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First, referring to an article by K. Freeze on “Natural Inflation”, we review e folds data, and also the role of a modified Heisenberg Uncertainty principle as to what to expect from initial conditions as to satisfying the onset of... more
First, referring to an article by K. Freeze on “Natural Inflation”, we review e folds data, and also the role of a modified Heisenberg Uncertainty principle as to what to expect from initial conditions as to satisfying the onset of inflation.. .. This leads to , combined with the authors work in delineating a ‘perfect bounce’ a minimum HFGW which may exist due to the early universe, possibly from the influence of a minimum nonsingular universe starting point forming the template of a minimum wave length for starting GW, which may lead to an initial quantum gravity influenced frequency which is subsequently e shifted down by inflation. The initial conditions for the generation of HFGW, may correspond to early universe quantum gravity . I.e. this last part is due to a question asked the author, Dr. Li Fangyu, in the first week of July 2016
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We review, using our prior work the Weyl tensor as an aid to reviewing the Penrose Weyl Tensor Conjecture near start of Inflation. Our supposition is that this Weyl tensor will not vanish, and this is in tandem with a non- zero initial... more
We review, using our prior work the Weyl tensor as an aid to reviewing the Penrose Weyl Tensor Conjecture near start of Inflation. Our supposition is that this Weyl tensor will not vanish, and this is in tandem with a non- zero initial entropy. In doing so, we make use of two representations of the scale factor, one with , and another in terms of , with the time, scaled as . The second representation of the derivative of will yield a not equal to zero due to initial time step not being zero, i.e. a quantization of time, whereas the first representation of depends upon the initial value assumed and picked. We then afterwards, say something as to Malek’s doctoral thesis rendition of , for n general dimensions as a way to buttress our conclusion, that indeed is non-zero at start of inflation provided certain assumptions are made. Which in turn affects entropy production at the start of the universe. Note . in the case of a Pre Planckian imaginary time , i.e. to have real valued, but no...
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We are using the book “Towards Quantum Gravity” with an article by Claus Kiefer as to a quantum gravity interpretation of the density matrix in the early universe. The density matrix we are using is a one loop approximation, with inflaton... more
We are using the book “Towards Quantum Gravity” with an article by Claus Kiefer as to a quantum gravity interpretation of the density matrix in the early universe. The density matrix we are using is a one loop approximation, with inflaton value and potential terms, like V (phi) using the Padmanabhan values one can expect if the scale factor is a ~a (Initial) times t ^ gamma. In doing so, we identify two time steps and presume a very small initial time step candidates initial time values which are from a polynomial for time values. A gravity wave analysis concludes our article with inflaton decay, which is finally linked to BHs. And then finally we show using work done by Hawking, et al. how this may give us Planck Sized Black Holes, in the onset of Inflation, with resulting consequences so outlined. A vastly simplified proof of BH masses of Planck mass is presented which ties in directly with issues of the mass of the inflaton initially generated by the 2nd derivative of the effecti...
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Use of super-radiance in BH physics, so specifies conditions for a mass of a graviton being less than or equal to 1065 grams, allows for determing what role additional dimensions may play in removing the datum that massive gravitons lead... more
Use of super-radiance in BH physics, so specifies conditions for a mass of a graviton being less than or equal to 1065 grams, allows for determing what role additional dimensions may play in removing the datum that massive gravitons lead to 3/4th the bending of light past the planet Mercury. The present document makes a given differentiation between super-radiance in the case of conventional BHs and Braneworld BH super-radiance, which may delineate whether Braneworlds contribute to an admissible massive graviton in terms of removing the usual problem of the 3/4th the bending of light past the planet Mercury which is normally associated with massive gravitons. This leads to a fork in the road between two alternatives with the possibility of needing a multiverse containment of BH structure or embracing what Hawkings wrote up recently, namely, a redo of the event horizon hypothesis as we know it.
