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A New Analytical Solution for the Distance Modulus in Flat Cosmology
, 2019 Lorenzo Zaninetti
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Weighted mining of massive collections of [Formula: see text]-values by convex optimization. [PDF]
Inf inference, 2018 Dobriban E.
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Water equivalent path length measurement in proton radiotherapy using time resolved diode dosimetry. [PDF]
Med Phys, 2011 Gottschalk B +5 more
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Nöther's symmetries in non-flat cosmologies
Il Nuovo Cimento B Series 11, 1994We study non-flat Friedman-Robertson-Walker (FRW) cosmologies searching for Nother symmetries in the pointlike Lagrangians derived from a general non-minimally coupled gravitational action. The presence of a quadratic coupling makes the dynamics degenerate if the spatial-curvature constantk is different from zero, while exact solutions, through the ...
Capozziello S. +2 more
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A spatially-flat cosmological model
Astrophysics and Space Science, 1993zbMATH Open Web Interface contents unavailable due to conflicting licenses.
Israelit, Mark, Rosen, Nathan
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Evolution of multidimensional flat anisotropic cosmological models
Physical Review D, 1993We study the dynamics of a flat multidimensional anisotropic cosmological model filled with an anisotropic fluidlike medium. By an appropriate choice of variables, the dynamical equations reduce to a two-dimensional dynamical system. We present a detailed analysis of the time evolution of this system and the conditions of the existence of spacetime ...
, Beloborodov +3 more
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Dilatons, flatness, and the cosmological constant
Physical Review D, 1988Symmetries that exist for some theories when considering small perturbations around some special backgrounds, which include flat but not de Sitter space and, among cosmological solutions spatially flat but generally not k = +- 1 Robertson-Walker solutions, are studied.
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Flat universe with decaying cosmological constant
The European Physical Journal Plus, 2014We have investigated the Robertson-Walker cosmological model with decaying vacuum density. We considered a special variation law in which the vacuum density Λ is proportional to the n-th power of the Hubble parameter H, i.e., Λ ∝ H n (where n is a constant) (Phys. Rev. D 58, 043506 (1998)).
R. K. Tiwari, Rameshwar Singh
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