1,211 research outputs found
Inward Motions of the Compact SiO Masers Around VX Sagittarii
We report Very Long Baseline Array (VLBA) observations of 43 GHz v=1, J=1-0
SiO masers in the circumstellar envelope of the M-type semi-regular variable
star VX Sgr at 3 epochs during 1999 April-May. These high-resolution VLBA
images reveal a persistent ringlike distribution of SiO masers with a projected
radius of ~3 stellar radii. The typical angular size of 0.5 mas for individual
maser feature was estimated from two-point correlation function analysis for
maser spots. We found that the apparent size scale of maser features was
distinctly smaller than that observed in the previous observations by comparing
their fractions of total power imaged. This change in the size scale of maser
emission may be related to stellar activity that caused a large SiO flare
during our observations. Our observations confirmed the asymmetric distribution
of maser emission, but the overall morphology has changed significantly with
the majority of masers clustering to the north-east of the star compared to
that lying to the south-west direction in 1992. By identifying 42 matched maser
features appearing in all the three epochs, we determined the contraction of an
SiO maser shell toward VX Sgr at a proper motion of -0.507 mas/yr,
corresponding to a velocity of about 4 km/s at a distance of 1.7 kpc to VX Sgr.
Such a velocity is on the order of the sound speed, and can be easily explained
by the gravitational infall of material from the circumstellar dust shell.Comment: 26 pages, 5 figures, 4 tables, accepted for publication in Ap
Axial Symmetry and Rotation in the SiO Maser Shell of IK Tauri
We observed v=1, J=1-0 43-GHz SiO maser emission toward the Mira variable IK
Tauri (IK Tau) using the Very Long Baseline Array (VLBA). The images resulting
from these observations show that SiO masers form a highly elliptical ring of
emission approximately 58 x 32 mas with an axial ratio of 1.8:1. The major axis
of this elliptical distribution is oriented at position angle of ~59 deg. The
line-of-sight velocity structure of the SiO masers has an apparent axis of
symmetry consistent with the elongation axis of the maser distribution.
Relative to the assumed stellar velocity of 35 km/s, the blue- and red-shifted
masers were found to lie to the northwest and southeast of this symmetry axis
respectively. This velocity structure suggests a NW-SE rotation of the SiO
maser shell with an equatorial velocity, which we determine to be ~3.6 km/s.
Such a NW-SE rotation is in agreement with a circumstellar envelope geometry
invoked to explain previous water and OH maser observations. In this geometry,
water and OH masers are preferentially created in a region of enhanced density
along the NE-SW equator orthogonal to the rotation/polar axis suggested by the
SiO maser velocities.Comment: 17 Pages, 4 figures (2 color); accepted for publication in Ap
Staying in touch in the digital era: New social work practice
The findings of a small-scale empirical study are drawn upon to explore the concept of social presence and the way in which it can contribute to meeting service usersâ expectations of relationship-based social work. Findings from the study highlight the role of mobile communication technologies in establishing social presence with service users and an argument is made for the proactive use of mobile devices as a component of direct practice. However, such emerging digital social work practices will require practitioners, and social work organisations, to respond positively to new ethical and organisational challenges
Two-dimensional model of dynamical fermion mass generation in strongly coupled gauge theories
We generalize the Schwinger model on the lattice by adding a charged
scalar field. In this so-called model the scalar field shields
the fermion charge, and a neutral fermion, acquiring mass dynamically, is
present in the spectrum. We study numerically the mass of this fermion at
various large fixed values of the gauge coupling by varying the effective
four-fermion coupling, and find an indication that its scaling behavior is the
same as that of the fermion mass in the chiral Gross-Neveu model. This suggests
that the model is in the same universality class as the
Gross-Neveu model, and thus renormalizable and asymptotic free at arbitrary
strong gauge coupling.Comment: 18 pages, LaTeX2e, requires packages rotating.sty and curves.sty from
CTA
W(h)ither the academy? An exploration of the role of university social work in shaping the future of social work in Europe
A controversial proposal to pilot the training of child protection social workers through an intensive work-based route in England is being supported and funded by the UK Government. Frontline, the brainchild of a former teacher, locates social work training within local authorities (âthe agencyâ) rather than university social work departments (âthe academyâ) and has stimulated debate amongst social work academics about their role in shaping the direction of the profession. As a contribution to this debate, this paper explores the duality of social work education, which derives its knowledge from both the academic social sciences and the experience of practice within social work agencies. While social work education has traditionally been delivered by the academy, this paper also explores whether the delivery of training in the allied professions of probation and nursing by âthe agencyâ is equally effective. Finally, this paper explores the Helsinki model which achieves a synergy of âacademyâ and âagencyâ. It suggests that there are alternative models of social work education, practice and research which avoid dichotomies between the âacademyâ and the âagencyâ and enable the profession to be shaped by both social work academics and practitioners
