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Color contour plot for 2 χ of the Hubble diagram for the Pantheon sample in ΛCDM cosmology when H 0 and M Ω are variables and 0.626 Λ Ω = .
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A bstract
A bouncing scenario of a flat homogeneous and isotropic universe is explored by using the reconstruction technique for the power-law parametrization of the Hubble parameter in a modified gravity theory with higher-order curvature and trace of the energy-momentum tensor terms. It is demonstrated that bouncing criteria are satisfied so that...
It is well known that a spherical triangle of 270 degree triangle is constructible on the surface of a sphere; a globe is a good example. Take a point (A) on the equator, draw a line 1/4 the way around (90 degrees of longitude) on the equator to a new point (B).
We consider a combination of perturbative and non-perturbative corrections in Kähler moduli stabilizations in the configuration of three magnetised intersecting D7 branes in the type-IIB/F theory, compactified on the 6d T^6/Z_N orbifold of Calabi-Yau three-fold (CY_3). Two of the Kähler moduli are stabilized non-perturbatively, out of the three whi...
Slides utilizados na apresentação do trabalho final da disciplina
![Figure 5. From Vatistas [5]](profile/Florentin-Smarandache/publication/377217898/figure/fig4/AS:11431281216151188@1704635269388/From-Vatistas-5_Q320.jpg)
It is known that most existing cosmology models do not include rotation, with few exceptions such as rotating Bianchi and rotating Godel metrics. Therefore in this paper we aim to discuss four possible ways to model rotating universe, including Nurgaliev's Ermakov-type equation. It is our hope that the new proposed method can be verified with obser...
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... In order to derive the radius in pc of the Einstein ring, we briefly review the angular distance in three relativistic cosmologies: the standard, the flat and the wCDM. The minimax approximation allows the derivation of three approximate formulae for the angular distance which are calibrated on the Pantheon sample [26] [27] [28]. ...
... The above integral cannot be done in analytical terms, except for the case of 0 Λ Ω =, but the Padé approximant, see Appendix A in [28], allows us to derive an approximation for the indefinite integral. In the relativistic models, the angular diameter distance, A D [30], is ( ) ...
... For n = 4 they are examples of spatial sections of a Robertson-Walker space-time [14]. Alternatively, they are spatial sections of a Milne universe [15][16][17][18][19][20][21][22][23][24][25]. Hyperbolic spaces are natural candidates for universes that are either completely empty, or filled with test matter (identified by Milne with galaxies). ...
A new dynamical paradigm merging quantum dynamics with cosmology is discussed. We distinguish between a universe and its background space-time. The universe here is the subset of space-time defined by Ψτ(x)≠0, where Ψτ(x) is a solution of a Schrödinger equation, x is a point in n-dimensional Minkowski space, and τ≥0 is a dimensionless `cosmic-time’ evolution parameter. We derive the form of the Schrödinger equation and show that an empty universe is described by a Ψτ(x) that propagates towards the future inside some future-cone V+. The resulting dynamical semigroup is unitary, i.e., ∫V+d4x|Ψτ(x)|2=1 for τ≥0. The initial condition Ψ0(x) is not localized at x=0. Rather, it satisfies the boundary condition Ψ0(x)=0 for x∉V+. For n=1+3 the support of Ψτ(x) is bounded from the past by the `gap hyperboloid’ ℓ2τ=c2t2−x2, where ℓ is a fundamental length. Consequently, the points located between the hyperboloid and the light cone c2t2−x2=0 satisfy Ψτ(x)=0, and thus do not belong to the universe. As τ grows, the gap between the support of Ψτ(x) and the light cone increases. The past thus literally disappears. Unitarity of the dynamical semigroup implies that the universe becomes localized in a finite-thickness future-neighbourhood of ℓ2τ=c2t2−x2, simultaneously spreading along the hyperboloid. Effectively, for large τ the subset occupied by the universe resembles a part of the gap hyperboloid itself, but its thickness Δτ is non-zero for finite τ. Finite Δτ implies that the three-dimensional volume of the universe is finite as well. An approximate radius of the universe, rτ, grows with τ due to Δτrτ3=Δ0r03 and Δτ→0. The propagation of Ψτ(x) through space-time matches an intuitive picture of the passage of time. What we regard as the Minkowski-space classical time can be identified with ctτ=∫d4xx0|Ψτ(x)|2, so tτ grows with τ as a consequence of the Ehrenfest theorem, and its present uncertainty can be identified with the Planck time. Assuming that at present values of τ (corresponding to 13–14 billion years) Δτ and rτ are of the order of the Planck length and the Hubble radius, we estimate that the analogous thickness Δ0 of the support of Ψ0(x) is of the order of 1 AU, and r03∼(ctH)3×10−44. The estimates imply that the initial volume of the universe was finite and its uncertainty in time was several minutes. Next, we generalize the formalism in a way that incorporates interactions with matter. We are guided by the correspondence principle with quantum mechanics, which should be asymptotically reconstructed for the present values of τ. We argue that Hamiltonians corresponding to the present values of τ approximately describe quantum mechanics in a conformally Minkowskian space-time. The conformal factor is directly related to |Ψτ(x)|2. As a by-product of the construction, we arrive at a new formulation of conformal invariance of m≠0 fields.
... For n = 4 they are examples of spatial sections of a Robertson-Walker space-time [14]. Alternatively, they are spatial sections of a Milne universe [15][16][17][18][19][20][21][22][23]. Hyperbolic spaces are natural candidates for universes that are either completely empty, or filled with test matter (identified by Milne with galaxies). ...
A new dynamical paradigm merging quantum dynamics with cosmology is discussed. Time evolution involves a genuine passage of time, which distinguishes the formalism from those where dynamics in space is equivalent to statics in space-time. Hyperbolic spatial sections occur as asymptotic large-cosmic-time supports of quantum wave functions. For simplicity, the wave functions are defined on $n$-dimensional Minkowski spaces. We begin with empty universe, but then outline the formalism that involves matter fields. As a by product, we arrive at a new formulation of conformal invariance of $m\neq 0$ fields.
