24,352 research outputs found
Counterexample to an additivity conjecture for output purity of quantum channels
A conjecture arising naturally in the investigation of additivity of
classical information capacity of quantum channels states that the maximal
purity of outputs from a quantum channel, as measured by the p-norm, should be
multiplicative with respect to the tensor product of channels. We disprove this
conjecture for p>4.79. The same example (with p=infinity) also disproves a
conjecture for the multiplicativity of the injective norm of Hilbert space
tensor products.Comment: 3 pages, 3 figures, revte
Numerical studies of planar closed random walks
Lattice numerical simulations for planar closed random walks and their
winding sectors are presented. The frontiers of the random walks and of their
winding sectors have a Hausdorff dimension . However, when properly
defined by taking into account the inner 0-winding sectors, the frontiers of
the random walks have a Hausdorff dimension .Comment: 15 pages, 15 figure
Weak magnetic fields in white dwarfs and their direct progenitors?
We have carried out a re-analysis of polarimetric data of central stars of
planetary nebulae, hot subdwarfs, and white dwarfs taken with FORS1 (FOcal
Reducer and low dispersion Spectrograph) on the VLT (Very Large Telescope), and
added a large number of new observations in order to increase the sample. A
careful analysis of the observations using only one wavelength calibration for
the polarimetrically analysed spectra and for all positions of the retarder
plate of the spectrograph is crucial in order to avoid spurious signals. We
find that the previous detections of magnetic fields in subdwarfs and central
stars could not be confirmed while about 10% of the observed white dwarfs have
magnetic fields at the kilogauss level.Comment: 6 pages, Proceedings of the 18th European White Dwarf Workshop, ASP
Conference Serie
A non-pulsating neutron star in the supernova remnant HESS J1731-347 / G353.6-0.7 with a carbon atmosphere
Context: The CCO candidate in the center of the supernova remnant shell HESS
J1731-347 / G353.6-0.7 shows no pulsations and exhibits a blackbody-like X-ray
spectrum. If the absence of pulsations is interpreted as evidence for the
emitting surface area being the entire neutron star surface, the assumption of
the measured flux being due to a blackbody emission translates into a source
distance that is inconsistent with current estimates of the remnant's distance.
Aims: With the best available observational data, we extended the pulse period
search down to a sub-millisecond time scale and used a carbon atmosphere model
to describe the X-ray spectrum of the CCO and to estimate geometrical
parameters of the neutron star. Methods: To search for pulsations we used data
of an observation of the source with XMM-Newton performed in timing mode. For
the spectral analysis, we used earlier XMM-Newton observations performed in
imaging mode, which permits a more accurate treatment of the background. The
carbon atmosphere models used to fit the CCO spectrum are computed assuming
hydrostatic and radiative equilibria and take into account pressure ionization
and the presence of spectral lines. Results: Our timing analysis did not reveal
any pulsations with a pulsed fraction above ~8% down to 0.2 ms. This finding
further supports the hypothesis that the emitting surface area is the entire
neutron star surface. The carbon atmosphere model provides a good fit to the
CCO spectrum and leads to a normalization consistent with the available
distance estimates of the remnant. The derived constraints on the mass and
radius of the source are consistent with reasonable values of the neutron star
mass and radius. After the CCO in Cas A, the CCO in HESS J1731-347 / G353.6-0.7
is the second object of this class for which a carbon atmosphere model provides
a consistent description of X-ray emission.Comment: 6 pages, 5 figures, accepted for publication in
Astronomy&Astrophysic
Analysis of enhanced tan(beta) corrections in MFV GUT scenarios
We analyse a minimal supersymmetric standard model (MSSM) taking a minimal
flavour violation (MFV) structure at the GUT scale. We evaluate the parameters
at the electroweak scale taking into account the full flavour structure in the
evolution of the renormalization group equations. We concentrate mainly on the
decay Bs -> mu mu and its correlations with other observables like b -> s
gamma, b -> s l l, Delta M_Bs and the anomalous magnetic moment of the muon. We
restrict our analysis to the regions in parameter space consistent with the
dark matter constraints. We find that the BR(Bs -> mu mu) can exceed the
current experimental limit in the regions of parameter space which are allowed
by all other constraints thus providing an additional bound on supersymmetric
parameters. This holds even in the constrained MSSM. Assuming an hypothetical
measurement of BR(Bs -> mu mu) ~ 10^-7 we analyse the predicted MSSM spectrum
and flavour violating decay modes of supersymmetric particles which are found
to be small.Comment: 47 pages, 16 figures (best viewed printed or in pdf format), updated
lattice inputs used, version submitted to PR
A future very-high-energy view of our Galaxy
The survey of the inner Galaxy with H.E.S.S. was remarkably successful in
detecting a wide range of new very-high-energy gamma-ray sources. New TeV
gamma-ray emitting source classes were established, although several of the
sources remain unidentified, and progress has been made in understanding
particle acceleration in astrophysical sources. In this work, we constructed a
model of a population of such very-high-energy gamma-ray emitters and
normalised the flux and size distribution of this population model to the
H.E.S.S.-discovered sources. Extrapolating that population of objects to lower
flux levels we investigate what a future array of imaging atmospheric
telescopes (IACTs) such as AGIS or CTA might detect in a survey of the Inner
Galaxy with an order of magnitude improvement in sensitivity. The sheer number
of sources detected together with the improved resolving power will likely
result in a huge improvement in our understanding of the populations of
galactic gamma-ray sources. A deep survey of the inner Milky Way would also
support studies of the interstellar diffuse gamma-ray emission in regions of
high cosmic-ray density. In the final section of this paper we investigate the
science potential for the Galactic Centre region for studying energy-dependent
diffusion with such a future array.Comment: Proceeding of "Heidelberg International Symposium on High Energy
Gamma-Ray Astronomy", held in Heidelberg, 7-11 July 2008, submitted to AIP
Conference Proceedings. 4 pages, 4 figure
On the origin of white dwarfs with carbon-dominated atmospheres: the case of H1504+65
We explore different evolutionary scenarios to explain the helium deficiency
observed in H1504+65, the most massive known PG1159 star. We concentrate mainly
on the possibility that this star could be the result of mass loss shortly
after the born-again and during the subsequent evolution through the [WCL]
stage. This possibility is sustained by recent observational evidence of
extensive mass-loss events in Sakurai's object and is in line with the recent
finding that such mass losses give rise to PG1159 models with thin helium-rich
envelopes and large rates of period change, as demanded by the pulsating star
PG1159-035. We compute the post born again evolution of massive sequences by
taking into account different mass-loss rate histories. Our results show that
stationary winds during the post-born-again evolution fail to remove completely
the helium-rich envelope so as to explain the helium deficiency observed in
H1504+65. Stationary winds during the Sakurai and [WCL] stages only remove at
most half of the envelope surviving the violent hydrogen burning during the
born-again phase. In view of our results, the recently suggested evolutionary
connection born-again stars --> H1504+65 --> white dwarfs with carbon-rich
atmospheres is difficult to sustain unless the whole helium-rich envelope could
be ejected by non-stationary mass-loss episodes during the Sakurai stage.Comment: 5 pages, 2 figures. To be published in Astronomy & Astrophysic
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