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We obtain a polynomial based iterative solution for early universe creation of the Higgs boson mass, using a polynomial with the coefficients for derived through integral formulations with the mass of a Higgs boson, and the construction... more
We obtain a polynomial based iterative solution for early universe creation of the Higgs boson mass, using a polynomial with the coefficients for derived through integral formulations with the mass of a Higgs boson, and the construction of the coefficients derived as of the using a potential system, for the Higgs, largely similar to the Peskin and Schroeder quantum field theoretic treatment for a Higgs potential. Afterwards, we examine if mass may have complex number and possibly imaginary values, with attendant description of consequences in the electroweak regime of space-time. We end with a description of Imaginary mass becoming Real in Electroweak, with resultant consequences for DM discussed in the last section with explicit construction of space-time bubbles nucleated due to imaginary mass of Higgs becoming real, as a contributing source of GW radiation in Electroweak era
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First, we do a Taylor series expansion of Entropy. Afterwards we define the arrow of time. After that, we define what terms we will analyze in the Taylor series expansion of entropy to help in finding initial conditions which may allow... more
First, we do a Taylor series expansion of Entropy. Afterwards we define the arrow of time. After that, we define what terms we will analyze in the Taylor series expansion of entropy to help in finding initial conditions which may allow for the earliest possible identification of the Arrow of Time in cosmology. Definition of the arrow of time will allow choosing different initial starting points. That is, that in the actual equations of classical GR, there is no reason to have time asymmetry after given initial conditions. Time asymmetry is built into initial conditions and we start to explore which initial conditions may assist in evaluating contributions to Entropy via an analysis of which terms in a Taylor series survive, and what their sign and contribution values are.
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what happens to vacuum energy, if Stoica's calculations , 2012, remove necessity of avoiding analyzing BB singularity for Einstein's equations
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Recently, the author read the Alicki-Van Ryn test as to behavior of photons in a test of violations of classicality. The same thing is proposed via use of a spin two graviton, using typical spin 2 matrices. While the technology currently... more
Recently, the author read the Alicki-Van Ryn test as to behavior of photons in a test of violations of classicality. The same thing is proposed via use of a spin two graviton, using typical spin 2 matrices. While the technology currently does not exist to perform such an analysis yet, the same sort of thought experiment is proposed in a way to allow for a first principle test of the either classical or quantum foundations of gravity. The reason for the present manuscript topic is due to a specific argument presented in a prior document as to how is formed from semiclassical reasoning. We referred to a procedure as to how to use Maxwell’s equations involving a closed boundary regime, in the boundary regime between Octonionic Geometry and quantum flat space. Conceivably, a similar argument could be made forgravitons, pending further investigations. Also the anlysis of if gravitons are constructed by a similar semiclassical argument is pending if gravitons as by the Alicki-Van Ryn test...
This document is due to a question by Debasish of the Saha institute of India asked in the Dark Side of the Universe conference, 2010, in Leon, Mexico, and also is connected with issues as to the initial configuration of the arrow of time... more
This document is due to a question by Debasish of the Saha institute of India asked in the Dark Side of the Universe conference, 2010, in Leon, Mexico, and also is connected with issues as to the initial configuration of the arrow of time brought up in both Rudn 10, in Rencontres de Blois, and Fundamental Frontiers of Physics 11, in Paris, in July 2010. Further reference is made as to how to reconcile early inflation with re acceleration, partly by dimensional analysis and partly due to recounting a suggestion as by Yurov, which the author thinks has merit and which ties into, to a point with using massive gravitons as a re acceleration of the universe a billion years ago enabler, as perhaps a variant of DE.
