The linear polarization position angle (PPA) of pulsar emission shows a wide variety of structures, which deviates from the classical rotating vector model. In this study we investigate the effect on the PPA due to emission arising from a range of heights. We demonstrate that by appropriately choosing the emission height we can reconstruct the PPA sweep across the integrated pulse profiles.

The recent discovery of a very high degree of linear polarization in the prompt emission of GRB 021206 (Coburn & Boggs 2003) has suggested that synchrotron emission may play a dominant role in the production of the prompt γ-ray photons. We here show that, under certain geometrical conditions, an even higher level of linear polarization is expected if the photons are produced by bulk inverse Com...

Using recent measurements of ultraviolet interstellar polarization, we have examined its relationship to ultraviolet extinction and to polarization and extinction measurements in the visible and infrared. The relationship between the relative amount of ultraviolet polarization and the parameter determined j max , using only visible data, is conÐrmed and strengthened, for example, by a tight cor...

We have observed the optical pulse profile of PSR B0656+14 in 10 phase bins at a high signal-to-noise ratio, and have measured the linear polarization profile over 30% of the pulsar period with some significance. The pulse profile is double-peaked, with a bridge of emission between the two peaks, similar to gamma-ray profiles observed in other pulsars. There is no detectable unpulsed flux, to a...

collinear configuration, in which the laser wave is linearly polarized with electric field E parallel to the initial electron momentum p 0, is the optimal configuration for the relativistic reversal. In that case, the transverse PF reverses its direction when the incident momentum is p0=mc. The reversal effect vanishes in the cases of circular and linear with E p 0 polarizations. We have discov...

We calculate the wavelength dependence of the ratio of the linear polarization degree to extinction (polarizing efficiency) P(λ)/A(λ) from the ultraviolet to near-infrared. The prolate and oblate particles with aspect ratios from a/b = 1.1 up to 10 are assumed to be rotating and partially aligned with the mechanism of paramagnetic relaxation (Davis– Greenstein). Size/shape/orientation effects a...

The optical lightcurve of GRB 010222 exhibited one of the slowest decays of any gamma-ray burst to date. Its broadband properties have been difficult to explain with conventional afterglow models, as they either require the power law index of the underlying electron energy distribution to be low, p < 2, or that the outflow is quasi-spherical thus reviving the energy problem. We argue that the s...

Monitoring results are presented for the Stangellini 1 Jy GHz-peaked-spectrum source sample, illustrating that several members exhibit variability in total flux and/or linear polarization over timescales of order a decade. The variability occurs while the spectrum, based on the integrated fluxes, remains steep and characteristic of a transparent source. Total flux variability is unexpected in v...

where the spectral index β is related to p through β = − 2 . β ∼ −3 is observed at microwave frequencies. The linear polarization fraction is at most (in a uniform ~ B field) fs = p+1 p+7/3 ∼ 0.75 for β ∼ −3. The parameter C indicates possible deviations from a pure power-law. Of course, all this is dependent on the position on the sky, i.e one really has Ts(ν0, n̂), β(n̂), C(n̂). The polarization...

Article history: Received 29 June 2011 Received in revised form 8 October 2011 Accepted 9 January 2012 Available online 18 January 2012