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GMR in Multilayers with an Alternating In - plane and Perpendicular Anisotropy
F. Stobiecki,B. Szymański,T. Luciñski,J. Dubowik,M. Urbaniak,K. Röll,J. B. Kim,K. W. Kim,Y. P. Lee 한국자기학회 2004 Journal of Magnetics Vol.9 No.2
The magnetic properties of sputtered (Ni_(83)Fe_(17)/Au/Co/Au) multilayers with various thicknesses of Au (0.5 ≤ t_(Au) ≤ 3 ㎚), Ni-Fe (1 ≤ t_(Ni-Fe) ≤ 4 ㎚) and Co (0.2 ≤ t_(Co) ≤ 1.5 ㎚) layers were characterized. An alternating inplane and out-of-plane anisotropy of the ferromagnetic layers was achieved for the structures (t_(Au)≥ 1.5 ㎚) showing a weak coupling between the Ni-Fe layers with an in-plane anisotropy and the Co layers (0.3 ≤ t_(Co) ≤ 1.2 ㎚) with a perpendicular anisotropy. For such a structure, a detailed discussion on the GMR effect is presented, relating to the magnetization reversal from a mutually perpendicular magnetic configuration at the remanence to a parallel one at the saturation. An influence of the dense labyrinth domain structure on the magnetoresistance effect is also addressed.
Solar neutrino measurements in Super-Kamiokande-IV
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Marti, Ll.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, M.,Sonoda, Y.,Takeda, A. American Physical Society 2016 Physical Review D Vol.94 No.5
<P>Upgraded electronics, improved water system dynamics, better calibration and analysis techniques allowed Super-Kamiokande-IV to clearly observe very low-energy B-8 solar neutrino interactions, with recoil electron kinetic energies as low as similar to 3.5 MeV. Super-Kamiokande-IV data-taking began in September of 2008; this paper includes data until February 2014, a total livetime of 1664 days. The measured solar neutrino flux is (2.308 +/- 0.020)(stat)(-0.040)(+0.039) (syst)) x 10(6)/(cm(2) sec) assuming no oscillations. The observed recoil electron energy spectrum is consistent with no distortions due to neutrino oscillations. An extended maximum likelihood fit to the amplitude of the expected solar zenith angle variation of the neutrino-electron elastic scattering rate in SK-IV results in a day/night asymmetry of (-3.6 +/- 1.6(stat) +/- 0.6(syst)%. The SK-IV solar neutrino data determine the solar mixing angle as sin(2)theta(12) = 0.327(-0.031)(+0.026), all SK solar data (SK-I, SK-II, SK III and SK-IV) measures this angle to be sin(2)theta(12) = 0.334(-0.023)(+0.027), the determined mass-squared splitting is Delta m(21)(2) = 4.8(-0.8)(+1.5) x 10(-5) eV(2).</P>