7,363 research outputs found
Broken axisymmetry phase of a spin-1 ferromagnetic Bose-Einstein condensate
A spin-1 ferromagnetic Bose-Einstein condensate subject to a certain magnetic
field exhibits a broken-axisymmetry phase in which the magnetization tilts
against the applied magnetic field due to the competition between
ferromagnetism and linear and quadratic Zeeman effects. The Bogoliubov analysis
shows that in this phase two Goldstone modes associated with U(1) and SO(2)
symmetry breakings exist, in which phonons and magnons are coupled to restore
the two broken symmetries.Comment: 11 pages, 6 figure
Meissner effect in honeycomb arrays of multi-walled carbon nanotubes
We report Meissner effect for type-II superconductors with a maximum Tc of 19
K, which is the highest value among those in new-carbon related
superconductors, found in the honeycomb arrays of multi-walled CNTs (MWNTs).
Drastic reduction of ferromagnetic catalyst and efficient growth of MWNTs by
deoxidization of catalyst make the finding possible. The weak magnetic
anisotropy, superconductive coherence length (- 7 nm), and disappearance of the
Meissner effect after dissolving array structure indicate that the graphite
structure of an MWNT and those intertube coupling in the honeycomb array are
dominant factors for the mechanism.Comment: 6 page
X-Ray and Gamma-Ray Emission from the PSR 1259-63 / Be Star System
PSR 1259-63 is a radio pulsar orbiting a Be star in a highly eccentric orbit.
Soft and hard X-rays are observed from this binary system. We apply the shock
powered emission model to this system. The collision of the pulsar and Be star
winds forms a shock, which accelerates electrons and positrons to the
relativistic energies. We derive the energy distribution of relativistic
electrons and positrons as a function of the distance from the shock in the
pulsar nebula. We calculate the X-rays and -rays emitted from the
relativistic electrons and positrons in the nebula at various orbital phases,
taking into account the Klein-Nishina effect fully. The shock powered emission
model can explain the observed X-ray properties approximately. We obtain from
the comparison with observations that a fraction of of the pulsar
spin-down luminosity should be transformed into the relativistic electrons and
positrons. We find that the magnetization parameter of the pulsar wind, the
ratio of the Poynting flux to the kinetic energy flux, is
immediately upstream of the termination shock of the pulsar wind, and may
decrease with distance from the pulsar. We predict the flux of 10 MeV - 100 GeV
-rays which may be nearly equal to the detection threshold in the
future projects.Comment: 18 pages, 9 figures, accepted for publication in PAS
Field Theoretical Analysis of On-line Learning of Probability Distributions
On-line learning of probability distributions is analyzed from the field
theoretical point of view. We can obtain an optimal on-line learning algorithm,
since renormalization group enables us to control the number of degrees of
freedom of a system according to the number of examples. We do not learn
parameters of a model, but probability distributions themselves. Therefore, the
algorithm requires no a priori knowledge of a model.Comment: 4 pages, 1 figure, RevTe
1 um Excess Sources in the UKIDSS - I. Three T Dwarfs in the SDSS Southern Equatorial Stripe
We report the discovery of two field brown dwarfs, ULAS J0128-0041 and ULAS
J0321+0051, and the rediscovery of ULAS J0226+0051 (IfA 0230-Z1), in the Sloan
Digital Sky Survey (SDSS) southern equatorial stripe. They are found in the
course of our follow-up observation program of 1 um excess sources in the
United Kingdom Infrared Telescope Infrared Deep Sky Survey. The Gemini
Multi-Object Spectrographs spectra at red optical wavelengths (6500-10500 A)
are presented, which reveal that they are early-T dwarfs. The classification is
also supported by their optical to near-infrared colors. It is noted that ULAS
J0321+0051 is one of the faintest currently known T dwarfs. The estimated
distances to the three objects are 50-110 pc, thus they are among the most
distant field T dwarfs known. Dense temporal coverage of the target fields
achieved by the SDSS-II Supernova Survey allows us to perform a simple
time-series analysis, which leads to the finding of significant proper motions
of 150-290 mas/yr or the transverse velocities of 40-100 km/s for ULAS
J0128-0041 and ULAS J0226+0051. We also find that there are no detectable,
long-term (a-few-year) brightness variations above a few times 0.1 mag for the
two brown dwarfs.Comment: Accepted for publication in the Astronomical Journal; Typos correcte
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