Effects of cosmological constant on clustering of Galaxies

Hameeda, Mir; Upadhyay, Sudhaker; Faizal, Mir; Ali, Ahmed Farag

doi:10.1093/mnras/stw2202

Cited by 38 publications

(27 citation statements)

References 69 publications

(67 reference statements)

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“…On the other hand, we assume that ( ) t a t tends to 0 for 0 t → which is the usual assumption for the Big Bang. Yet, unlike a universe with four space-time dimensions, the overall scaling parameter ( ) Inserting (12) and (13) into (7)-(9) leads to the equations ( )…”

Section: Discussion and Limits Of The Five-dimensional Friedmann Equamentioning

confidence: 99%

“…Since the early 1990s, it has been known that the energy-matter content of the Universe consists not only of visible baryonic matter which contributes ≈ 5% to the Universe's energy, but also of Dark Matter (≈23%) and a phenomenon called Dark Energy (≈72%) which is related to the expansion of the Universe and probably associated to the cosmological constant [2]- [7] where measurements of the Universe's expansion suggest a value of approximately 10 −52 m −2 [8] [9] [10] [11]. In current theories, the cosmological constant has a fundamental meaning for certain phenomena in our Universe, such as on the clustering of galaxies [12] or on the gravity's rainbow effect [13] of black holes on the propagation of photons with different wave lengths where the cosmological constant is treated equivalent to the thermodynamic pressure [14] [15]. This latter property of the cosmological constant is, for example, also used to derive a relation amongst geometry, thermodynamics and information theory by using complexity [16].…”

Section: Introductionmentioning

confidence: 99%

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A Solution to the Cosmological Constant Problem in Two Time Dimensions

Köhn¹

2020

JHEPGC

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For the last hundred years, the existence and the value of the cosmological constant Λ has been a great enigma. So far, any theoretical model has failed to predict the value of Λ by several orders of magnitude. We here offer a solution to the cosmological constant problem by extending the Einstein-Friedmann equations by one additional time dimension. Solving these equations, we find that the Universe is flat on a global scale and that the cosmological constant lies between 10 −90 m −2 and 10 −51 m −2 which is in range observed by experiments. It also proposes a mean to explain the Planck length and to mitigate the singularity at the Big Bang.

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Section: Discussion and Limits Of The Five-dimensional Friedmann Equamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Solution to the Cosmological Constant Problem in Two Time Dimensions

Köhn¹

2020

JHEPGC

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“…Our motivation here is to study the effects of such corrections on the characterization of the clustering of galaxies on very large scales. The clustering of galaxies within the framework of modified Newton's gravity through the cosmological constant only has been studied very recently [38].…”

Section: Overview and Motivationmentioning

confidence: 99%

Thermodynamics and galactic clustering with a modified gravitational potential

Upadhyay

2017

Phys. Rev. D

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Based on thermodynamics, we study the galactic clustering of an expanding Universe by considering the logarithmic and volume (quantum) corrections to Newton's law along with the repulsive effect of a harmonic force induced by the cosmological constant (Λ) in the formation of the large scale structure of the Universe. We derive the N -body partition function for extended-mass galaxies (galaxies with halos) analytically. For this partition function, we compute the exact equations of states, which exhibit the logarithmic, volume and cosmological constant corrections. In this setting, a modified correlation (clustering) parameter (due to these corrections) emerges naturally from the exact equations of state. We compute a corrected grand canonical distribution function for this system. Furthermore, we obtain a deviation in differential forms of the two-point correlation functions for both the point-mass and extended-mass cases. The consequences of these deviations on the correlation function's power law are also discussed.Keywords: Cosmology; Modified gravity; Galaxies cluster; Large scale structure of universe;Correlation function; Distribution function. I. OVERVIEW AND MOTIVATIONThe characterization of galactic clusters on very large scales under the influence of their mutual gravitational interaction is a matter of vast interest. The importance of such a process can be exaggerated as the evolution and distribution of the galaxies throughout the Universe are the main manifestations of this. The analysis of the correlation functions is one of the standard ways to study the formation of the Universe. The observation tells us that the power law of two-point correlation function scales as (intergalactic distance) −1.6 to (intergalactic distance) −1.8 [1], which has also been approved by N -body computer simulations [2] and by the analytic gravitational quasiequilibrium thermodynamics [3]. The calculation of the power law of the correlation function is based on the assumption that the conversion of the initial primordial matter into the observed many-body galaxies took place at the stage of evolution of the Universe and these galaxies are coupled to the expansion of the Universe. The theories of the many-body (galaxies) distribution function have been developed mainly from a thermodynamic point of view [3][4][5][6][7][8]. Theses theories utilize only the first two laws of thermodynamics to derive the exact equations of state of the expanding Universe (a quasiequilibrium evolution).The relation between thermodynamics and relativity was originated in the work of Bekenstein [9], Hawking [10], and Unruh [11]. Later, Jacobson established an important connection between thermodynamics and general relativity, by which the Einstein equations themselves can be viewed as a thermodynamic equation of state under a set of minimal assumptions involving the equivalence principle and the identification of the area of a causal horizon with entropy [12][13][14][15][16]. Recently, Verlinde proposed a constructive idea stating that gravity...

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“…Work has been done to see the impact of modified potentials on thermodynamics of galaxy clustering [20,24,32]. The effect of the cosmological constant on the clustering of galaxies has been used deriving the gravitational partition function for galaxies in a universe with a cosmological constant and the influence on distribution of galaxies has been studied [33,34]. It is important to mention the phenomenological Tohline-Kuhn modified gravity approach to the problem of dark matter [35][36][37].…”

Section: Introductionmentioning

confidence: 99%

Two approaches that prove divergence free nature of non-local gravity

et al. 2021

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This paper is an attempt to study the thermodynamics of the structure formation in the large scale universe in the non local gravity using Boltzmann statistics and the Tsallis statistics. The partition function is obtained in both the approaches and the corresponding thermodynamics properties are evaluated. The important thing about the paper is that we surprisingly get the divergence free integrals and thus stress upon the fact that the nonlocal gravity is the singularity free model of gravity.

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Effects of cosmological constant on clustering of Galaxies

Cited by 38 publications

References 69 publications

A Solution to the Cosmological Constant Problem in Two Time Dimensions

A Solution to the Cosmological Constant Problem in Two Time Dimensions

Thermodynamics and galactic clustering with a modified gravitational potential

Two approaches that prove divergence free nature of non-local gravity

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