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Hasegawa, S.,Shinozaki, K.,Honma, T.,Dimitrov, V.,Kim, H.G.,Komatsu, T. North-Holland 2016 Journal of non-crystalline solids Vol.452 No.-
<P>Glasses based on the system of Y2O3-BaO-Nb2O5-B2O3, corresponding to the pseudo-binary 64Ba(1 - x)Y(2x/3)Nb(2)O(6)-B2O3 with x = 0.1-0.5, were prepared, and their thermal properties, electronic polarizabilities, optical basicities, and crystallization behavior were clarified. The glasses showed the glass transition temperature of 602-610 degrees C, crystallization peak temperature of 686-676 degrees C, and refractive index of 1.967-2.007. All the glasses showed the bulk crystallization behavior, providing Ba1 - xY2x/3Nb2O6 nanocrystals with a tetragonal tungsten bronze structure. It was found from high resolution transmission electron microscope observations that the morphology of Ba1 - xY2x/3Nb2O6 nanocrystals is ellipsoidal and their average particle size is in the range of 20-40 nm. The glass-ceramics with Ba1 - xY2x/3Nb2O6 nanocrystals showed high dielectric constants (frequency: 1 kHz) of similar to 90 at room temperature and a ferroelectric nature. Highly oriented Ba1 - xY2x/3Nb2O6 crystal lines were patterned by laser (continuous wave Yb:YVO4 fiber laser with a wavelength of 1080 nm) irradiation with the condition of a laser power of 1.9 W and a laser scanning speed of 4 pm/s and with the laser focal position of 20 mu m beneath from the surface in 2NiO-1.1Y(2)O(3)-29.8BaO-33.1Nb(2)O(5)-36B(2)O(3) glass. (C) 2016 Elsevier B.V. All rights reserved.</P>
SAWADA-SATOH, S.,AKIYAMA, K.,NIINUMA, K.,NAGAI, H.,KINO, M.,D'AMMANDO, F.,KOYAMA, S.,HADA, K.,ORIENTI, M.,HONMA, M.,SHIBATA, K.M. The Korean Astronomical Society 2015 天文學論叢 Vol.30 No.2
We present a kinematic study of the parsec-scale radio jet in OJ 287, one of the most studied BL Lac objects, during ${\gamma}$-ray flares, to explore the relation between parsec-scale radio jet activity and ${\gamma}$-ray emission. The 22-GHz light curve of OJ 287 show three obvious flare events around 2011 May, 2011 October, and 2012 March. The second radio flare occurred during the ${\gamma}$-ray flaring period, and the third radio flare seemed to precede the ${\gamma}$-ray flare by one month. One jet component moved outward with respect to the core component with an apparent superluminal speed (~ 11c) from 2010 November to 2011 November. Then it changed direction, moving apparently inward in 2011 November, when the ${\gamma}$-ray flare occurred. The observed apparent inward motion of the jet at 22 GHz could be caused by a new jet component, unresolved at 22 GHz, in the innermost region.