGW, provided the frequency ω ≤1010Hz. Linde et al. (2008) computed g an incident relic graviton flux of N ≅2.89×1014/sec at a detector site, as opposed to a graviton flux g of <n> ~7.872×10+21/sec at the onset of the big bang. In addition, a prediction that makes the case for quantum g entanglement detectors and Li et al. (2008), where there is a gap between constant value HFGWs gravitons detectable, by the Li-Baker detector, and relic gravity wave HFGW gravitons is given by Eqn (27) Equations (27), (28) and (29) imply that there is ample room to detect energized gravitons and that astrophysical neutrinos have energies ≤1012GeV , and that for every graviton, there is about 105neutrinos, according to Baumann et al. (2007). This means that, by using N ≈ 2.89×1014 << N ≈1020 (31) g−relic−GW relic−Neutrinos and assuming relic gravitons can have frequencies up to 102GHz(Brustein, et al., 1995 and 1997), or up to 1010Hz (Grishchuk, 2007), it can be concluded that the energy density today in horizon-size gravitational waves is at most a tiny fraction, about 104, of the closure density of the universe. Such waves would correspond to a distribution of gravitons of the Planck epoch that would be produced by a very mild degree of chaos. This requires extraordinary sensitivity to detect. However, just as with photons (but at a much earlier era because of the exceedingly weak interaction of gravitons), gravitons attain a characteristic energy distribution. The nature of quantum gravity and graviton interactions are uncertain and this need not be a blackbody distribution. The high end of graviton energy distribution probably is connected with the difference in mass, i.e., if neutrinos have ≤1012GeV per individual neutrino, then gravitons would have ≤10−34×1012GeV per graviton; meaning that it would require refined HFGW detectors such as the Li-Baker detector to observe them at all. If there is a ratio of 1 graviton per ten to the fifth power or so neutrinos, data from refined HFGW detectors should be able to be matched to IceCubeIceCube data. Inflation models, neutrino detection and HFGWs If there is a density increase as given by an inflation φ occurring because of chaotic inflation 10