arXiv subjects

M. Yahiro

Publications and source records attributed to M. Yahiro.

22 records · Page 2Linked to original sources

arXiv2003

New treatment of breakup continuum in the method of continuum discretized coupled channels

A new method of pseudo-state discretization is proposed for the method of continuum discretized coupled channels (CDCC) to deal with three-body breakup processes. We propose real- and complex-range Gaussian bases for the pseudo-state wave functions, and show that they form in good approximation a complete set in the configuration space which is important for breakup processes. Continuous S-matrix elements are derived with the approximate completeness from discrete ones calculated by CDCC. Accuracy of the method is tested quantitatively for two realistic examples, d+$^{58}$Ni scattering at 80 MeV and $^{6}$Li+$^{40}$Ca scattering at 156 MeV with the satisfactory results. Possibility of application of the method to four-body breakup processes is also discussed.

nucl-th↗

arXiv2002

Observational Constraints on Dark Radiation in Brane Cosmology

We analyze the observational constraints on brane-world cosmology whereby the universe is described as a three-brane embedded in a five-dimensional anti-de Sitter space. In this brane-universe cosmology, the Friedmann equation is modified by the appearance of extra terms which derive from existence of the extra dimensions. In the present work we concentrate on the ``dark radiation'' term which diminishes with cosmic scale factor as $a^{-4}$. We show that, although the observational constraints from primordial abundances allow only a small contribution when this term is positive, a much wider range of negative values is allowed. Furthermore, such a negative contribution can reconcile the tension between the observed primordial $\he4$ and D abundances. We also discuss the possible constraints on this term from the power spectrum of CMB anisotropies in the limit of negligible cosmological perturbation on the brane world. We show that BBN limits the possible contribution from dark radiation just before the nucleosynthesis epoch to lie between -65% and $+5%$ of the background photon energy density. Combining this with the CMB constraint reduces this range to between -24% and $+3.5%$ at the $2σ$ confidence level.

astro-ph↗

arXiv2002

Constrainting Cosmic Quintessence

A generic feature of cosmic quintessence models is the possibility of significant energy density in the scalar field during the radiation dominated epoch. This possibility is even greater if the quintessence field begins in a kinetic-dominated regime, for example as might be generated at the end of "quintessential inflation." As such, these models can be constrained by primordial nucleosynthesis and the epoch of photon decoupling. Here, we analyze both kinetic dominated and power-law quintessence fields (with and without a supergravity correction). We quantify the allowed initial conditions and effective-potential parameters. We also deduce constraints on the epoch of matter creation at the end of quintessential inflation.

astro-ph↗

arXiv2002

Constraints on Cosmic Quintessence and Quintessential Inflation

Recently, attempts have been made to understand the apparent near coincidence of the present dark energy and matter energy in terms of a dynamical attractor-like solution for the evolution of a scalar field. In these models the field couples with the dominant constituent and only acts like a cosmological constant after the onset of the matter-diminated epoch. A generic feature of such solutions, however, is the possibility of significant energy density in the scalar field during the radiation-dominated epoch. This possibility is even greater if the quintessence field begins in a kinetic-dominated regime generated at the end of quintessential inflation. As such, these models can affect and be constrained by primordial nucleosynthesis and the epoch of of photon decoupling. Here, we analyze one popular form of the quintessence field (with and without a supergravity correction) and quantify constraints on the allowed initial conditions and parameters for the effective potential. We also deduce constraints on the epoch of matter creation at the end of quintessential inflation.

astro-ph↗