Inflationary gravitational waves from unified spinor fields

Ridao, Luis Santiago; Arcodía, Marcos R. A.; Romero, Jesús Martín; Bellini, Mauricio

doi:10.1140/epjp/i2018-12337-x

Cited by 9 publications

(3 citation statements)

References 19 publications

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“…Let us discuss an additional number of issues concerning our proposed formalism of a (4+4)-world. First, in [51], following a unified spinor field theory, a pre-inflationary universe which makes a global topological phase transition was considered. It seems interesting to link our work with this reference in order to consider a kind of topological phase transition in a (4+4)-universe.…”

Section: Final Remarksmentioning

confidence: 99%

Aspects of (4 + 4)-Kaluza–Klein type theory

Nieto

Aguilar

2019

Phys. Scr.

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We develop a type of Kaluza-Klein formalism in (4 + 4)-dimensions. In the framework of this formalism we obtain a new kind of Schwarzschild metric solutions that via Kruskal-Szequeres can be interpreted as mirror black and white holes. We found that this new type of mirror black and white holes solutions in (3 + 1)-dimensions support the idea that the original space-time can be extended to (4 + 4)-signature. Using octonions, we also discus linearized gravity in (4 + 4)-dimensions.On the other hand, it is well known that the Kruskal-Szekeres coordinates give an alternative description of the event horizon of black-holes [21,22]. Traditionally, one starts with the Schwarzschild metric described by the coordinates t, r and the angular coordinates θ and φ associated with a unit sphere and after several algebraic steps one computes the Kruskal-Szekeres coordinates T and X which become functions of t and r. The key result of this process is that while the Schwarzschild metric is singular at the horizon r = 2GM = r s the Kruskal-Szekeres metric is not. However, the final transformations between the coordinates t, r and T and X seems to be, in a sense, intriguing because instead of describing only two regions (2-region) as in the case of Schwarzschild black-holes (interior and exterior) one

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Section: Final Remarksmentioning

confidence: 99%

Aspects of (4 + 4)-Kaluza–Klein type theory

Nieto

Aguilar

2019

Phys. Scr.

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“…. quantum relativistic components of the velocity on the background Riemann manifold, such that x is the background 4-length related to the line element of the coordinated space in (12). Furthermore, d bg R is an extended version of the Palatini identity [17], defined by the expression 6…”

Section: Back-reaction From a Ricci Flowmentioning

confidence: 99%

“…A natural question to ask is how to generalize the non-minimal spinor string to curved backgrounds, but the more important question is how to construct a string non-perturbative formalism on a curved background which can be explained from a non-commutative quantum space-time. A proposal named Unified Spinor Fields (USF) was recently introduced with the aim to resolve this question with a quantization of the space-time included [12][13][14][15][16], by taking into account also self-interactions of quantum spinor fields. The USF theory is developed in 8 dimensions, 4 of them related to the space-time coordinates ( m x ), and the other 4 related to the inner space (f m ), and are compact coordinates which have spin components as canonical momentums: ( m s ).…”

Section: Introductionmentioning

confidence: 99%

Ricci flow in general relativity: dynamics of gluon fields on an arbitrary curved background from unified spinor fields

Bellini

2021

Phys. Scr.

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Exponential collapse with variable time scale driven by a scalar field

Hernández

Bellini

Moreno

2019

Physics of the Dark Universe

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We study the dynamic collapse driven by a scalar field, when a relativistic observer falls co-moving with the collapse and cross the horizon of a Schwarzschild black-hole (BH), at t = t 0 . During the collapse the scale of time is considered as variable. Back-reaction effects and gravitational waves produced during the exponential collapse are studied. We demonstrate that back-reaction effects act as the source of gravitational waves emitted during the collapse, and wavelengths of gravitational waves (GW) are in the range: λ ≪ r s ≡ e −2h 0 t 0 2h 0 , that is, smaller than the Schwarzschild radius. We demonstrate that during all the collapse the global topology of the space-time remains hyperbolic when the observer cross the horizon. *

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Inflationary gravitational waves from unified spinor fields

Cited by 9 publications

References 19 publications

Aspects of (4 + 4)-Kaluza–Klein type theory

Aspects of (4 + 4)-Kaluza–Klein type theory

Ricci flow in general relativity: dynamics of gluon fields on an arbitrary curved background from unified spinor fields

Exponential collapse with variable time scale driven by a scalar field

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