Polarization characterization based on multidimensional Stokes vectors applied in aerosol identification

2019 ◽  
Author(s):  
Riwei Liao ◽  
Nan Zeng
Keyword(s):  
Stokes Vectors

scholarly journals Evolving optical polarisation of the black hole X-ray binary MAXI J1820+070

2019 ◽  
Vol 623 ◽  
pp. A75 ◽  
Author(s):  
Alexandra Veledina ◽  
Andrei V. Berdyugin ◽  
Ilia A. Kosenkov ◽  
Jari J. E. Kajava ◽  
Sergey S. Tsygankov ◽  
...  
Keyword(s):  
Black Hole ◽  
Optical Emission ◽  
Position Angle ◽  
Stokes Parameters ◽  
X Ray ◽  
Before And After ◽  
Stokes Vectors ◽  
The Magnetic Field ◽  
Optical Polarisation ◽  
Polarisation Measurements

Aims. The optical emission of black hole transients increases by several magnitudes during the X-ray outbursts. Whether the extra light arises from the X-ray heated outer disc, from the inner hot accretion flow, or from the jet is currently debated. Optical polarisation measurements are able to distinguish the relative contributions of these components. Methods. We present the results of BVR polarisation measurements of the black hole X-ray binary MAXI J1820+070 during the period of March-April 2018. Results. We detect small, ∼0.7%, but statistically significant polarisation, part of which is of interstellar origin. Depending on the interstellar polarisation estimate, the intrinsic polarisation degree of the source is between ∼0.3% and 0.7%, and the polarisation position angle is between ∼10 ° −30°. We show that the polarisation increases after MJD 58222 (2018 April 14). The change is of the order of 0.1% and is most pronounced in the R band. The change of the source Stokes parameters occurs simultaneously with the drop of the observed V-band flux and a slow softening of the X-ray spectrum. The Stokes vectors of intrinsic polarisation before and after the drop are parallel, at least in the V and R filters. Conclusions. We suggest that the increased polarisation is due to the decreasing contribution of the non-polarized component, which we associate with the the hot flow or jet emission. The low polarisation can result from the tangled geometry of the magnetic field or from the Faraday rotation in the dense, ionised, and magnetised medium close to the black hole. The polarized optical emission is likely produced by the irradiated disc or by scattering of its radiation in the optically thin outflow.

Stokes vectors, Mueller matrices, and polarized scattered light

1985 ◽  
Vol 53 (5) ◽  
pp. 468-478 ◽  
Author(s):  
William S. Bickel ◽  
Wilbur M. Bailey
Keyword(s):  
Scattered Light ◽  
Mueller Matrices ◽  
Stokes Vectors

Monte Carlo simulation of Stokes vectors of polarized light scattering from two-dimensional random rough surfaces

2011 ◽  
Vol 58 (18) ◽  
pp. 1651-1658 ◽  
Author(s):  
Shu Jiang ◽  
Chunyong Wang ◽  
Jiancheng Lai ◽  
Baomin Bian ◽  
Jian Lu ◽  
...  
Keyword(s):  
Monte Carlo Simulation ◽  
Monte Carlo ◽  
Light Scattering ◽  
Rough Surfaces ◽  
Polarized Light ◽  
Two Dimensional ◽  
Random Rough Surfaces ◽  
Stokes Vectors

scholarly journals Optical imaging based on time-resolved stokes vectors in filamentous tissues

2003 ◽  
Vol 42 (4) ◽  
pp. 750 ◽  
Author(s):  
Chia-Wei Sun ◽  
Chih-Chung Yang ◽  
Yean-Woei Kiang
Keyword(s):  
Optical Imaging ◽  
Time Resolved ◽  
Stokes Vectors

Stokes vectors and polarization lasers

1985 ◽  
Vol 2 (10) ◽  
pp. 1690 ◽  
Author(s):  
M. V. Tratnik ◽  
J. E. Sipe
Keyword(s):  
Stokes Vectors
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