3,016 research outputs found
Using adiabatic coupling techniques in atom-chip waveguide structures
Adiabatic techniques are well known tools in multi-level electron systems to
transfer population between different states with high fidelity. Recently it
has been realised that these ideas can also be used in ultra-cold atom systems
to achieve coherent manipulation of the atomic centre-of-mass states. Here we
present an investigation into a realistic setup using three atomic waveguides
created on top of an atom chip and show that such systems hold large potential
for the observation of adiabatic phenomena in experiments.Comment: 10 pages, 6 figures, accepted for publication in Physica Scripta for
the CEWQO2009 proceeding
Persistent topographic development along a strike-slip fault system: The Mount McKinley restraining bend
The Denali Fault is a major strike-slip fault extending from British Colombia, into western Alaska. Mount McKinley, at 6,114 m, is the highest peak in North America and is located to the south of a bend in the Denali Fault (Fig.1). To the north, at the apex of the bend in the fault, Peters Dome (3,221 m) is the highest peak and north-side peak elevations rapidly decrease moving away from the bend’s apex
Observed Faraday Effects in Damped Lyman-Alpha Absorbers and Lyman Limit Systems: The Magnetised Environment of Galactic Building Blocks at Redshift=2
Protogalactic environments are typically identified using quasar absorption
lines, and these galactic building blocks can manifest as Damped Lyman-Alpha
Absorbers (DLAs) and Lyman Limit Systems (LLSs). We use radio observations of
Faraday effects to test whether DLAs and LLSs host a magnetised medium, by
combining DLA and LLS detections throughout the literature with 1.4 GHz
polarization data from the NRAO VLA Sky Survey (NVSS). We obtain a control, a
DLA, and a LLS sample consisting of 114, 19, and 27 lines-of-sight respectively
- all of which are polarized at to ensure Rician bias is
negligible. Using a Bayesian framework, we are unable to detect either coherent
or random magnetic fields in DLAs: the regular coherent magnetic fields within
the DLAs must be G, and the lack of depolarization is consistent
with the weakly magnetised gas in DLAs being non-turbulent and quiescent.
However, we find mild suggestive evidence that LLSs have coherent magnetic
fields: after controlling for the redshift-distribution of our data, we find a
71.5% probability that LLSs have a higher RM than a control sample. We also
find strong evidence that LLSs host random magnetic fields, with a 95.5%
probability that LLS lines-of-sight have lower polarized fractions than a
control sample. The regular coherent magnetic fields within the LLSs must be
G, and the magnetised gas must be highly turbulent with a typical
scale on the order of -20 pc, which is similar to that of the Milky
Way. This is consistent with the standard dynamo pedagogy, whereby magnetic
fields in protogalaxies increase in coherence and strength as a function of
cosmic time. Our results are consistent with a hierarchical galaxy formation
scenario, with the DLAs, LLSs, and strong magnesium II (MgII) systems exploring
three different stages of magnetic field evolution in galaxies.Comment: Submitted to Ap
The transport of cosmic rays in self-excited magnetic turbulence
The process of diffusive shock acceleration relies on the efficacy with which
hydromagnetic waves can scatter charged particles in the precursor of a shock.
The growth of self-generated waves is driven by both resonant and non-resonant
processes. We perform high-resolution magnetohydrodynamic simulations of the
non-resonant cosmic-ray driven instability, in which the unstable waves are
excited beyond the linear regime. In a snapshot of the resultant field,
particle transport simulations are carried out. The use of a static snapshot of
the field is reasonable given that the Larmor period for particles is typically
very short relative to the instability growth time. The diffusion rate is found
to be close to, or below, the Bohm limit for a range of energies. This provides
the first explicit demonstration that self-excited turbulence reduces the
diffusion coefficient and has important implications for cosmic ray transport
and acceleration in supernova remnants.Comment: 8 pages, 8 figures, accepted for publication in MNRA
Broadband, radio spectro-polarimetric study of 100 radiative-mode and jet-mode AGN
We present the results from a broadband (1 to 3 GHz), spectro-polarimetry
study of the integrated emission from 100 extragalactic radio sources with the
ATCA, selected to be highly linearly polarized at 1.4 GHz. We use a general
purpose, polarization model-fitting procedure that describes the Faraday
rotation measure (RM) and intrinsic polarization structure of up to three
distinct polarized emission regions or 'RM components' of a source. Overall,
37%/52%/11% of sources are best fit by one/two/three RM components. However,
these fractions are dependent on the signal-to-noise ratio (S/N) in
polarization (more RM components more likely at higher S/N). In general, our
analysis shows that sources with high integrated degrees of polarization at 1.4
GHz have low Faraday depolarization, are typically dominated by a single RM
component, have a steep spectral index, and a high intrinsic degree of
polarization. After classifying our sample into radiative-mode and jet-mode
AGN, we find no significant difference between the Faraday rotation or Faraday
depolarization properties of jet-mode and radiative-mode AGN. However, there is
a statistically significant difference in the intrinsic degree of polarization
between the two types, with the jet-mode sources having more intrinsically
ordered magnetic field structures than the radiative-mode sources. We also find
a preferred perpendicular orientation of the intrinsic magnetic field structure
of jet-mode AGN with respect to the jet direction, while no clear preference is
found for the radiative-mode sources.Comment: 29 pages (including Appendix), 28 figures, 7 tables. Accepted for
publication in MNRA
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