4,996 research outputs found
DIRK Schemes with High Weak Stage Order
Runge-Kutta time-stepping methods in general suffer from order reduction: the
observed order of convergence may be less than the formal order when applied to
certain stiff problems. Order reduction can be avoided by using methods with
high stage order. However, diagonally-implicit Runge-Kutta (DIRK) schemes are
limited to low stage order. In this paper we explore a weak stage order
criterion, which for initial boundary value problems also serves to avoid order
reduction, and which is compatible with a DIRK structure. We provide specific
DIRK schemes of weak stage order up to 3, and demonstrate their performance in
various examples.Comment: 10 pages, 5 figure
Resistance after viral failure on atazanavir-containing therapy: multinational clinical cohort (BMS AI424-128 — 'IMPACT') final analysis
An algebraic Birkhoff decomposition for the continuous renormalization group
This paper aims at presenting the first steps towards a formulation of the
Exact Renormalization Group Equation in the Hopf algebra setting of Connes and
Kreimer. It mostly deals with some algebraic preliminaries allowing to
formulate perturbative renormalization within the theory of differential
equations. The relation between renormalization, formulated as a change of
boundary condition for a differential equation, and an algebraic Birkhoff
decomposition for rooted trees is explicited
Linear and nonlinear susceptibilities of a decoherent two-level system
The linear and nonlinear dynamical susceptibilities of a two level system are
calculated as it undergoes a transition to a decoherent state. Analogously to
the Glover-Tinkham-Ferrell sum rule of superconductivity, spectral weight in
the linear susceptibility is continuously transferred from a finite frequency
resonance to nearly zero frequency, corresponding to a broken symmetry in the
thermodynamic limit. For this reason, the behavior of the present model (the
Mermin model) differs significantly from the spin-boson model. The third order
nonlinear susceptibility, corresponding to two-photon absorption, has an
unexpected non-monotonic behavior as a function of the environmental coupling,
reaching a maximum within the decoherent phase of the model. Both linear and
nonlinear susceptibilities may be expressed in a universal form.Comment: 10 pages, 9 figure
t-3-Pentyl-r-2,c-6-diphenylpiperidin-4-one
In the title molecule, C22H27NO, the piperidine ring adopts a chair conformation, with all substituents equatorial. The dihedral angle between the two phenyl rings is 56.90 (5)°. In the crystal, molecules are linked by weak C—H⋯O hydrogen bonds. A C—H⋯π interaction involving the phenyl ring at the 6-position is also found in the crystal structure
Photometric Properties of Galaxy Population in the Cluster EIS 0048-2942 at z~0.64
~Deep photometric data in the V-, R-, I-, z- and K-bands for the cluster of
galaxies EIS 0048-2942 are used to investigate the properties of the galaxy
populations at z~0.64 in a field of 2.5x2.5 Mpc^2. The sample of candidate
cluster members (N = 171) is selected by the photometric redshift technique and
is complete up to I=22.5. Galaxies were classified as spheroids and disks
according to the shape of the light profile in the I-band, as parametrized by
the Sersic index. In both optical and NIR, spheroids define a sharp
colour-magnitude sequence, whose slope and zero points are consistent with a
high formation redshift (z_f > 2). The disk population occupies a different
region in the colour-magnitude diagram, having bluer colours with respect to
the red sequence. Interestingly, we find some level of mixing between the
properties of the two classes: some disks lie on the colour-magnitude sequence
or are redder, while some spheroids turn out to be bluer. The spatial
distribution of cluster galaxies show a clumpy structure, with a main
over-density of radius ~0.5 Mpc, and at least two other clumps distant ~1 Mpc
from the center. The various sub-structures are mostly populated by the red
galaxies, while the blue population has an almost uniform distribution. The
fraction of blue galaxies in EIS 0048-2942 is f_B=0.11 +/-0.07. This is much
lower than what expected on the basis of the Butcher-Oemler effect at lower
redshifts.Comment: 22 pages, 12 figures. A&A in pres
Backward error analysis and the substitution law for Lie group integrators
Butcher series are combinatorial devices used in the study of numerical
methods for differential equations evolving on vector spaces. More precisely,
they are formal series developments of differential operators indexed over
rooted trees, and can be used to represent a large class of numerical methods.
The theory of backward error analysis for differential equations has a
particularly nice description when applied to methods represented by Butcher
series. For the study of differential equations evolving on more general
manifolds, a generalization of Butcher series has been introduced, called
Lie--Butcher series. This paper presents the theory of backward error analysis
for methods based on Lie--Butcher series.Comment: Minor corrections and additions. Final versio
Evolution since z = 0.5 of the Morphology-Density relation for Clusters of Galaxies
Using traditional morphological classifications of galaxies in 10
intermediate-redshift (z~0.5) clusters observed with WFPC-2 on the Hubble Space
Telescope, we derive relations between morphology and local galaxy density
similar to that found by Dressler for low-redshift clusters. Taken
collectively, the `morphology-density' relationship, M-D, for these more
distant, presumably younger clusters is qualitatively similar to that found for
the local sample, but a detailed comparison shows two substantial differences:
(1) For the clusters in our sample, the M-D relation is strong in centrally
concentrated ``regular'' clusters, those with a strong correlation of radius
and surface density, but nearly absent for clusters that are less concentrated
and irregular, in contrast to the situation for low redshift clusters where a
strong relation has been found for both. (2) In every cluster the fraction of
elliptical galaxies is as large or larger than in low-redshift clusters, but
the S0 fraction is 2-3 times smaller, with a proportional increase of the
spiral fraction. Straightforward, though probably not unique, interpretations
of these observations are (1) morphological segregation proceeds
hierarchically, affecting richer, denser groups of galaxies earlier, and (2)
the formation of elliptical galaxies predates the formation of rich clusters,
and occurs instead in the loose-group phase or even earlier, but S0's are
generated in large numbers only after cluster virialization.Comment: 35 pages, 19 figures, uses psfig. Accepted for publication in Ap
Is the Butcher-Oemler effect a function of the cluster redshift ?
Using PSPC {\it Rosat} data, we measure x-ray surface brightness profiles,
size and luminosity of the Butcher-Oemler (BO) sample of clusters of galaxies.
The cluster x-ray size, as measured by the Petrosian r_{\eta=2} radius, does
not change with redshift and is independent from x-ray luminosity. On the other
hand, the x-ray luminosity increases with redshift. Considering that fair
samples show no-evolution, or negative luminosity evolution, we conclude that
the BO sample is not formed from the same class of objects observed at
different look-back times. This is in conflict with the usual interpretation of
the Butcher-Oemler as an evolutionary (or redshift-dependent) effect, based on
the assumption that we are comparing the same class of objects at different
redshifts. Other trends present in the BO sample reflect selection criteria
rather than differences in look-back time, as independently confirmed by the
fact that trends loose strength when we enlarge the sample with x-ray selected
sample of clusters. The variety of optical sizes and shapes of the clusters in
the Butcher-Oemler sample, and the Malmquist-like bias, are the reasons for
these selection effects that mimic the trends usually interpreted as changes
due to evolution.Comment: ApJ, in press, scheduled on May, 10 issue. 17 pages & 11 figure
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