1,922 research outputs found
Evaluating kernels on Xeon Phi to accelerate Gysela application
This work describes the challenges presented by porting parts ofthe Gysela
code to the Intel Xeon Phi coprocessor, as well as techniques used for
optimization, vectorization and tuning that can be applied to other
applications. We evaluate the performance of somegeneric micro-benchmark on Phi
versus Intel Sandy Bridge. Several interpolation kernels useful for the Gysela
application are analyzed and the performance are shown. Some memory-bound and
compute-bound kernels are accelerated by a factor 2 on the Phi device compared
to Sandy architecture. Nevertheless, it is hard, if not impossible, to reach a
large fraction of the peek performance on the Phi device,especially for
real-life applications as Gysela. A collateral benefit of this optimization and
tuning work is that the execution time of Gysela (using 4D advections) has
decreased on a standard architecture such as Intel Sandy Bridge.Comment: submitted to ESAIM proceedings for CEMRACS 2014 summer school version
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Asteroseismic Theory of Rapidly Oscillating Ap Stars
This paper reviews some of the important advances made over the last decade
concerning theory of roAp stars.Comment: 9 pages, 5 figure
Adaptive Covariance Estimation with model selection
We provide in this paper a fully adaptive penalized procedure to select a
covariance among a collection of models observing i.i.d replications of the
process at fixed observation points. For this we generalize previous results of
Bigot and al. and propose to use a data driven penalty to obtain an oracle
inequality for the estimator. We prove that this method is an extension to the
matricial regression model of the work by Baraud
Ultrafast Magneto-Acoustics in Nickel Films
We report about the existence of magneto-acoustic pulses propagating in a
200-nm-thick ferromagnetic nickel film excited with 120 fs laser pulses. They
result from the coupling between the magnetization of the ferromagnetic film
and the longitudinal acoustic waves associated to the propagation of the
lattice deformation induced by the femtosecond laser pulses. The
magneto-acoustic pulses are detected from both the front and back sides of the
film, using the time-resolved magneto-optical Kerr technique, measuring both
the time dependent rotation and ellipticity. We show that the propagating
acoustic pulse couples efficiently to the magnetization and is strong enough to
induce a precession of the magnetization. It is due to a transient change of
the crystalline anisotropy associated to the lattice deformation. It is shown
that the results can be interpreted by combining the concepts of acoustic pulse
propagation and ultrafast magnetization dynamics.Comment: 4 pages, 3 figures, Submitted to Physical Review Letters on November
30th 201
On the understanding of pulsations in the atmosphere of roAp stars: phase diversity and false nodes
Studies based on high-resolution spectroscopic data of rapidly oscillating Ap
stars show a surprising diversity of pulsation behavior in the atmospheric
layers, pointing, in particular, to the co-existence of running and standing
waves. The correct interpretation of these data requires a careful modelling of
pulsations in these magnetic stars. In light of this, in this work we present a
theoretical analysis of pulsations in roAp stars, taking into account the
direct influence of the magnetic field. We derive approximate analytical
solutions for the displacement components parallel and perpendicular to the
direction of the magnetic field, that are appropriate to the outermost layer.
From these, we determine the expression for the theoretical radial velocity for
an observer at a general position, and compute the corresponding pulsation
amplitude and phase as function of height in the atmosphere. We show that the
integral for the radial velocity has contributions from three different types
of wave solutions, namely, running waves, evanescent waves, and standing waves
of nearly constant amplitude. We then consider a number of case studies to
illustrate the origin of the different pulsational behaviour that is found in
the observations. Concerning pulsation amplitude, we find that it generally
increases with atmospheric height. Pulsation phase, however, shows a diversity
of behaviours, including phases that are constant, increasing, or decreasing
with atmospheric height. Finally, we show that there are situations in which
the pulsation amplitude goes through a zero, accompanied by a phase jumps of
, and argue that such behaviour does not correspond to a pulsation node in
the outermost layers of the star, but rather to a visual effect, resulting from
the observers inability to resolve the stellar surface.Comment: 21 pages, 25 figure
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