TY - JOUR
T1 - Microscopic Studies on Y2Ba4Cu7O15-δby Use of TEM and NQR Techniques
AU - Kato, Masaki
AU - Nakanishi, Makoto
AU - Miyano, Toshio
AU - Shimizu, Tadashi
AU - Kakihana, Masato
AU - Yoshimura, Kazuyoshi
AU - Kosuge, Koji
N1 - Funding Information:
Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut f?r Radioastronomie (MPIfR) at Effelsberg. The Nan?ay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS). We acknowledge financial support from 'Programme National de Cosmologie and Galaxies' (PNCG) of CNRS/INSU, France. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope is supported by a consolidated grant from the STFC in the UK. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from The Netherlands Foundation for Scientific Research NWO. This research was performed using several supercomputers: the CCIN2P3 computer cluster of the CNRS-IN2P3 (Lyon-France), the ARAGO computer cluster of the Fran??ois Arago Centre (Paris-France), the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc using Strategic Research Infrastructure Funding from the Higher Education Funding Council for England and funding from the Science and Technology Facilities Council, and the Vulcan cluster of MPIfGAEI (Golm-Germany). The authors acknowledge the support of VirtualData from LABEX P2IO for providing computing resources through its StratusLab cloud. This work was supported in part by the National Science Foundation under grant no. PHYS-1066293 and the hospitality of the Aspen Center for Physics. LL was supported by a Junior Research Fellowship at Trinity Hall College, Cambridge University. ST was supported by appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. CMFM was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. AS and JG are supported by the Royal Society. SAS acknowledges funding from an NWO Vidi fellowship (PI JWTH). RNC acknowledges the support of the International Max Planck Research School Bonn/Cologne and the Bonn-Cologne Graduate School. KJL is supported by the National Natural Science Foundation of China (grant no.11373011). RvH is supported by NASA Einstein Fellowship grant PF3-140116. JWTH acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant 'DRAGNET' (337062). PL acknowledges the support of the International Max Planck Research School Bonn/Cologne. SO is supported by the Alexander von Humboldt Foundation.
Funding Information:
LL was supported by a Junior Research Fellowship at Trinity Hall College, Cambridge University. ST was supported by appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. CMFM was supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. AS and JG are supported by the Royal Society. SAS acknowledges funding from an NWO Vidi fellowship (PI JWTH). RNC acknowledges the support of the International Max Planck Research School Bonn/Cologne and the Bonn-Cologne Graduate School. KJL is supported by the National Natural Science Foundation of China (grant no.11373011). RvH is supported by NASA Einstein Fellowship grant PF3-140116. JWTH acknowledges funding from an NWO Vidi fellowship and ERC Starting Grant ‘DRAGNET’ (337062). PL acknowledges the support of the International Max Planck Research School Bonn/Cologne. SO is supported by the Alexander von Humboldt Foundation.
Funding Information:
This research was performed using several supercomputers: the CCIN2P3 computer cluster of the CNRS-IN2P3 (Lyon-France), the ARAGO computer cluster of the François Arago Centre (Paris-France), the Darwin Supercomputer of the University of Cambridge High Performance Computing Service (http://www.hpc.cam.ac.uk/), provided by Dell Inc using Strategic Research Infrastructure Funding from the Higher Education Funding Council for England and funding from the Science and Technology Facilities Council, and the Vulcan cluster of MPIfG-AEI (Golm-Germany). The authors acknowledge the support of VirtualData from LABEX P2IO for providing computing resources through its StratusLab cloud. This work was supported in part by the National Science Foundation under grant no. PHYS-1066293 and the hospitality of the Aspen Center for Physics.
Funding Information:
Part of this work is based on observations with the 100-m telescope of the Max-Planck-Institut für Radioastronomie (MPIfR) at Effelsberg. The Nanc¸ay radio Observatory is operated by the Paris Observatory, associated with the French Centre National de la Recherche Scientifique (CNRS). We acknowledge financial support from ‘Programme National de Cosmologie and Galaxies’ (PNCG) of CNRS/INSU, France. Pulsar research at the Jodrell Bank Centre for Astrophysics and the observations using the Lovell Telescope is supported by a consolidated grant from the STFC in the UK. The Westerbork Synthesis Radio Telescope is operated by the Netherlands Institute for Radio Astronomy (ASTRON) with support from The Netherlands Foundation for Scientific Research NWO.
PY - 1998/9
Y1 - 1998/9
N2 - Y2Ba4Cu7O15-δcompounds were characterized by microscopic investigation using TEM and NQR techniques. We synthesized Y247 compounds by two kinds of preparation methods: the conventional solid-state reaction (sample A) and the polymerized-complex method (sample B). The value ofTcfor sample A was found to be 65 K and that for sample B was 93 K by ac-χmeasurements. As a result of TEM experiments, stacking faults along thecaxis were observed more frequently in sample B than in sample A. These stacking faults resulted in microdomains containing pure Y123 or Y124 thin blocks of several unit cells. NQR experiments revealed that the microscopic environment of Cu(2) sites in sample A differed from either of those in the Y123 and Y124 compounds. NQR frequency values (νQ) of Cu(2) sites agreed well with those calculated by the point charge model applied for the Y247 structure. The spectra of Cu(2) sites in sample B could be regarded, however, as a combination of those of pure Y123, Y124, and also Y247 compounds. This fact was coincident with the result of TEM experiments. We concluded that the superconductivity of Y247 with higherTcoriginates from the thin block of Y123.
AB - Y2Ba4Cu7O15-δcompounds were characterized by microscopic investigation using TEM and NQR techniques. We synthesized Y247 compounds by two kinds of preparation methods: the conventional solid-state reaction (sample A) and the polymerized-complex method (sample B). The value ofTcfor sample A was found to be 65 K and that for sample B was 93 K by ac-χmeasurements. As a result of TEM experiments, stacking faults along thecaxis were observed more frequently in sample B than in sample A. These stacking faults resulted in microdomains containing pure Y123 or Y124 thin blocks of several unit cells. NQR experiments revealed that the microscopic environment of Cu(2) sites in sample A differed from either of those in the Y123 and Y124 compounds. NQR frequency values (νQ) of Cu(2) sites agreed well with those calculated by the point charge model applied for the Y247 structure. The spectra of Cu(2) sites in sample B could be regarded, however, as a combination of those of pure Y123, Y124, and also Y247 compounds. This fact was coincident with the result of TEM experiments. We concluded that the superconductivity of Y247 with higherTcoriginates from the thin block of Y123.
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U2 - 10.1006/jssc.1998.7840
DO - 10.1006/jssc.1998.7840
M3 - Article
AN - SCOPUS:0039400165
VL - 139
SP - 266
EP - 273
JO - Journal of Solid State Chemistry
JF - Journal of Solid State Chemistry
SN - 0022-4596
IS - 2
ER -