1,346 research outputs found
Smearing of the 2D Kohn anomaly in a nonquantizing magnetic field: Implications for the interaction effects
Thermodynamic and transport characteristics of a clean two-dimensional
interacting electron gas are shown to be sensitive to the weak perpendicular
magnetic field even at temperatures much higher than the cyclotron energy, when
the quantum oscillations are completely washed out. We demonstrate this
sensitivity for two interaction-related characteristics: electron lifetime and
the tunnel density of states. The origin of the sensitivity is traced to the
field-induced smearing of the Kohn anomaly; this smearing is the result of
curving of the semiclassical electron trajectories in magnetic field.Comment: 4.5 pages, 3 figures, published versio
Blurred maximal cyclically monotone sets and bipotentials
Let X be a reflexive Banach space and Y its dual. In this paper we find
necessary and sufficient conditions for the existence of a bipotential for a
blurred maximal cyclically monotone graph. Equivalently, we find a necessary
and sufficient condition on for that the differential
inclusion can be put in the form
, with a bipotential.Comment: Revised version, corrections in theorem 6.
Magnetic Helicity Generation from the Cosmic Axion Field
The coupling between a primordial magnetic field and the cosmic axion field
generates a helical component of the magnetic field around the time in which
the axion starts to oscillate. If the energy density of the seed magnetic field
is comparable to the energy density of the universe at that time, then the
resulting magnetic helicity is about |H_B| \simeq (10^{-20} G)^2 kpc and
remains constant after its generation. As a corollary, we find that the
standard properties of the oscillating axion remain unchanged even in the
presence of very strong magnetic fields.Comment: 6 pages, 2 figures. Accepted for publication in Phys. Rev. D. Minor
revisions and new references adde
Temperature dependence of polarization relaxation in semiconductor quantum dots
The decay time of the linear polarization degree of the luminescence in
strongly confined semiconductor quantum dots with asymmetrical shape is
calculated in the frame of second-order quasielastic interaction between
quantum dot charge carriers and LO phonons. The phonon bottleneck does not
prevent significantly the relaxation processes and the calculated decay times
can be of the order of a few tens picoseconds at temperature K,
consistent with recent experiments by Paillard et al. [Phys. Rev. Lett.
{\bf86}, 1634 (2001)].Comment: 4 pages, 4 figure
Exciton-LO-phonon dynamics in InAs/GaAs quantum dots: Effects of zone-edge phonon damping
The dynamics of an exciton-LO-phonon system after an ultrafast optical
excitation in an InAs/GaAs quantum dot is studied theoretically. Influence of
anharmonic phonon damping and its interplay with the phonon dispersion is
analyzed. The signatures of the zone-edge decay process in the absorption
spectrum and time evolution are highlighted, providing a possible way of
experimental investigation on phonon anharmonicity effects.Comment: 10 pages, 2 figure
One-Dimensional Directed Sandpile Models and the Area under a Brownian Curve
We derive the steady state properties of a general directed ``sandpile''
model in one dimension. Using a central limit theorem for dependent random
variables we find the precise conditions for the model to belong to the
universality class of the Totally Asymmetric Oslo model, thereby identifying a
large universality class of directed sandpiles. We map the avalanche size to
the area under a Brownian curve with an absorbing boundary at the origin,
motivating us to solve this Brownian curve problem. Thus, we are able to
determine the moment generating function for the avalanche-size probability in
this universality class, explicitly calculating amplitudes of the leading order
terms.Comment: 24 pages, 5 figure
Cascading on extragalactic background light
High-energy gamma-rays propagating in the intergalactic medium can interact
with background infrared photons to produce e+e- pairs, resulting in the
absorption of the intrinsic gamma-ray spectrum. TeV observations of the distant
blazar 1ES 1101-232 were thus recently used to put an upper limit on the
infrared extragalactic background light density. The created pairs can
upscatter background photons to high energies, which in turn may pair produce,
thereby initiating a cascade. The pairs diffuse on the extragalactic magnetic
field (EMF) and cascade emission has been suggested as a means for measuring
its intensity. Limits on the IR background and EMF are reconsidered taking into
account cascade emissions. The cascade equations are solved numerically.
Assuming a power-law intrinsic spectrum, the observed 100 MeV - 100 TeV
spectrum is found as a function of the intrinsic spectral index and the
intensity of the EMF. Cascades emit mainly at or below 100 GeV. The observed
TeV spectrum appears softer than for pure absorption when cascade emission is
taken into account. The upper limit on the IR photon background is found to be
robust. Inversely, the intrinsic spectra needed to fit the TeV data are
uncomfortably hard when cascade emission makes a significant contribution to
the observed spectrum. An EMF intensity around 1e-8 nG leads to a
characteristic spectral hump in the GLAST band. Higher EMF intensities divert
the pairs away from the line-of-sight and the cascade contribution to the
spectrum becomes negligible.Comment: 5 pages, to be published as a research note in A&
Pulsar rotation measures and the magnetic structure of our Galaxy
We have obtained 63 rotation measures (RMs) from polarization observations of
southern pulsars, of which 54 are new measurements and 3 are varied from
previous values. The new pulsar RM data at high Galactic latitudes are mostly
consistent with the antisymmetric RM distribution found previously. For the
Galactic disc, evidence for a field reversal near the Perseus arm, and possibly
another beyond it, is presented. Inside the Solar Circle, in addition to the
two known field reversals in or near the Carina-Sagittartus arm and the
Crux-Scutum arm, a further reversal in the Norma arm is tentatively identified.
These reversals, together with the pitch angle derived from pulsar RM and
stellar polarization distributions, are consistent with bisymmetric spiral
(BSS) models for the large-scale magnetic field structure in the disc of our
Galaxy. However, discrimination between models is complicated by the presence
of smaller-scale irregularities in the magnetic field, as well as uncertainties
in the theoretical modelling.Comment: 10pages; 8 figures; Accepted by MNRA
Galaxy rotation curves: the effect of j x B force
Using the Galaxy as an example, we study the effect of j x B force on the
rotational curves of gas and plasma in galaxies. Acceptable model for the
galactic magnetic field and plausible physical parameters are used to fit the
flat rotational curve for gas and plasma based on the observed baryonic
(visible) matter distribution and j x B force term in the static MHD equation
of motion. We also study the effects of varied strength of the magnetic field,
its pitch angle and length scale on the rotational curves. We show that j x B
force does not play an important role on the plasma dynamics in the
intermediate range of distances 6-12 kpc from the centre, whilst the effect is
sizable for larger r (r > 15 kpc), where it is the most crucial.Comment: Accepted for publication in Astrophysics & Space Science (final
printed version, typos in proofs corrected
Point-like gamma ray sources as signatures of distant accelerators of ultra high energy cosmic rays
We discuss the possibility of observing distant accelerators of ultra high
energy cosmic rays in synchrotron gamma rays. Protons propagating away from
their acceleration sites produce extremely energetic electrons during
photo-pion interactions with cosmic microwave background photons. If the
accelerator is embedded in a magnetized region, these electrons will emit high
energy synchrotron radiation. The resulting synchrotron source is expected to
be point-like and detectable in the GeV-TeV energy range if the magnetic field
is at the nanoGauss level.Comment: 4 pages 2 figures. To be published in PR
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