321 research outputs found
Quantum phase transition in HTSC thick films: YBa2Cu 3O x, YBa2Cu3O x (5 % Ag-Doped) in a Strong Pulsed Magnetic Field up to 32 T at low temperatures (58-100 K), current densities and stress-effect
We have researched the influence of pulsed magnetic fields up to 32 T on the magneto-resistance of thick films (50 Mk) of YBa2Cu3O x and YBa2Cu3O x (5 % Ag-doped) that were produced from synthesized powders. (Figs. 1-9): concentrate with 6.85-6.9 % O2 and a tail fraction 6.5-6.6 % O2. We observed a linear plot at currents of more than 1 mA at 77 K in YBa2Cu 3O x (5 % Ag-doped) at B>5 T and in the concentrate YBa2Cu3O x samples with I=1 mA, T=68.2 K. Pulsed magnetic fields up to 32 T, at I=1 mA had practically no influence on the value of the magneto-resistance in the concentrate YBa2Cu 3O x specimens at T=57.9 K and up to 17 T for YBa 2Cu3O x (5 % Ag) at 77 K (Meissner effect). However, for B>17 T, YBa2Cu3O x (5 % Ag) at 77 K demonstrates a tendency toward lower resistance. In the presence to 10 pulses in a cyclic pulsed magnetic field of 32 T, there is a sharp change of magnetic properties of an HTSC that can lead to nontrivial changes in the transition temperature, due to the strong mechanic stresses, sharp change value structure, and because one of the phases becomes superconducting (Figs. 3A, 3B). The behavior of the magnetoresistance of S-N-S contacts in pulsed magnetic fields is described via the system's parallel resistance, R n, and the inductance, L S-N-S. Analysis of microscopic models of quantum phase transitions was made in a granular superconductor in an attempt to explain the results on the studied HTSC-films and to give a physical interpretation to the deduced parameters of some experiments on the basis of "spin (vortex) glass" (vortex ice). © 2012 Springer Science+Business Media New York
Spin-orientation-dependent spatial structure of a magnetic acceptor state in a zincblende semiconductor
The spin orientation of a magnetic dopant in a zincblende semiconductor
strongly influences the spatial structure of an acceptor state bound to the
dopant. The acceptor state has a roughly oblate shape with the short axis
aligned with the dopant's core spin. For a Mn dopant in GaAs the local density
of states at a site 8 angstrom away from the dopant can change by as much by
90% when the Mn spin orientation changes. These changes in the local density of
states could be probed by scanning tunneling microscopy to infer the magnetic
dopant's spin orientation.Comment: 5 pages, 4 figure
Magnetotransport in Double Quantum Well with Inverted Energy Spectrum: HgTe/CdHgTe
We present the first experimental study of the double-quantum-well (DQW)
system made of 2D layers with inverted energy band spectrum: HgTe. The
magnetotransport reveals a considerably larger overlap of the conduction and
valence subbands than in known HgTe single quantum wells (QW), which may be
regulated by an applied gate voltage . This large overlap manifests itself
in a much higher critical field separating the range above it where the
quantum peculiarities shift linearly with and the range below with a
complicated behavior. In the latter case the -shaped and double--shaped
structures in the Hall magnetoresistance are observed with their
scale in field pronouncedly enlarged as compared to the pictures observed in an
analogous single QW. The coexisting electrons and holes were found in the whole
investigated range of positive and negative as revealed from fits to the
low-field -shaped and from the Fourier analysis of
oscillations in . A peculiar feature here is that the found
electron density remains almost constant in the whole range of investigated
while the hole density drops down from the value a factor of 6 larger
than at extreme negative to almost zero at extreme positive
passing through the charge neutrality point. We show that this difference
between and stems from an order of magnitude larger density of states
for holes in the lateral valence band maxima than for electrons in the
conduction band minimum. We interpret the observed reentrant sign-alternating
between electronic and hole conductivities and its zero
resistivity state in the quantum Hall range of fields on the basis of a
calculated picture of magnetic levels in a DQW.Comment: 15 pages, 13 figure
The variation of the magnetic field of the Ap star HD~50169 over its 29 year rotation period
Context. The Ap stars that rotate extremely slowly, with periods of decades
to centuries, represent one of the keys to the understanding of the processes
leading to the differentiation of stellar rotation.
Aims. We characterise the variations of the magnetic field of the Ap star HD
50169 and derive constraints about its structure.
Methods. We combine published measurements of the mean longitudinal field
of HD 50169 with new determinations of this field moment from circular
spectropolarimetry obtained at the 6-m telescope BTA of the Special
Astrophysical Observatory of the Russian Academy of Sciences. For the mean
magnetic field modulus , literature data are complemented by the analysis of
ESO spectra, both newly acquired and from the archive. Radial velocities are
also obtained from these spectra.
Results. We present the first determination of the rotation period of HD
50169, Prot = (29.04+/-0.82) y. HD 50169 is currently the longest-period Ap
star for which magnetic field measurements have been obtained over more than a
full cycle. The variation curves of both and have a significant degree
of anharmonicity, and there is a definite phase shift between their respective
extrema. We confirm that HD 50169 is a wide spectroscopic binary, refine its
orbital elements, and suggest that the secondary is probably a dwarf star of
spectral type M.
Conclusions. The shapes and mutual phase shifts of the derived magnetic
variation curves unquestionably indicate that the magnetic field of HD 50169 is
not symmetric about an axis passing through its centre. Overall, HD 50169
appears similar to the bulk of the long-period Ap stars.Comment: 10 pages, 3 figures, accepted for publication in A&
Search for stellar spots in field blue horizontal-branch stars
Blue horizontal-branch stars are Population II objects which are burning
helium in their core and possess a hydrogen-burning shell and radiative
envelope. Because of their low rotational velocities, diffusion has been
predicted to work in their atmospheres. In many respects, blue
horizontal-branch stars closely resemble the magnetic chemically peculiar stars
of the upper main sequence, which show photometric variability caused by
abundance spots on their surfaces. These spots are thought to be caused by
diffusion and the presence of a stable magnetic field. However, the latter does
not seem to be axiomatic. We searched for rotationally induced variability in
30 well-established bright field blue horizontal-branch stars in the solar
neighbourhood and searched the literature for magnetic fields measurements of
our targets. We employed archival photometric time series data from the ASAS,
ASAS-SN, and SuperWASP surveys. The data were carefully reduced and processed,
and a time series analysis was applied using several different techniques. We
also synthesized existing photometric and spectroscopic data of magnetic
chemically peculiar stars in order to study possible different surface
characteristics producing lower amplitudes. In the accuracy limit of the
employed data, no significant variability signals were found in our sample
stars. The resulting upper limits for variability are given. We conclude that
either no stellar surface spots are present in field blue horizontal-branch
stars, or their characteristics (contrast, total area, and involved elements)
are not sufficient to produce amplitudes larger than a few millimagnitudes in
the optical wavelength region. New detailed models taking into account the
elemental abundance pattern of blue horizontal-branch stars are needed to
synthesize light curves for a comparison with our results.Comment: 6 pages, 2 figures, 2 tables, accepted for publication in Astronomy &
Astrophysic
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