The Rare Blood Factor rh('') or Eu

Sussman, Leon N.

doi:10.1182/blood.v10.12.1241.1241

Cited by 13 publications

(34 citation statements)

References 3 publications

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“…In the present article we provide a continuation and broad generalization of [54] and [55]. Hence, we extend, enhance and generalize all previous literature, since we examine by rigorous, qualitative and numeric arguments the fulfillment of sufficient conditions for an effective acceleration for domains in generic models, as opposed to looking at excessively simplified toy models (as in [47,48,50]) or particular cases defined by observational constraints (as in [51]) or suitable ansatzes (as in [52,53]).…”

Section: Introductionmentioning

confidence: 92%

“…To simplify notation, and whenever there is no risk of confusion, we will use the symbol r as argument of these functions. The difference between the average functionals (7) and (8) and their associated functions (9) is illustrated in figure 1 (see also [54,55]). ‡ Our notation reflects the fact that spherical domains are characterized by a radial range and are univocally labeled by the comoving radius of the boundaryr = r. This notation is easily compared with the standard notation: S [r] = S D[r] .…”

Section: Proper Volume Average and Quasi-local Averagementioning

confidence: 99%

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Back-reaction and effective acceleration in generic LTB dust models

Sussman¹

2011

Class. Quantum Grav.

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Abstract. We provide a thorough examination of the conditions for the existence of back-reaction and an "effective" acceleration (in the context of Buchert's averaging formalism) in regular generic spherically symmetric Lemaître-Tolman-Bondi (LTB) dust models. By considering arbitrary spherical comoving domains, we verify rigorously the fulfillment of these conditions expressed in terms of suitable scalar variables that are evaluated at the domains' boundaries. Effective deceleration necessarily occurs in all domains in: (a) the asymptotic radial range of models converging to a FLRW background, (b) the asymptotic time range of non-vacuum hyperbolic models, (c) LTB self-similar solutions and (d) near a simultaneous big bang. Accelerating domains are proven to exist in the following scenarios: (i) central vacuum regions, (ii) central (non-vacuum) density voids, (iii) the intermediate radial range of models converging to a FLRW background, (iv) the asymptotic radial range of models converging to a Minkowski vacuum and (v) domains near and/or intersecting a non-simultaneous big bang. All these scenarios occur in hyperbolic models with negative averaged and local spatial curvature, though scenarios (iv) and (v) are also possible in low density regions of a class of elliptic models in which local spatial curvature is negative but its average is positive. Rough numerical estimates between −0.003 and −0.5 were found for the effective deceleration parameter. While the existence of accelerating domains cannot be ruled out in models converging to an Einstein de Sitter background and in domains undergoing gravitational collapse, the conditions for this are very restrictive. The results obtained may provide important theoretical clues on the effects of back-reaction and averaging in more general non-spherical models.

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Section: Introductionmentioning

confidence: 92%

Section: Proper Volume Average and Quasi-local Averagementioning

confidence: 99%

Back-reaction and effective acceleration in generic LTB dust models

Sussman¹

2011

Class. Quantum Grav.

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“…for the domain D[z] delimited by z =constant and contained in the hypersurface t=constant. Here h is the determinant of the 3-dimensional part of the projection tensor h ab = g ab +u a u b , and F is a physically meaningful weighting function that was discussed in [45][46][47][48][49].…”

Section: B Growth Rate Equations and Integration In Curved Szekeres mentioning

confidence: 99%

“…It was shown in [45][46][47][48] that ρ q is a coordinate independent quantity that can be expressed in terms of curvature invariants and is given for the Szekeres Class-I models by [48] ρ q (t, z) = 6M (z) S(t, z) 3 .…”

Section: B Growth Rate Equations and Integration In Curved Szekeres mentioning

confidence: 99%

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Growth of structure in the Szekeres class-II inhomogeneous cosmological models and the matter-dominated era

Ishak

Peel

2012

Phys. Rev. D

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This study belongs to a series devoted to using the Szekeres inhomogeneous models in order to develop a theoretical framework where cosmological observations can be investigated with a wider range of possible interpretations. While our previous work addressed the question of cosmological distances versus redshift in these models, the current study is a start at looking into the growth rate of large-scale structure. The Szekeres models are exact solutions to Einstein's equations that were originally derived with no symmetries. We use here a formulation of the Szekeres models that is due to Goode and Wainwright, who considered the models as exact perturbations of a Friedmann-Lemaître-Robertson-Walker (FLRW) background. Using the Raychaudhuri equation we write, for the two classes of the models, exact growth equations in terms of the under/overdensity and measurable cosmological parameters. The new equations in the overdensity split into two informative parts. The first part, while exact, is identical to the growth equation in the usual linearly perturbed FLRW models, while the second part constitutes exact non-linear perturbations. We integrate numerically the full exact growth rate equations for the flat and curved cases. We find that for the matter-dominated cosmic era, the Szekeres growth rate is up to a factor of three to five stronger than the usual linearly perturbed FLRW cases, reflecting the effect of exact Szekeres non-linear perturbations. We also find that the Szekeres growth rate with an Einstein-de Sitter background is stronger than that of the well-known non-linear spherical collapse model, and the difference between the two increases with time. This highlights the distinction when we use general inhomogeneous models where shear and a tidal gravitational field are present and contribute to the gravitational clustering. Additionally, it is worth observing that the enhancement of the growth found in the Szekeres models during the matter-dominated era could suggest a substitute to the argument that dark matter is needed when using FLRW models to explain the enhanced growth and resulting large-scale structures that we observe today.PACS numbers: 98.80. Es,95.30.Sf

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Rh Blood Group System

Daniels¹

2002

Human Blood Groups

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The Rare Blood Factor rh('') or Eu

Cited by 13 publications

References 3 publications

Back-reaction and effective acceleration in generic LTB dust models

Back-reaction and effective acceleration in generic LTB dust models

Growth of structure in the Szekeres class-II inhomogeneous cosmological models and the matter-dominated era

Rh Blood Group System

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