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RISS 인기검색어
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- 저자 : Ipatov, S. (검색결과 4 건)
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GMI Effect of Amorphous Microwires with Enhanced Magnetic Softness
A. Zhukov,M. Ipatov,A. Talaat,V. Zhukova,C. Garcia 한국물리학회 2013 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.62 No.10
We present our results on studies of soft magnetic properties and GMI effect in thin microwires at elevated frequencies paying special attention to tailoring the GMI effect and achievement of high GMI ratio (∆Z/Z), high magnetic field sensitivity (dZ/dH) with low hysteretic behavior. We measured magnetic field dependence of real part, of the longitudinal wire impedance up to frequency, f, 4 GHz in Co-rich microwires. We observed that the GMI magnetic field dependence can be tailored either controlling magnetoelastic anisotropy of as-prepared microwires or by heat treatment.
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GMR Effect in Co-Cu Microwires
V. Zhukova,J. J. del Val,M. Ilyn,M. Ipatov,R. Varga,C. Garcia,A. Zhukov 한국물리학회 2013 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.62 No.12
We studied magnetic properties and GMR effect of Cox − Cu100−x (10 ≤ x30 at%) microwires. We observed considerable magnetoresistance (MR), ΔR/R, in Co-Cu glass coated microwires withx = 10-30%. For low x content (x = 10), ΔR/R we observed negative MR, tending to saturate inhigh magnetic fields, H. On the other hand, for the samples x = 30 ΔR/R(H) dependences showednon-monotonic behavior, exhibiting R/R increase with H at low H-values (up to 5 kOe) and alsoconsiderable GMR effect. Temperature dependence of magnetization measured in samples cooled without magnetic field(zero field cooling, ZFC) and cooled under magnetic field (field cooled, FC) exhibit significantdifference for Cox Cu100−x (x = 30). For Cox Cu100−x (x = 10) microwires we observed a maximumat quite low temperature, indicating possibility of existence of some amount of small Co-grains. X-ray diffraction (XRD) results reveal that the structure of the metallic core is granular withtwo phases: the main one, fcc Cu (lattice parameter 3.61 °A), found in all samples and fcc -Co(lattice parameter 3.54 °A) which is present in microwires with higher Co content. In the case oflow Co content, XRD indicates that Co atoms are distributed within the Cu crystals. The quantityand the crystallite size of the formed phases strongly depend on the geometry of the microwire.
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A census of variability in globular cluster M 68 (NGC 4590)
Kains, N.,Arellano Ferro, A.,Figuera Jaimes, R.,Bramich, D. M.,Skottfelt, J.,Jørgensen, U. G.,Tsapras, Y.,Street, R. A.,Browne, P.,Dominik, M.,Horne, K.,Hundertmark, M.,Ipatov, S.,Snodgrass, C.,Steele EDP Sciences 2015 Astronomy and astrophysics Vol.578 No.-
<P>Aims. We analyse 20 nights of CCD observations in the V and I bands of the globular cluster M?68 (NGC 4590) and use them to detect variable objects. We also obtained electron-multiplying CCD (EMCCD) observations for this cluster in order to explore its core with unprecedented spatial resolution from the ground. Methods. We reduced our data using difference image analysis to achieve the best possible photometry in the crowded field of the cluster. In doing so, we show that when dealing with identical networked telescopes, a reference image from any telescope may be used to reduce data from any other telescope, which facilitates the analysis significantly. We then used our light curves to estimate the properties of the RR Lyrae (RRL) stars in M?68 through Fourier decomposition and empirical relations. The variable star properties then allowed us to derive the cluster’s metallicity and distance. Results. M?68 had 45 previously confirmed variables, including 42 RRL and 2 SX Phoenicis (SX Phe) stars. In this paper we determine new periods and search for new variables, especially in the core of the cluster where our method performs particularly well. We detect 4 additional SX Phe stars and confirm the variability of another star, bringing the total number of confirmed variable stars in this cluster to 50. We also used archival data stretching back to 1951 to derive period changes for some of the single-mode RRL stars, and analyse the significant number of double-mode RRL stars in M?68. Furthermore, we find evidence for double-mode pulsation in one of the SX Phe stars in this cluster. Using the different classes of variables, we derived values for the metallicity of the cluster of [Fe/H] = −2.07 ±0.06 on the ZW scale, or −2.20 ±0.10 on the UVES scale, and found true distance moduli μ0 = 15.00±0.11 mag (using RR0 stars), 15.00 ± 0.05 mag (using RR1 stars), 14.97 ±0.11 mag (using SX Phe stars), and 15.00±0.07 mag (using the MV–[Fe/H] relation for RRL stars), corresponding to physical distances of 10.00 ±0.49, 9.99±0.21, 9.84 ±0.50, and 10.00 ±0.30 kpc, respectively. Thanks to the first use of difference image analysis on time-series observations of M?68, we are now confident that we have a complete census of the RRL stars in this cluster.</P>
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