Research Interests: Physics, Early Universe, Arrow of time, Cosmology, Universe, and 6 moreAcceleration, Writ, Graviton, Cq, Kv, and K
This paper shows how increased entropy values from an initially low big bang level can be measured experimentally by counting relic gravitons. Furthermore the physical mechanism of this entropy increase is explained via analogies with... more
This paper shows how increased entropy values from an initially low big bang level can be measured experimentally by counting relic gravitons. Furthermore the physical mechanism of this entropy increase is explained via analogies with early-universe phase transitions.As summarized by Thanu Padmanabhan (IUCAA) in the recent 25th IAGRG presentation he made, “Gravity: The Inside Story “, entropy can be thought of as due to ‘ignored’ degrees of freedom, classically, and is generalized in general relativity by appealing to to extremising entropy for all the null surfaces of space time. Padmanabhan claims the process of extemizing entropy then leads to equations for the background metric of the spacetime. I .e. that the process of entropy being put in an entremal form leads to the Einsteinian equations of motion. What is done in this present work is more modest. I.e. entropy is thought of in terms of being increased by relic graviton production, and the discussion then examines the conseq...
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We represent how an off diagonal representation of stress energy in GR as given by Dodelson can be affected by an axion style domain wall treatment of a stress energy tensor in GR, as given by Kolb and Turner.We argue that this is a way... more
We represent how an off diagonal representation of stress energy in GR as given by Dodelson can be affected by an axion style domain wall treatment of a stress energy tensor in GR, as given by Kolb and Turner.We argue that this is a way of presenting how domain wall physics may impact graviton production which in turn has, through Dodelson and his off diagonal stress energy terms consequences as to non uniform evolution of space time cosmology. We close with a treatment of axions (a candidate for DM) as impacting GW, and through Dodelson having consequences which we outline at the end of this document. The off diagonal terms of the stress energy tensor alluded to are allegedly for large scale space-time evolution, but the transition for space-time from the big bang to the Electroweak regime is many thousands of times larger than Planckian space-time, so we argue that the off diagonal relation so used still holds
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In this paper, the author asks if DM and gravitons could also impact the cosmic acceleration of the universe, leading to an increase of acceleration one billion years ago, in a manner usually attributed to DE. Following Alves, etal.... more
In this paper, the author asks if DM and gravitons could also impact the cosmic acceleration of the universe, leading to an increase of acceleration one billion years ago, in a manner usually attributed to DE. Following Alves, etal. (2009) the author will high light what KK style gravitons, with a slightly difierent mass proflle could mean in terms of DM. The conse- quences are from assuming that axions are CDM, and KK gravitons are for WDM, then up to a point, ‰Warm-Dark-Matter would dominate not only structure formation in early universe forma- tion. Further efiorts in obtaining data for such suppositions would lie in electro magnetic-graviton interactions contributing toward h 2›gw(f) being appropriately measured.
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The Mach's principle as unveiled in this paper is really a statement as to information conservation, with gravitons and gravitinos being information carriers.This Mach's principle application has tremendous implications as far... more
The Mach's principle as unveiled in this paper is really a statement as to information conservation, with gravitons and gravitinos being information carriers.This Mach's principle application has tremendous implications as far as if quantum mechanics is essential to formation of information in early universe physics In addition, we review Gryzinski's inelastic scattering results which have close fidelity to a normally quantum result of inelastic scattering in atomic hydrogen calculations and suggest that forming Planck's parameter we set as ( ) t h in this document could also be due to semiclassical processes, initially, leaving open the possibility quantum processes, initially are not mandatory in terms of formation of initial formulation of constants put into the Machian relations used in this paper.
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Based upon Alcubierre’s formalism about energy flux of gravitational waves, as well as Saunder’s treatment of temperature dependence of the Hubble parameter in the early universe, we initiate a particle count treat-ment of gravitons, and... more
Based upon Alcubierre’s formalism about energy flux of gravitational waves, as well as Saunder’s treatment of temperature dependence of the Hubble parameter in the early universe, we initiate a particle count treat-ment of gravitons, and subsequent entropy generation which gives, via the standard model treatment of the FRW metric a way to explain/justify a value of entropy of the order of 6 710 10S ~ at the very onset of in-flation.
