Uréia para vacas leiteiras no pós-parto: teor plasmático de uréia e pH uterino

Oliveira, Margarida Maria Nascimento Figueirêdo de; Torres, Ciro Alexandre Alves; Costa, Eduardo Paulino da; Carvalho, G. A.

doi:10.1590/s1516-35982004000100016

Cited by 2 publications

(1 citation statement)

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“…Great worldwide efforts are currently being devoted to measuring CMB polarization in the hope of measuring the primordial gravitational wave amplitude Q t via large scale B-modes [115,116]. A key theoretical question is therefore what amplitude Q t to expect, since this determines the prospects for upcoming experiments to discover what they are looking for and influences their funding and design.…”

Section: Implications For Gravitational Waves and Spectral Indicesmentioning

confidence: 99%

What does inflation really predict?

Tegmark

2005

J. Cosmol. Astropart. Phys.

189

232

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If the inflaton potential has multiple minima, as may be expected in, e.g., the string theory "landscape", inflation predicts a probability distribution for the cosmological parameters describing spatial curvature (Ωtot), dark energy (ρΛ, w, etc.), the primordial density fluctuations (Q, ns, dns/d ln k, etc.) and primordial gravitational waves (r, nt, etc.). We compute this multivariate probability distribution for various classes of single-field slow-roll models, exploring its dependence on the characteristic inflationary energy scales, the shape of the potential V and and the choice of measure underlying the calculation. We find that unless the characteristic scale ∆φ on which V varies happens to be near the Planck scale, the only aspect of V that matters observationally is the statistical distribution of its peaks and troughs. For all energy scales and plausible measures considered, we obtain the predictions Ωtot ≈ 1 ± 10 −5 , w = −1 and ρΛ in the observed ballpark but uncomfortably high. The high energy limit predicts ns ≈ 0.96, dns/d ln k ≈ −0.0006, r ≈ 0.15 and nt ≈ −0.02, consistent with observational data and indistinguishable from eternal V ∝ φ 2 inflation. The low-energy limit predicts 5 parameters but prefers larger Q and redder ns than observed. We discuss the coolness problem, the smoothness problem and the pothole paradox, which severely limit the viable class of models and measures. Predictions insensitive to pre-inflationary conditions can arise either from eternal inflation attractor behavior or from anthropic selection effects probing merely a tiny non-special part of the initial distribution. We argue that these two mechanisms are severely challenged by the coolness problem and the smoothness problem, respectively. Our findings bode well for detecting an inflationary gravitational wave signature with future CMB polarization experiments, with the arguably best-motivated single-field models favoring the detectable level r ∼ 0.03.

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Section: Implications For Gravitational Waves and Spectral Indicesmentioning

confidence: 99%