Dynamical electron mass in a strong magnetic field

Abstract

Motivated by recent interest in understanding properties of strongly magnetized matter, we study the dynamical electron mass generated through approximate chiral symmetry breaking in QED in a strong magnetic field. We reliably calculate the dynamical electron mass by numerically solving the nonperturbative Schwinger-Dyson equations in a consistent truncation within the lowest Landau level approximation. It is shown that the generation of dynamical electron mass in a strong magnetic field is significantly enhanced by the perturbative electron mass that explicitly breaks chiral symmetry in the absence of a magnetic field.

Linear and non-linear perturbations in dark energy models

“…Currently, there is no strong observational evidence either for departures from w = −1 or for a time evolution of the dark energy EoS. However, since such results would be of great impact on cosmology, a number of studies on dark energy parameterisations have been discussed in the literature (see, e.g., [11][12][13][14][15][16] and references therein).…”

Forecasting cosmological constraints from age of high-zgalaxies

“…In our analyses, we follow Wang (2008) and consider a c = 2/3 (z c = 0.5), so that the above equation can be written in terms of z as…”

“…(6) is a rearrangement of parametrization (4) that minimizes the correlation between the parameters w 0 and w a and allows us to obtain tighter constraints on the parametric space. The parameters w 0.5 , w 0 , and w a are directly related by w 0.5 = w 0 + w a 3 (see Wang 2008;and Sendra & Lazkoz 2012, for more details).…”

“…For the dark energy EoS, w DE , we consider the CPL parametrization Wang (2008) derived an uncorrelated form for the above parameterization by rewriting it at the value a c (or, equivalently, z c ) at which the parameters w 0 and w a are uncorrelated, i.e.,…”

“…To this end, we assume the observational error distribution of a sample of 32 passively evolving galaxies studied by Simon et al (2005) and run Monte Carlo simulations to generate synthetic samples of galaxy ages with different sizes and characteristics. To perform our analysis we assume the so-called Chevalier-Polarski- Linder (CPL;Chevalier & Polarski 2001;Linder 2003) dark energy EoS parameterization and its uncorrelated form (Wang 2008). We discuss the improvement in the figure of merit (FoM) for the EoS parameters of both parameterizations with the size and precision of age samples as well as with the combination of age data and current baryonic acoustic oscillation (BAO) measurements.…”