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We will from first principles examine what adding acceleration does, and will not do as to the HUP previously derived. In doing so we will be examining a Friedmann equation for the evolution of the scale factor, using explicitly two... more
We will from first principles examine what adding acceleration does, and will not do as to the HUP previously derived. In doing so we will be examining a Friedmann equation for the evolution of the scale factor, using explicitly two cases, one case being when the acceleration of expansion of the scale factor is kept in, another when it is out, and the intermediate cases of when the acceleration factor, and the scale factor is important but not dominant. In doing so we will be tying it in our discussion with the earlier work done on the HUP. The ratio of 2nd derivative of a (time derivative), divided by a (a is a scale factor) set equal to zero would mean that the ratio of the 1st derivative of a (time derivative) divided by a could have complex solution roots, whereas the ration of the 2nd derivative of a (time derivative) divided by a with a, the scale factor as a ration not equal to zero, but constant, and large would frequently imply the first time derivative of a divided by a wo...
Research Interests: Physics and Acceleration
We find that having the scale factor close to zero due to a given magnetic field value in, an early universe magnetic field affects how we would interpret Mukhanov’s chapter on ‘self reproduction of the universe’ in in his reference... more
We find that having the scale factor close to zero due to a given magnetic field value in, an early universe magnetic field affects how we would interpret Mukhanov’s chapter on ‘self reproduction of the universe’ in in his reference “Physical foundations of cosmology” terms of production of inhomogeneity during inflation and its aftermath. The stronger an early universe magnetic field is, the greater the likelihood of production of about 20 new domains of size 1/ H, with H early universe Hubble’s constant, per Planck time interval in evolution. One final caveat to consider. What may happen is that the Camara (2004) density and Quintessential density (Corda et al.) are both simultaneously satisfied, which would put additional restrictions on the magnetic field which in turn affects structure formation. In time, once Eq.(16) of this paper is refined further, the author hopes that some of the issues raised by Kobayashi and Seto as to allowed inflation models may be addressed, once furt...
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Problems with space-time foam, if BB singularities no longer are inaccessible to modified version of Einstein equations, as given by Stoica (2012)
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The case for a four dimensional graviton mass (non zero) influencing reacceleration of the universe in five dimensions is stated; with emphasis upon if five dimensional geometries as given below give us new physical insight as to... more
The case for a four dimensional graviton mass (non zero) influencing reacceleration of the universe in five dimensions is stated; with emphasis upon if five dimensional geometries as given below give us new physical insight as to cosmological evolution. A calculated inflaton φ(t) may partly reemerge after fading out in the aftermath of inflation. The inflaton may be the source of re acceleration of the universe, especially if the effects of a re emergent inflaton are in tandem with the appearance of macro effects of a small graviton mass, leading to a speed up of the rate of expansion of the universe at red shit value of Z ~ .423. A final statement as to how and why the radius of the universe question may be affected by these deliberations is presented , in terms of if the graviton is either purely a field theoretic , or semi classical object, as via t'Hoofts deterministic QM is presented in the end, as an open question.
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The following document is to answer if higher dimensions add value to answering fundamental cosmology questions. The results are mixed, 1st with higher dimensions apparently helping in reconstructing and preserving the value of Planck’s... more
The following document is to answer if higher dimensions add value to answering fundamental cosmology questions. The results are mixed, 1st with higher dimensions apparently helping in reconstructing and preserving the value of Planck’s constant, and the fine structure constant from a prior to a present universe, while 2nd failing to add anything different from four dimensional cosmological models to the question of what would cause an increase in the expansion rate of the universe, as of a billion years ago. Finally 3rd, higher dimensions may allow creation of a joint DM and DE model. A choice between LQG and brane world geometry is introduced by Snyder geometry, where Snyder geometry’s minimum uncertainty length calculations Δx may help determine to what extent gravity is an emergent field that is classical. Independent of the choice of LQG and branes (four dimensions versus higher dimensional cosmology models) is the following question: If gravity is largely classical, how much n...