264 research outputs found
Global Spiral Modes in NGC 1566: Observations and Theory
We present an observational and theoretical study of the spiral structure in
galaxy NGC 1566. A digitized image of NGC 1566 in I-band was used for
measurements of the radial dependence of amplitude variations in the spiral
arms. We use the known velocity dispersion in the disk of NGC 1566, together
with its rotation curve, to construct linear and 2D nonlinear simulations which
are then compared with observations. A two-armed spiral is the most unstable
linear global mode in the disk of NGC 1566. The nonlinear simulations are in
agreement with the results of the linear modal analysis, and the theoretical
surface amplitude and the velocity residual variations across the spiral arms
are in qualitative agreement with the observations. The spiral arms found in
the linear and nonlinear simulations are considerably shorter than those
observed in the disk of NGC 1566. We argue therefore, that the surface density
distribution in the disk of the galaxy NGC 1566 was different in the past, when
spiral structure in NGC 1566 was linearly growing.Comment: 41 pages, 20 figures, to be published in the Astrophysical Journa
Influences of Apolipoprotein E and α1-Antichymotrypsin Genotypes on Regional Cerebral Glucose Metabolism in Alzheimer\u27s Disease
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Trapped Surfaces in Vacuum Spacetimes
An earlier construction by the authors of sequences of globally regular,
asymptotically flat initial data for the Einstein vacuum equations containing
trapped surfaces for large values of the parameter is extended, from the time
symmetric case considered previously, to the case of maximal slices. The
resulting theorem shows rigorously that there exists a large class of initial
configurations for non-time symmetric pure gravitational waves satisfying the
assumptions of the Penrose singularity theorem and so must have a singularity
to the future.Comment: 14 page
Skewed parton distributions and the scale dependence of the transverse size parameter
We discuss the scale dependence of a skewed parton distribution of the pion
obtained from a generalized light-cone wave function overlap formula. Using a
simple ansatz for the transverse momentum dependence of the light-cone wave
function and restricting ourselves to the case of a zero skewedness parameter,
the skewed parton distribution can be expressed through an ordinary parton
distribution multiplied by an exponential function. Matching the generalized
and ordinary DGLAP evolution equations of the skewed and ordinary parton
distributions, respectively, we derive a constraint for the scale dependence of
the transverse size parameter, which describes the width of the pion wave
function in transverse momentum space. This constraint has implications for the
Fock state probability and valence distribution. We apply our results to the
pion form factor.Comment: 10 pages, 4 figures; version to appear in Phys. Rev. D; Refs. added,
new discussion of results for pion form factor in view of new dat
On the Mass of Population III Stars
Performing 1D hydrodynamical calculations coupled with non-equilibrium
processes for H2 formation, we pursue the thermal and dynamical evolution of
filamentary primordial clouds and attempt to make an estimate on the mass of
population III stars. It is found that, almost independent of initial
conditions, a filamentary cloud continues to collapse nearly isothermally due
to H_2 cooling until the cloud becomes optically thick against the H_2 lines.
During the collapse the cloud structure separates into two parts, i.e., a
denser spindle and a diffuse envelope. The spindle contracts quasi-statically,
and thus the line mass of the spindle keeps a characteristic value determined
solely by the temperature ( K). Applying a linear theory, we find
that the spindle is unstable against fragmentation during the collapse. The
wavelength of the fastest growing perturbation lessens as the collapse
proceeds. Consequently, successive fragmentation could occur. When the central
density exceeds , the successive fragmentation may
cease since the cloud becomes opaque against the H_2 lines and the collapse
decelerates appreciably. The mass of the first star is then expected to be
typically , which may grow up to by accreting
the diffuse envelope. Thus, the first-generation stars are anticipated to be
massive but not supermassive.Comment: 23 pages, 6 figures, accepted by ApJ (April 10
Polarized Parton Distribution Functions in the Nucleon
Polarized parton distribution functions are determined by using world data
from the longitudinally polarized deep inelastic scattering experiments. A new
parametrization of the parton distribution functions is adopted by taking into
account the positivity and the counting rule. From the fit to the asymmetry
data A_1, the polarized distribution functions of u and d valence quarks, sea
quarks, and gluon are obtained. The results indicate that the quark spin
content is \Delta\Sigma=0.20 and 0.05 in the leading order (LO) and the
next-to-leading-order (NLO) MS-bar scheme, respectively. However, if x
dependence of the sea-quark distribution is fixed at small x by "perturbative
QCD" and Regge theory, it becomes \Delta \Sigma=0.24 ~ 0.28 in the NLO. The
small-x behavior cannot be uniquely determined by the existing data, which
indicates the importance of future experiments. From our analysis, we propose
one set of LO distributions and two sets of NLO ones as the
longitudinally-polarized parton distribution functions.Comment: 51 pages, REVTeX, aps.sty, aps12.sty, epsfig.sty, prabib.sty,
revtex.sty, revtex.cls, 17 eps figures. Submitted for publication. Email:
[email protected]
Spin dependent parton distributions and structure functions
Nuclear parton distributions and structure functions are determined in an
effective chiral quark theory. We also discuss an extension of our model to
fragmentation functions.Comment: To appear in the proceedings of the 20th European Conference on
Few-Body Problems in Physics, Pisa, September 10-14, 200
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