57,204 research outputs found
Magnetic field amplification by cosmic rays in supernova remnants
Magnetic field amplification is needed to accelerate cosmic cays to PeV
energies in supernova remants. Escaping cosmic rays trigger a return current in
the plasma that drives a non-resonant hybrid instability. We run simulations in
which we represent the escaping cosmic rays with the plasma return current,
keeping the maximum cosmic ray energy fixed, and evaluate its effects on the
upstream medium. In addition to magnetic field amplification, density
perturbations arise that, when passing through the shock, further increase
amplification levels downstream. As the growth rate of the instability is most
rapid for the smaller scales, the resolution is a limiting factor in the
amplification that can be reached with these simulations.Comment: 4 pages, 2 figures, to appear in the proceedings of the conference
"370 years of Astronomy in Utrecht", eds. G. Pugliese, A. de Koter and M.
Wijbur
Cosmic ray acceleration in young supernova remnants
We investigate the appearance of magnetic field amplification resulting from
a cosmic ray escape current in the context of supernova remnant shock waves.
The current is inversely proportional to the maximum energy of cosmic rays, and
is a strong function of the shock velocity. Depending on the evolution of the
shock wave, which is drastically different for different circumstellar
environments, the maximum energy of cosmic rays as required to generate enough
current to trigger the non-resonant hybrid instability that confines the cosmic
rays follows a different evolution and reaches different values. We find that
the best candidates to accelerate cosmic rays to ~few PeV energies are young
remnants in a dense environment, such as a red supergiant wind, as may be
applicable to Cassiopeia A. We also find that for a typical background magnetic
field strength of 5 microG the instability is quenched in about 1000 years,
making SN1006 just at the border of candidates for cosmic ray acceleration to
high energies.Comment: 14 pages, 8 figures. Accepted for publication in MNRA
Confining the high-energy cosmic rays
Diffusive shock acceleration is the prime candidate for efficient
acceleration of cosmic rays. Galactic cosmic rays are believed to originate
predominantly from this process in supernova remnant shock waves. Confinement
of the cosmic rays in the shock region is key in making the mechanism
effective. It has been known that on small scales (smaller than the typical
gyroradius) high-amplitude non-resonant instabilities arise due to cosmic ray
streaming ahead of the shock. For the efficiency of scattering of the highest
energy cosmic rays it is of interest to determine the type of instabilities
that act on longer length scales, i.e. larger than the cosmic ray gyroradius.
We will present the results of our analysis of an instability that acts in this
regime and will discuss its driving mechanism and typical growth times.Comment: 4 pages, 1 figure. Proceedings for the conference on Cosmic Rays and
the Interstellar Medium (CRISM) in June 2011, Montpellier, France. To appear
in MSA
From cosmic ray source to the Galactic pool
The Galactic cosmic ray spectrum is a remarkably straight power law. Our
current understanding is that the dominant sources that accelerate cosmic rays
up to the knee ( eV) or perhaps even the ankle ( eV), are young Galactic supernova remnants. In theory, however, there
are various reasons why the spectrum may be different for different sources,
and may not even be a power law if nonlinear shock acceleration applies during
the most efficient stages of acceleration. We show how the spectrum at the
accelerator translates to the spectrum that make up the escaping cosmic rays
that replenish the Galactic pool of cosmic rays. We assume that cosmic ray
confinement, and thus escape, is linked to the level of magnetic field
amplification, and that the magnetic field is amplified by streaming cosmic
rays according to the non-resonant hybrid or resonant instability. When a fixed
fraction of the energy is transferred to cosmic rays, it turns out that a
source spectrum that is flatter than will result in a escape
spectrum, whereas a steeper source spectrum will result in an escape spectrum
with equal steepening. This alleviates some of the concern that may arise from
expected flat or concave cosmic ray spectra associated with nonlinear shock
modification.Comment: 5 pages, 1 figure. Accepted for publication in MNRA
Stoichiometry control of the electronic properties of the LaAlO_3/SrTiO_3 heterointerface
We investigate the effect of the laser parameters of pulsed laser deposition
on the film stoichiometry and electronic properties of LaAlO_3/SrTiO_3 (001)
heterostructures. The La/Al ratio in the LaAlO_3 films was varied over a wide
range from 0.88 to 1.15, and was found to have a strong effect on the interface
conductivity. In particular, the carrier density is modulated over more than
two orders of magnitude. The film lattice expansion, caused by cation
vacancies, is found to be the important functional parameter. These results can
be understood to arise from the variations in the electrostatic boundary
conditions, and their resolution, with stoichiometry.Comment: 4 pages, 3 figures, submitted for publicatio
Surface location of alkaline-earth atom impurities on helium nanodroplets
There has been notable uncertainty regarding the degree of solvation of
alkaline-earth atoms, especially Mg, in free He-4 nanodroplets. We have
measured the electron energy dependence of the ionization yield of picked-up
atoms. There is a qualitative shape difference between the yield curves of
species solvated in the middle of the droplet and species located in the
surface region; this difference arises from the enhanced role played by the
Penning ionization process in the latter case. The measurements demonstrate
that Mg, Ca, Sr and Ba all reside at or near the droplet surface.Comment: 11 pages, 3 figure
Detecting and quantifying the contribution made by aircraft emissions to ambient concentrations of nitrogen oxides in the vicinity of a large international airport
Plans to build a third runway at London Heathrow Airport (LHR) have been held back because of concerns that the development would lead to annual mean concentrations of nitrogen dioxide (NO2) in excess of EU Directives, which must be met by 2010. The dominant effect of other sources of NOX close to the airport, primarily from road traffic, makes it difficult to detect and quantify the contribution made by the airport to local NOX and NO2 concentrations. This work presents approaches that aim to detect and quantify the airport contribution to NOX at a network of seven measurement sites close to the airport. Two principal approaches are used. First, a graphical technique using bivariate polar plots that develops the idea of a pollution rose is used to help discriminate between different source types. The sampling uncertainties associated with the technique have been calculated through a randomised re-sampling approach. Second, the unique pattern of aircraft activity at LHR enables data filtering techniques to be used to statistically verify the presence of aircraft sources. It is shown that aircraft NOX sources can be detected to at least 2.7 km from the airport, despite that the airport contribution is very small at that distance. Using these approaches, estimates have been made of the airport contribution to long-term mean concentrations of NOX and NO2. At the airport boundary we estimate that approximately 28 % (34 Ī¼g m-3) of the annual mean NOX is due to airport operations. At background locations 2-3 km downwind of the airport we estimate that the upper limit of the airport contribution to be less than 15 % (< 10 Ī¼g m-3). This work also provides approaches that would help validate and refine dispersion modelling studies used for airport assessments
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