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In models with Ων ≤ 0.4 and scale-invariant spectrum of density perturbations (n = 1), T/S⪆10(h - 0.47).
This normalization of the spectrum of density perturbations has been used to calculate numerically the value of the large scale CMB anisotropy and the relative contribution of cosmological gravitational waves, T/S.
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We show that the considered models admit both moderate red and blue spectra of density perturbations n ∈ [0.9, 1.2] with rather high abundance hot dark matter, Ων ∈ [0.2, 0.4].
Beverland, M. E. et al. Spectrum estimation of density operators with alkaline-earth atoms.
A method is presented for the description of a heterogeneous cell population with respect to the volume and density of its cellular components, based on computer analysis of the cell-volume spectra of density-gradient fractions.
Abstract: We introduce "anamorphic" cosmology, an approach for explaining the smoothness and flatness of the universe on large scales and the generation of a nearly scale-invariant spectrum of adiabatic density perturbations.
Using this approach, we can investigate the expected dependence of structure characteristics upon the mass of dark matter particles and/or the shape of small scale power spectrum of initial density perturbations.
Fig. 6 a Wavelet power spectrum of the density residual at 550 km altitude.
EPBs contain a broad spectrum of plasma density irregularities, as measured by sounding rockets and satellites.
Quantifying the small-scale structure of dark matter halos, which is influenced by the spectrum of primordial density fluctuations and the micro-physics of dark matter, can allow us to probe multiple areas of fundamental physics.
I will show how a phase of slow contraction before the big bang can explain the observed degree of flatness and homogeneity of our universe, as well as generate a nearly scale-invariant spectrum of primordial density perturbations.
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Justyna Jupowicz-Kozak
CEO of Professional Science Editing for Scientists @ prosciediting.com