Parasitology

Chernin, Jack

doi:10.1201/9781482268003

Cited by 9 publications

(9 citation statements)

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“…The antigravity domination makes the flow expand with acceleration, and it is showed that because of this, the LFD is cooling with time and its time-rate tends to the cosmological value H 0 . These results (Chernin et al 2000(Chernin et al ,2004Baryshev et al 2001;Karachentsev et al 2003b;Teerikorpi et al 2005) are consistent with general astronomical considerations by Sandage et al (2006) and cosmological simulations by Macció et al (2005), Peirani & de Freitas (2008), Nurmi et al (2010). The same physics reveals itself also in several other well studied expansion flows on the spatial scales of 1-10 Mpc (Chernin et al 2007a,b,c, 2010, Chernin 2013).…”

Section: Introductionsupporting

confidence: 81%

“…In the case of the LFD, there is no additional environmental enhancement for the dark energy domination, and nevertheless the flow is expanding with acceleration as is found by Chernin et al (2000Chernin et al ( , 2004; see also discussion below and Fig.6 ( MNRAS 449, 2069MNRAS 449, , 2015 where the deceleration parameter q(R) for the LFD is presented which is negative for all the flow bodies. The example of the LFD suggests that a flow may be accelerating even if the mean matter density in its area is not less than the cosmological matter density; but the criterion |ρ ef f |/ < ρ M > 0 ≥ 1 must necessarily be satisfied.…”

Section: Lfd: No Underdensitymentioning

confidence: 67%

“…In search for the physical nature of the coldness of the local flows and their nearly cosmological time-rates, two main acting factors have been proposed: the universal dark energy background and the particular local environments of the flows. The studies of the local dark energy effects (Chernin et al 2000;Baryshev et al 2001;) assume that the dark energy is represented by Einstein's cosmological constant Λ, as in the currently standard ΛCDM cosmology. The constant is positive which implies that the dark energy produces a repulsive "force of antigravity".…”

Section: Introductionmentioning

confidence: 99%

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Dark energy domination in the local flow of giant galaxies

Chernin

Emel'Yanov

Караченцев

2015

Monthly Notices of the Royal Astronomical Society

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A dozen most luminous galaxies at distances up to 10 Mpc from the Local Group are moving away from the group forming the local expansion flow of giants.We use recent Hubble Space Telescope data on the local giants and their numerous fainter companions to study the dynamical structure and evolutionary trends of the flow. A N-body computer model that reproduces the observed kinematic of the flow is constructed under the assumption that the flow is embedded in the universal dark energy background. In the model, the motions of the flow members are controlled by their mutual attraction force and the repulsion force produced by the dark energy. It is found that the dark energy repulsion dominates the force field of the flow. Because of this, the flow expands with acceleration quantified with the local deceleration parameter. The dark energy domination is enhanced by the environment effect of the low mean matter density on the spatial scale of 50 Mpc in the local universe. The accelerating expansion cools the flow and introduces to it a nearly linear velocity-distance relation with the time-rate that is close to Hubble's factor of the global cosmological expansion.

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Section: Introductionsupporting

confidence: 81%

Section: Lfd: No Underdensitymentioning

confidence: 67%

Section: Introductionmentioning

confidence: 99%

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Dark energy domination in the local flow of giant galaxies

Chernin

Emel'Yanov

Караченцев

2015

Monthly Notices of the Royal Astronomical Society

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“…The question about the importance of DE on the dynamics of the Local Cluster (LC) was considered by Chernin (2001Chernin ( , 2008 and Chernin et al (2009). Simple estimations confirm this importance and, for the presently accepted values of the DE density ρ v = (0.72 ± 0.03) · 10 −29 g/cm 3 , the mass of the local group, including the dark mater input, is between M LC ∼ 3.5 · 10 12 M ⊙ , according to Chernin et al (2009), and M LC ∼ 1.3 · 10 12 M ⊙ , according to Karachentsev et al (2006). The radius R LC of the LC is known even worse.…”

Section: Application To the Local Galaxy Clustermentioning

confidence: 99%

“…So, the radius of the LC may be estimated as R LC = (GM LC /v 2 t ) = (1.5 ÷ 4) Mpc, with a very high error box, which we cannot estimate properly. Chernin et al (2009) give different intervals for the mass and radius of LC, without using the fixed value of v t , but considering the whole picture of the distribution of the galaxy velocities. They obtained…”

Section: Application To the Local Galaxy Clustermentioning

confidence: 99%

Polytropic Equilibrium Models With Non-Zero Cosmological Constant

Merafina¹,

Бисноватый-Коган²,

Tarasov³

2015

The Thirteenth Marcel Grossmann Meeting

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We solve the equation of the equilibrium of the gravitating body, with a polytropic equation of state of the matter P = Kρ γ , with γ = 1+1/n, in the frame of the Newtonian gravity, with non-zero cosmological constant Λ. We consider the cases with n = 1, 1.5, 3 and construct series of solutions with a fixed value of Λ. For each value of n, the non-dimensional equation of the static equilibrium has a family of solutions, instead of the unique solution of the Lane-Emden equation at Λ = 0. The equilibrium state exists only for central densities ρ0 larger than the critical value ρc. There are no static solutions at ρ0 < ρc. We investigate the stability of equilibrium bodies in presence of nonzero Λ, and show that dark energy decease the dynamic stability of the configuration. We apply our results for analyzing the properties of equilibrium states for cluster of galaxies in the present universe with non-zero Λ.

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Comparative genomic analysis of simple sequence repeats in three Plasmodium species

2010

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Simple sequence repeats (SSRs) are known to be responsible for genetic complexities and play major roles in gene and genome evolution. To this respect, malaria parasites are known to have rapidly evolving and complex genomes with complicated and differential pathogenic behaviors. Hence, by studying the whole genome comparative SSRs patterns, one can understand genomic complexities and differential evolutionary patterns of these species. We herein utilized the whole genome sequence information of three Plasmodium species, Plasmodium falciparum, Plasmodium vivax, and Plasmodium knowlesi, to comparatively analyze genome-wide distribution of SSRs. The study revealed that despite having the smallest genome size, P. falciparum bears the highest SSR content among the three Plasmodium species. Furthermore, distribution patterns of different SSRs types (e.g., mono, di, tri, tetra, penta, and hexa) in term of relative abundance and relative density provide evidences for greater accumulation of di-repeats and marked decrease of mono-repeats in P. falciparum in comparison to other two species. Overall, the types and distribution of SSRs in P. falciparum genome was found to be different than that of P. vivax and P. knowlesi. The latter two species have quite similar SSR organizations in many aspects of the data. The results were discussed in terms of comparative SSR patterns among the three Plasmodium species, uniqueness of P. falciparum in SSR organization and general pattern of evolution of SSRs in Plasmodium.

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Parasitology

Cited by 9 publications

References 0 publications

Dark energy domination in the local flow of giant galaxies

Dark energy domination in the local flow of giant galaxies

Polytropic Equilibrium Models With Non-Zero Cosmological Constant

Comparative genomic analysis of simple sequence repeats in three Plasmodium species

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