Ginsparg-Wilson Fermions: A study in the Schwinger Model
Qualitative features of Ginsparg-Wilson fermions, as formulated by Neuberger,
coupled to two dimensional U(1) gauge theory are studied. The role of the
Wilson mass parameter in changing the number of massless flavors in the theory
and its connection with the index of the Dirac operator is studied. Although
the index of the Dirac operator is not related to the geometric definition of
the topological charge for strong couplings, the two start to agree as soon as
one goes to moderately weak couplings. This produces the desired singularity in
the quenched chiral condensate which appears to be very difficult to reproduce
with staggered fermions. The fermion determinant removes the singularity and
reproduces the known chiral condensate and the meson mass within understandable
errors.Comment: Corrected a few typos and changed some references. Minor changes to
the conten
Correlation between Infrared Colors and Intensity Ratios of SiO Maser Lines
We present the results of SiO millimeter-line observations of a sample of
known SiO maser sources covering a wide dust-temperature range. A cold part of
the sample was selected from the SiO maser sources found in our recent SiO
maser survey of cold dusty objects. The aim of the present research is to
investigate the causes of the correlation between infrared colors and SiO maser
intensity ratios among different transition lines. In particular, the
correlation between infrared colors and SiO maser intensity ratio among the
J=1-0 v=1, 2, and 3 lines are mainly concerned in this paper. We observed in
total 75 SiO maser sources with the Nobeyama 45m telescope quasi-simultaneously
in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines. We also observed the
sample in the 29SiO J=1-0 v=0 and J=2-1 v=0, and 30SiO J=1-0 v=0 lines, and the
H2O 6(1,6)-5(2,3) line. As reported in previous papers, we confirmed that the
intensity ratios of the SiO J=1-0 v=2 to v=1 lines clearly correlate with
infrared colors. In addition, we found possible correlation between infrared
colors and the intensity ratios of the SiO J=1-0 v=3 to v=1&2 lines. Two
overlap lines of H2O (i.e., 11(6,6) nu_2=1 -> 12(7,5) nu_2=0 and 5(0,5) nu_2=2
-> 6(3,4) nu_2=1) might explain these correlation if these overlap lines become
stronger with increase of infrared colors, although the phenomena also might be
explained by more fundamental ways if we take into account the variation of
opacity from object to object.Comment: 49 pages, 7 figures, 3 tables, accepted for publication in ApJ. Full
resolution version available at
http://www.asiaa.sinica.edu.tw/~junichi/paper
Semliki Forest virus induced, immune mediated demyelination: the effect of irradiation
International audienceThe Dark Energy Camera has captured a large set of images as part of Science Verification (SV) for the Dark Energy Survey (DES). The SV footprint covers a large portion of the outer Large Magellanic Cloud (LMC), providing photometry 1.5 mag fainter than the main sequence turn-off of the oldest LMC stellar population. We derive geometrical and structural parameters for various stellar populations in the LMC disc. For the distribution of all LMC stars, we find an inclination of i = -38.14° ± 0.08° (near side in the north) and a position angle for the line of nodes of Ξ0 = 129.51° ± 0.17°. We find that stars younger than âŒ4 Gyr are more centrally concentrated than older stars. Fitting a projected exponential disc shows that the scale radius of the old populations is R>4 Gyr = 1.41 ± 0.01 kpc, while the younger population has R = 0.72 ± 0.01 kpc. However, the spatial distribution of the younger population deviates significantly from the projected exponential disc model. The distribution of old stars suggests a large truncation radius of Rt = 13.5 ± 0.8 kpc. If this truncation is dominated by the tidal field of the Galaxy, we find that the LMC is {âŒeq } 24^{+9}_{-6} times less massive than the encircled Galactic mass. By measuring the Red Clump peak magnitude and comparing with the best-fitting LMC disc model, we find that the LMC disc is warped and thicker in the outer regions north of the LMC centre. Our findings may either be interpreted as a warped and flared disc in the LMC outskirts, or as evidence of a spheroidal halo component
Hamiltonian lattice QCD at finite density: equation of state in the strong coupling limit
The equation of state of Hamiltonian lattice QCD at finite density is
examined in the strong coupling limit by constructing a solution to the
equation of motion corresponding to an effective Hamiltonian describing the
ground state of the many body system. This solution exactly diagonalizes the
Hamiltonian to second order in field operators for all densities and is used to
evaluate the vacuum energy density from which we obtain the equation of state.
We find that up to and beyond the chiral symmetry restoration density the
pressure of the quark Fermi sea can be negative indicating its mechanical
instability. Our result is in qualitative agreement with continuum models and
should be verifiable by future lattice simulations of strongly coupled QCD at
finite density.Comment: 27 pages, 6 figures. Uses ReVTeX4 and BiBTeX. Revised versio
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