2,437 research outputs found
Helicity, polarization, and Riemann-Silberstein vortices
Riemann-Silberstein (RS) vortices have been defined as surfaces in spacetime
where the complex form of a free electromagnetic field given by F=E+iB is null
(F.F=0), and they can indeed be interpreted as the collective history swept out
by moving vortex lines of the field. Formally, the nullity condition is similar
to the definition of "C-lines" associated with a monochromatic electric or
magnetic field, which are curves in space where the polarization ellipses
degenerate to circles. However, it was noted that RS vortices of monochromatic
fields generally oscillate at optical frequencies and are therefore
unobservable while electric and magnetic C-lines are steady. Here I show that
under the additional assumption of having definite helicity, RS vortices are
not only steady but they coincide with both sets of C-lines, electric and
magnetic. The two concepts therefore become one for waves of definite frequency
and helicity. Since the definition of RS vortices is relativistically invariant
while that of C-lines is not, it may be useful to regard the vortices as a
wideband generalization of C-lines for waves of definite helicity.Comment: 5 pages, no figures. Submitted to J of Optics A, special issue on
Singular Optics; minor changes from v.
Simultaneous BeppoSAX and Rossi X-ray Timing Explorer observations of 4U1812-12
4U1812-12 is a faint persistent and weakly variable neutron star X-ray
binary. It was observed by BeppoSAX between April 20th and 21st, 2000 in a hard
spectral state with a bolometric luminosity of ~2x10^36 ergs/s. Its broad band
energy spectrum is characterized by the presence of a hard X-ray tail extending
above ~100 keV. It can be represented as the sum of a dominant hard Comptonized
component (electron temperature of ~36 keV and optical depth ~3) and a weak
soft component. The latter component which can be fitted with a blackbody of
about 0.6 keV and equivalent radius of ~2 km is likely to originate from the
neutron star surface. We also report on the first measurement of the power
density spectrum of the source rapid X-ray variability, as recorded during a
simultaneous snapshot observation performed by the Rossi X-ray Timing Explorer.
As expected for a neutron star system in such hard spectral state, its power
density spectrum is characterized by the presence of a ~0.7 Hz low frequency
quasi-periodic oscillation together with three broad noise components, one of
which extends above ~200 Hz.Comment: 6 pages, 3 figures, accepted for publication in A&
Interpreting the High Frequency QPO Power Spectra of Accreting Black Holes
In the context of a relativistic hot spot model, we investigate different
physical mechanisms to explain the behavior of quasi-periodic oscillations
(QPOs) from accreting black holes. The locations and amplitudes of the QPO
peaks are determined by the ray-tracing calculations presented in Schnittman &
Bertschinger (2004a): the black hole mass and angular momentum give the
geodesic coordinate frequencies, while the disk inclination and the hot spot
size, shape, and overbrightness give the amplitudes of the different peaks. In
this paper additional features are added to the existing model to explain the
broadening of the QPO peaks as well as the damping of higher frequency
harmonics in the power spectrum. We present a number of analytic results that
closely agree with more detailed numerical calculations. Four primary pieces
are developed: the addition of multiple hot spots with random phases, a finite
width in the distribution of geodesic orbits, Poisson sampling of the detected
photons, and the scattering of photons from the hot spot through a corona of
hot electrons around the black hole. Finally, the complete model is used to fit
the observed power spectra of both type A and type B QPOs seen in XTE
J1550-564, giving confidence limits on each of the model parameters.Comment: 30 pages, 5 figures, submitted to Ap
The E-peak distribution of the GRBs detected by HETE FREGATE instrument
The FREGATE gamma ray detector of HETE-2 is sensitive to photons between 6
and 400 keV. This sensitivity range, extended towards low energies, allows us
to explore the emission of GRBs in hard X-rays. We fit the spectra of 23 GRBs
with Band's spectral function in order to derive the distribution of their peak
energies (E-peak). This distribution is then compared with the E-peak
distributions measured by BATSE and GINGA.Comment: 3 pages, Woods Hole Proceeding
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