2,786 research outputs found
Magnetic flux pumping in 3D nonlinear magnetohydrodynamic simulations
A self-regulating magnetic flux pumping mechanism in tokamaks that maintains
the core safety factor at , thus preventing sawteeth, is analyzed
in nonlinear 3D magnetohydrodynamic simulations using the M3D-C code. In
these simulations, the most important mechanism responsible for the flux
pumping is that a saturated quasi-interchange instability generates
an effective negative loop voltage in the plasma center via a dynamo effect. It
is shown that sawtoothing is prevented in the simulations if is
sufficiently high to provide the necessary drive for the
instability that generates the dynamo loop voltage. The necessary amount of
dynamo loop voltage is determined by the tendency of the current density
profile to centrally peak which, in our simulations, is controlled by the
peakedness of the applied heat source profile.Comment: submitted to Physics of Plasmas (23 pages, 15 Figures
A High-Resolution Study of the HI Content of Local Group Dwarf Irregular Galaxy WLM
Dwarf irregular galaxies are unique laboratories for studying the interaction
between stars and the interstellar medium in low mass environments. We present
the highest spatial resolution observations to date of the neutral hydrogen
content of the Local Group dwarf irregular galaxy WLM. We find that WLM's
neutral hydrogen distribution is typical for a galaxy of its type and size and
derive an HI mass of 6.3e7 Msun for WLM. In addition, we derive an HI extent
for WLM of 30 arcmin, which is much less than the 45 arcmin extent found by
Huchtmeier, Seiradakis, and Materne (1981). We show that the broken ring of
high column density neutral hydrogen surrounding the center of WLM is likely
the result of star formation propagating out from the center of the galaxy. The
young stars and Ha emission in this galaxy are mostly correlated with the high
column density neutral hydrogen. The gap in the central ring is the result of
star formation in that region using up, blowing out, or ionizing all of the
neutral hydrogen. Like many late-type galaxies, WLM's velocity field is
asymmetric with the approaching (northern) side appearing to be warped and a
steeper velocity gradient for the approaching side than for the receding side
in the inner region of the galaxy. We derive a dynamical mass for WLM of 2.16e9
Msun.Comment: 38 pages, 15 figures, 5 tables, accepted by AJ, high resolution
version at http://www.astro.wisc.edu/~kepley/kepley_wlm.p
Time asymmetries in quantum cosmology and the searching for boundary conditions to the Wheeler-DeWitt equation
The paper addresses the quantization of minisuperspace cosmological models by
studying a possible solution to the problem of time and time asymmetries in
quantum cosmology. Since General Relativity does not have a privileged time
variable of the newtonian type, it is necessary, in order to have a dynamical
evolution, to select a physical clock. This choice yields, in the proposed
approach, to the breaking of the so called clock-reversal invariance of the
theory which is clearly distinguished from the well known motion-reversal
invariance of both classical and quantum mechanics. In the light of this new
perspective, the problem of imposing proper boundary conditions on the space of
solutions of the Wheeler-DeWitt equation is reformulated. The symmetry-breaking
formalism of previous papers is analyzed and a clarification of it is proposed
in order to satisfy the requirements of the new interpretation.Comment: 25 pages, 1 figur
Dynamical age differences among coeval star clusters as revealed by blue stragglers
Globular star clusters that formed at the same cosmic time may have evolved
rather differently from a dynamical point of view (because that evolution
depends on the internal environment) through a variety of processes that tend
progressively to segregate stars more massive than the average towards the
cluster centre. Therefore clusters with the same chronological age may have
reached quite different stages of their dynamical history (that is, they may
have different dynamical ages). Blue straggler stars have masses greater than
those at the turn-off point on the main sequence and therefore must be the
result of either a collision or a mass-transfer event. Because they are among
the most massive and luminous objects in old clusters, they can be used as test
particles with which to probe dynamical evolution. Here we report that globular
clusters can be grouped into a few distinct families on the basis of the radial
distribution of blue stragglers. This grouping corresponds well to an effective
ranking of the dynamical stage reached by stellar systems, thereby permitting a
direct measure of the cluster dynamical age purely from observed properties.Comment: Published on the 20 December 2012 issue of Natur
F(T) gravity and k-essence
Modified teleparallel gravity theory with the torsion scalar have recently
gained a lot of attention as a possible explanation of dark energy. We perform
a thorough reconstruction analysis on the so-called models, where
is some general function of the torsion term, and derive conditions for the
equivalence between of models with purely kinetic k-essence. We present
a new class models of -gravity and k-essence. We also proposed some new
models of generalized gases and knot universes as well as some generalizations
of gravity.Comment: 25 page
Efficacy of Work-Related Training for Individuals with Autism Spectrum Disorder
Research suggests that traditional models of work-related training, in addition to a lack of on-the-job support, may exacerbate difficulties experienced by individuals with autism spectrum disorder with obtaining and maintaining employment
The poor employment outcomes experienced by individuals with ASD are well-documented throughout literature and have resulted in the need to examine more effective ways of providing support and work-related interventions.
