Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity

Weinberg, Steven; Dicke, R. H.

doi:10.1119/1.1987308

Cited by 2,344 publications

(4,300 citation statements)

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“…3), and the subject's breakthroughs were quickly documented in textbooks whose influence would last for decades. 69,[79][80][81][82] Cosmology had become a quantitative subject, served by a plethora of observations, as reflected in its now often accompanying adjective "physical". 60,79 According to relativistic cosmology, a homogeneous and isotropic expanding universe can either be flat, open, or closed, all corresponding to different fates of cosmic evolution.…”

Section: How Cosmology Gained Its Weightmentioning

confidence: 99%

How dark matter came to matter

2017

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The history of the dark matter problem can be traced back to at least the 1930s, but it was not until the early 1970s that the issue of 'missing matter' was widely recognized as problematic. In the latter period, previously separate issues involving missing mass were brought together in a single anomaly. We argue that reference to a straightforward 'accumulation of evidence' alone is inadequate to comprehend this episode. Rather, the rise of cosmological research, the accompanying renewed interest in the theory of relativity and changes in the manpower division of astronomy in the 1960s are key to understanding how dark matter came to matter. At the same time, this story may also enlighten us on the methodological dimensions of past practices of physics and cosmology.Uncovering the nature of 'dark matter'-the mysterious substance that dominates the mass budget of the universe from sub-galactic to cosmological scales-is arguably one of the greatest challenges of modern physics and cosmology. Indeed, many physicists and astronomers across the world are today trying to identify the nature of dark matter.

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Section: How Cosmology Gained Its Weightmentioning

confidence: 99%

How dark matter came to matter

2017

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“…The comoving relative separation r 12 in a space described by the Robertson–Walker metric is (Weinberg 1972, equation 14.2.7; Osmer 1981) where θ is the angular separation of the two objects on the sky, and κ= ( H 0 / c ) 2 (Ω 0 +Λ 0 − 1). This equation is not symmetric in z 1 and z 2 for a non‐flat universe (κ≠ 0).…”

Section: Statistics Of the Cluster Distributionmentioning

confidence: 99%

Superclusters with thermal Sunyaev--Zel'dovich effect surveys

Diaferio

Nusser

Yoshida

et al. 2003

Monthly Notices of the Royal Astronomical Society

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We use a simple analytic model to compute the angular correlation function of clusters identified in upcoming thermal Sunyaev-Zel'dovich (SZ) effect surveys. We then compute the expected fraction of close pairs of clusters on the sky that are also close along the line of sight. We show how the expected number of cluster pairs as a function of redshift is sensitive to the assumed biasing relation between the cluster and the mass distribution. We find that, in a -cold dark matter model, the fraction of physically associated pairs is 70 per cent for angular separations smaller than 20 arcmin and clusters with a specific flux difference larger than 200 mJy at 143 GHz. The agreement of our analytic results with the Hubble volume N-body simulations is satisfactory. These results quantify the feasibility of using SZ surveys to compile catalogues of superclusters at any redshift.

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“…If Equation (11) were a 5D free particle Lagrangian for x α ( ξ ), then the Euler–Lagrange equations would provide geodesic equations

0 = \frac{D {\overset{x}{true}}^{γ}}{D ξ} = {\overset{x}{true}}^{γ} + Γ_{α β}^{γ} {\overset{x}{true}}^{α} {\overset{x}{true}}^{β},

where D / Dξ is the absolute derivative (in the notation of Weinberg [Weinberg ]) and

Γ_{α β}^{γ} = g^{γ δ} Γ_{δ α β} = \frac{1}{2} g^{γ δ} (\partial_{α} g_{δ β} + \partial_{β} g_{δ α} - \partial_{δ} g_{β α}),

is the standard Christoffel symbol in 5D.…”

Section: Canonical Mechanicsmentioning

confidence: 99%

Local metric with parameterized evolution

Land

2019

Astron Nachr

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We present a canonical Hamiltonian formulation of general relativity in which , the parameter of system evolution, is external to spacetime, playing a role similar to what we call time in nonrelativistic mechanics. This approach, known as Stueckelberg-Horwitz-Piron (SHP) theory, inherits the full computational power of classical analytical mechanics while maintaining manifest covariance throughout and eliminating possible conflict with general diffeomorphism invariance. In particular, SHP theory simplifies the initial value problem with potential applications in highly dynamical interactions, such as black hole collisions. By allowing the energy-momentum tensor and metric to depend explicitly on , we may describe particle motion in geodesic form with respect to a dynamically evolving background metric. As a toy model, we consider a -dependent mass M( ), first as a perturbation in the Newtonian approximation and then for a Schwarzschild-like metric. As expected, the extended Einstein equations imply a nonzero energy-momentum tensor, proportional to dM/d , representing a flow of mass and energy into spacetime that corresponds to the changing source mass. In -equilibrium, this system becomes a generalized Schwarzschild solution for which the extended Ricci tensor and energy-momentum tensor vanish. K E Y W O R D Sgeneral relativity, evolution theories, initial value problem Astron. Nachr. / AN. 2019;340:983-988.www.an-journal.org

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Gravitation and Cosmology: Principles and Applications of the General Theory of Relativity

Cited by 2,344 publications

References 0 publications

How dark matter came to matter

How dark matter came to matter

Superclusters with thermal Sunyaev--Zel'dovich effect surveys

Local metric with parameterized evolution

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