2,861 research outputs found
MuMax: a new high-performance micromagnetic simulation tool
We present MuMax, a general-purpose micromagnetic simulation tool running on
Graphical Processing Units (GPUs). MuMax is designed for high performance
computations and specifically targets large simulations. In that case speedups
of over a factor 100x can easily be obtained compared to the CPU-based OOMMF
program developed at NIST. MuMax aims to be general and broadly applicable. It
solves the classical Landau-Lifshitz equation taking into account the
magnetostatic, exchange and anisotropy interactions, thermal effects and
spin-transfer torque. Periodic boundary conditions can optionally be imposed. A
spatial discretization using finite differences in 2 or 3 dimensions can be
employed. MuMax is publicly available as open source software. It can thus be
freely used and extended by community. Due to its high computational
performance, MuMax should open up the possibility of running extensive
simulations that would be nearly inaccessible with typical CPU-based
simulators.Comment: To be published in JMM
Detecting Star Formation in Brightest Cluster Galaxies with GALEX
We present the results of GALEX observations of 17 cool core (CC) clusters of
galaxies. We show that GALEX is easily capable of detecting star formation in
brightest cluster galaxies (BCGs) out to and 50-100 kpc. In most of
the CC clusters studied, we find significant UV luminosity excesses and colors
that strongly suggest recent and/or current star formation. The BCGs are found
to have blue UV colors in the center that become increasingly redder with
radius, indicating that the UV signature of star formation is most easily
detected in the central regions. Our findings show good agreement between UV
star formation rates and estimates based on H observations. IR
observations coupled with our data indicate moderate-to-high dust attenuation.
Comparisons between our UV results and the X-ray properties of our sample
suggest clear correlations between UV excess, cluster entropy, and central
cooling time, confirming that the star formation is directly and
incontrovertibly related to the cooling gas.Comment: 39 pages, 11 figures; accepted for publication in The Astrophysical
Journal. Figure quality reduced to comply with arXiv file size requirement
Magneto-resistance in a lithography defined single constrained domain wall spin valve
We have measured domain wall magnetoresistance in a single lithographically constrained domain wall. An H-shaped Ni nano-bridge was fabricated by e-beam lithography with the two sides being single magnetic do- mains showing independent magnetic switching. The connection between the sides constraining the domain wall when the sides line up anti-parallel. The magneto-resistance curve clearly identifies the magnetic con- figurations that are expected from a spin valve-like structure. The value of the magneto-resistance at room temperature is around 0.1% or 0.4 Â. This value is shown to be in agreement with a theoretical formulation based on spin accumulation. Micromagnetic simulations show it is possible to reduce the size of the domain wall further by shortening the length of the bridge
Venus methane and water
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/94590/1/grl6638.pd
Pahs, Ionized Gas, and Molecular Hydrogen in Brightest Cluster Galaxies of Cool Core Clusters of Galaxies
We present measurements of 5-25 {\mu}m emission features of brightest cluster
galaxies (BCGs) with strong optical emission lines in a sample of 9 cool-core
clusters of galaxies observed with the Infrared Spectrograph on board the
Spitzer Space Telescope. These systems provide a view of dusty molecular gas
and star formation, surrounded by dense, X-ray emitting intracluster gas. Past
work has shown that BCGs in cool-core clusters may host powerful radio sources,
luminous optical emission line systems, and excess UV, while BCGs in other
clusters never show this activity. In this sample, we detect polycyclic
aromatic hydrocarbons (PAHs), extremely luminous, rotationally-excited
molecular hydrogen line emission, forbidden line emission from ionized gas ([Ne
II] and [Ne III]), and infrared continuum emission from warm dust and cool
stars. We show here that these BCGs exhibit more luminous forbidden neon and H2
rotational line emission than star-forming galaxies with similar total infrared
luminosities, as well as somewhat higher ratios of 70 {\mu}m / 24 {\mu}m
luminosities. Our analysis suggests that while star formation processes
dominate the heating of the dust and PAHs, a heating process consistent with
suprathermal electron heating from the hot gas, distinct from star formation,
is heating the molecular gas and contributing to the heating of the ionized gas
in the galaxies. The survival of PAHs and dust suggests that dusty gas is
somehow shielded from significant interaction with the X-ray gas.Comment: 27 preprint pages, 18 figures, accepted by Astrophysical Journa
Field-induced domain wall propagation velocity in magnetic nanowires
A thory of field-induced domain wall (DW) propagation is developed. The
theory not only explains why a DW in a defect-free nanowire must propagate at a
finite velocity, but also provides a proper definition of DW propagation
velocity. This definition, valid for an arbitrary DW structure, allows one to
compute the instantaneous DW velocity in a meaningful way even when the DW is
not moving as a rigid body. A new velocity-field formula beyond the Walker
breakdown field, which is in excellent agreement with both experiments and
numerical simulations, is derived
Optical IFU Observations of the Brightest Cluster Galaxy NGC 4696: The Case for a Minor Merger and Shock-excited Filaments
We present deep optical integral-field spectroscopic observations of the
nearby (z ~ 0.01) brightest cluster galaxy NGC 4696 in the core of the
Centaurus Cluster, made with the Wide Field Spectrograph (WiFeS) on the ANU
2.3m telescope at Siding Spring Observatory. We investigate the morphology,
kinematics, and excitation of the emission-line filaments and discuss these in
the context of a model of a minor merger. We suggest that the emission-line
filaments in this object have their origin in the accretion of a gas-rich
galaxy and that they are excited by v ~100-200 km/s shocks driven into the cool
filament gas by the ram pressure of the transonic passage of the merging system
through the hot halo gas of NGC 4696.Comment: 19 pages, 15 figures, accepted for publication in The Astrophysical
Journa
NoSOCS in SDSS. I. Sample Definition and Comparison of Mass Estimates
We use Sloan Digital Sky Survey (SDSS) data to investigate galaxy cluster
properties of systems first detected within DPOSS. With the high quality
photometry of SDSS we derived new photometric redshifts and estimated richness
and optical luminosity. For a subset of low redshift () clusters, we
have used SDSS spectroscopic data to identify groups in redshift space in the
region of each cluster, complemented with massive systems from the literature
to assure the continuous mass sampling. A method to remove interlopers is
applied, and a virial analysis is performed resulting in estimates of velocity
dispersion, mass, and a physical radius for each low- system. We discuss the
choice of maximum radius and luminosity range in the dynamical analysis,
showing that a spectroscopic survey must be complete to at least M if one
wishes to obtain accurate and unbiased estimates of velocity dispersion and
mass. We have measured X-ray luminosity for all clusters using archival data
from RASS. For a smaller subset (twenty-one clusters) we selected temperature
measures from the literature and estimated mass from the M-T relation,
finding that they show good agreement with the virial estimate. However, these
two mass estimates tend to disagree with the caustic results. We measured the
presence of substructure in all clusters of the sample and found that clusters
with substructure have virial masses higher than those derived from T. This
trend is not seen when comparing the caustic and X-ray masses. That happens
because the caustic mass is estimated directly from the mass profile, so it is
less affected by substructure.Comment: 21 pages, 17 figures, 5 tables, Accepted to MNRA
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