Numerical Analysis for the Transport Properties of the Oxide S-N-S Junction

The Quenching of the Ultra-Faint Dwarf Galaxies in the Reionization Era

“…While UMa I is dominated by old metal-poor stars, it appears to be systematically younger than the other galaxies in our sample. UMa I may be distorted, and Okamoto et al (2008) argue that it appears to be undergoing disruption; elongation along our sightline could be broadening the CMD, producing an apparent age spread. Hercules is the brightest galaxy in our sample (M v = −6.6 mag; Martin et al 2008b); it may have retained more gas during the reionization era, leading to a non-negligible population of younger stars.…”

“…An appropriate object is the Galactic globular cluster M92 -one of the most ancient and metal-poor stellar systems known. Of the globular clusters with little extinction, it is the most metal-poor (Harris 1996), and it has served as a reference population in previous studies of UFDs (e.g., Belokurov et al 2006Belokurov et al , 2007Belokurov et al , 2009Belokurov et al , 2010Okamoto et al 2008Okamoto et al , 2012Sand et al 2009Sand et al , 2010Sand et al , 2012. It was observed with the same camera and filters by Brown et al (2005), and its CMD is shown in Figure 4.…”

“…Photometric and spectroscopic observations of the UFD galaxies have shown that they are excellent candidates for demonstrating the existence of fossil galaxies. Colormagnitude diagrams (CMDs) indicate the UFDs are generally dominated by old (>10 Gyr) populations (e.g., Sand et al 2009Sand et al , 2010Okamoto et al 2008Okamoto et al , 2010Okamoto et al , 2012de Jong et al 2008b;Hughes et al 2008;Martin et al 2008a;Greco et al 2008;Muñoz et al 2010;Weisz et al 2014b), while spectroscopy of their giant stars indicates low metallicities, but with a dispersion significantly larger than the measurement errors Norris et al 2010;Kirby et al 2008Kirby et al , 2011Kirby et al , 2013. The internal kinematics from such spectroscopy also imply large mass-to-light ratios (M/L V 100; e.g., Kleyna et al 2005;Muñoz et al 2006;Martin et al 2007;Simon & Geha 2007).…”

Orbital ordering inLaMnO3:Electron-electron and electron-lattice interactions

“…The theoretical results of the Raman spectra from the orbital wave agree with the polarization dependence of the spectra and their relative intensities in experiment. 40 Since the characteristic energy of the orbital excitation is much higher than that of the lattice vibration, we introduce the adiabatic approximation for the lattice degree of freedom in the calculation of the orbital wave. Then, the energy of orbital wave is approximately given by ω orb = (3J 1 +…”

Phase transition in perovskite manganites with orbital degree of freedom

“…The mean field theory proposed by de Gennes 24 is applied to the present system with orbital degeneracy and electron correlation. 25 In this theory, the spin and pseudo-spin operators are treated as classical vectors: (S ix , S iy , S iz ) = 1 2 (sin θ s i cos φ s i , sin θ s i sin φ s i , cos θ s i ), (5) and…”