6,201 research outputs found
RadioAstron probes the ultra-fine spatial structure in the HO maser emission in the star forming region W49N
HO maser emission associated with the massive star formation region W49N
were observed with the Space-VLBI mission RadioAstron. The procedure for
processing of the maser spectral line data obtained in the RadioAstron
observations is described. Ultra-fine spatial structures in the maser emission
were detected on space-ground baselines of up to 9.6 Earth diameters. The
correlated flux densities of these features range from 0.1% to 0.6% of the
total flux density. These low values of correlated flux density are probably
due to turbulence either in the maser itself or in the interstellar medium.Comment: Accepted for publication in Advances in Space Researc
H-Dihyperon in Quark Cluster Model
The H dihyperon (DH) is studied in the framework of the SU(3) chiral quark
model. It is shown that except the chiral field, the overall effect of
the other SU(3) chiral fields is destructive in forming a stable DH. The
resultant mass of DH in a three coupled channel calculation is ranged from 2225
to 2234 .Comment: 9 pages, emte
Intra-Landau level polarization effect for a striped Hall gas
We calculate the polarization function including only intra-Landau level
correlation effects of striped Hall gas. Using the polarization function, the
dielectric function, the dispersion of the plasmon and the correlation energy
are computed in a random phase approximation (RPA) and generalized random phase
approximation (GRPA). The plasmon becomes anisotropic and gapless owing to the
anisotropy of the striped Hall gas and two dimensionality of the quantum Hall
system. The plasmon approximately agrees with the phonon derived before by the
single mode approximation. The (G)RPA correlation energy is compared with other
numerical calculations.Comment: 15 pages,15 figures, revtex4, published versio
High-dose paroxetine treatment for an adolescent with obsessive-compulsive disorder comorbid with Asperger's disorder
The definitive version is available at www.blackwell-synergy.comArticlePSYCHIATRY AND CLINICAL NEUROSCIENCES. 63(2):251 (2009)journal articl
Nonmagnetic impurity perturbation to the quasi-two-dimensional quantum helimagnet LiCu2O2
A complete phase diagram of Zn substituted quantum quasi-two-dimensional
helimagnet LiCu2O2 has been presented. Helical ordering transition temperature
(T_h) of the original LiCu2O2 follows finite size scaling for less than ~ 5.5%
Zn substitution, which implies the existence of finite helimagnetic domains
with domain boundaries formed with nearly isolated spins. Higher Zn
substitution > 5.5% quenches the long-range helical ordering and introduces an
intriguing Zn level dependent magnetic phase transition with slight thermal
hysteresis and a universal quadratic field dependence for T_c (Zn > 0.055,H).
The magnetic coupling constants of nearest-neighbor (nn) J1 and
next-nearest-neighbor (nnn) J2 (alpha=J2/J1) are extracted from high
temperature series expansion (HTSE) fitting and N=16 finite chain exact
diagonalization simulation. We have also provided evidence of direct
correlation between long-range helical spin ordering and the magnitude of
electric polarization in this spin driven multiferroic material
Complex organics in IRAS 4A revisited with ALMA and PdBI: Striking contrast between two neighbouring protostellar cores
We used the Atacama Large (sub-)Millimeter Array (ALMA) and the IRAM Plateau
de Bure Interferometer (PdBI) to image, with an angular resolution of 0.5
(120 au) and 1 (235 au), respectively, the emission from 11 different
organic molecules in the protostellar binary NGC1333 IRAS 4A. We clearly
disentangled A1 and A2, the two protostellar cores present. For the first time,
we were able to derive the column densities and fractional abundances
simultaneously for the two objects, allowing us to analyse the chemical
differences between them. Molecular emission from organic molecules is
concentrated exclusively in A2 even though A1 is the strongest continuum
emitter. The protostellar core A2 displays typical hot corino abundances and
its deconvolved size is 70 au. In contrast, the upper limits we placed on
molecular abundances for A1 are extremely low, lying about one order of
magnitude below prestellar values. The difference in the amount of organic
molecules present in A1 and A2 ranges between one and two orders of magnitude.
Our results suggest that the optical depth of dust emission at these
wavelengths is unlikely to be sufficiently high to completely hide a hot corino
in A1 similar in size to that in A2. Thus, the significant contrast in
molecular richness found between the two sources is most probably real. We
estimate that the size of a hypothetical hot corino in A1 should be less than
12 au. Our results favour a scenario in which the protostar in A2 is either
more massive and/or subject to a higher accretion rate than A1, as a result of
inhomogeneous fragmentation of the parental molecular clump. This naturally
explains the smaller current envelope mass in A2 with respect to A1 along with
its molecular richness.Comment: Accepted in Astronomy and Astrophysic
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