Although research has investigated the efficacy of work-related training on successful employment outcomes when used with individuals with ASD, a systematic review summarizing this evidence has yet to be published. Therefore, this review examines and interprets current research evidence on the efficacy of work-related training for individuals
Blue Straggler Stars in Globular Clusters: a powerful tool to probe the internal dynamical evolution of stellar systems
This chapter presents an overview of the main observational results obtained
to date about Blue Straggler Stars (BSSs) in Galactic Globular Clusters (GCs).
The BSS specific frequency, radial distribution, chemical composition and
rotational properties are presented and discussed in the framework of using
this stellar population as probe of GC internal dynamics. In particular, the
shape of the BSS radial distribution has been found to be a powerful tracer of
the dynamical age of stellar systems, thus allowing the definition of the first
empirical "dynamical clock".Comment: Chapter 5, in Ecology of Blue Straggler Stars, H.M.J. Boffin, G.
Carraro & G. Beccari (Eds), Astrophysics and Space Science Library, Springe
Young Globular Clusters and Dwarf Spheroidals
Most of the globular clusters in the main body of the Galactic halo were
formed almost simultaneously. However, globular cluster formation in dwarf
spheroidal galaxies appears to have extended over a significant fraction of a
Hubble time. This suggests that the factors which suppressed late-time
formation of globulars in the main body of the Galactic halo were not operative
in dwarf spheroidal galaxies. Possibly the presence of significant numbers of
``young'' globulars at R_{GC} > 15 kpc can be accounted for by the assumption
that many of these objects were formed in Sagittarius-like (but not
Fornax-like) dwarf spheroidal galaxies, that were subsequently destroyed by
Galactic tidal forces. It would be of interest to search for low-luminosity
remnants of parental dwarf spheroidals around the ``young'' globulars Eridanus,
Palomar 1, 3, 14, and Terzan 7. Furthermore multi-color photometry could be
used to search for the remnants of the super-associations, within which outer
halo globular clusters originally formed. Such envelopes are expected to have
been tidally stripped from globulars in the inner halo.Comment: 18 pages, with 2 figures, in LaTeX format; to appear in the
Astrophysical Journal in February 200
Deep HST-WFPC2 photometry of NGC 288. II. The Main Sequence Luminosity Function
The Main Sequence Luminosity Function (LF) of the Galactic globular cluster
NGC 288 has been obtained using deep WFPC2 photometry. We have employed a new
method to correct for completeness and fully account for bin-to-bin migration
due to blending and/or observational scatter. The effect of the presence of
binary systems in the final LF is quantified and is found to be negligible.
There is a strong indication of the mass segregation of unevolved single stars
and clear signs of a depletion of low mass stars in NGC 288 with respect to
other clusters. The results are in good agreement with the prediction of
theoretical models of the dynamical evolution of NGC 288 that take into account
the extreme orbital properties of this cluster.Comment: 16 pages, 6 .ps figures. Low resolution version of fig. 1; full
resolution figure soon available at http://www.bo.astro.it/bap/BAPhome.html
l. Latex. emulateapj5.sty macro included. Accepted for publication by The
Astronomical Journa
Timing of Millisecond Pulsars in NGC 6752: Evidence for a High Mass-to-Light Ratio in the Cluster Core
Using pulse timing observations we have obtained precise parameters,
including positions with about 20 mas accuracy, of five millisecond pulsars in
NGC 6752. Three of them, located relatively close to the cluster center, have
line-of-sight accelerations larger than the maximum value predicted by the
central mass density derived from optical observation, providing dynamical
evidence for a central mass-to-light ratio >~ 10, much higher than for any
other globular cluster. It is likely that the other two millisecond pulsars
have been ejected out of the core to their present locations at 1.4 and 3.3
half-mass radii, respectively, suggesting unusual non-thermal dynamics in the
cluster core.Comment: Accepted by ApJ Letter. 5 pages, 2 figures, 1 tabl
- âŠ