Polarized emission effect realized in CH3NH3PbI3 perovskite nanocrystals

2017 ◽  
Vol 5 (34) ◽  
pp. 8699-8706 ◽  
Author(s):  
Zhi-Feng Shi ◽  
Ying Li ◽  
Sen Li ◽  
Hui-Fang Ji ◽  
Ling-Zhi Lei ◽  
...  
Keyword(s):  
Linear Polarization ◽  
Polarization Degree ◽  
Perovskite Nanocrystals ◽  
Polarized Emission ◽  
Emission Effect

A polarized emission effect has been realized in CH3NH3PbI3 perovskite nanocrystals with a linear polarization degree of 0.28.

Comparison of linear polarization degree in healthy and wounded rat skin

2001 ◽  
Author(s):  
Martha S. Ribeiro ◽  
Anderson Z. Freitas ◽  
Daniela F. Silva ◽  
Denise M. Zezell ◽  
Cleusa M. R. Pellegrini ◽  
...  
Keyword(s):  
Linear Polarization ◽  
Polarization Degree ◽  
Rat Skin

3mm POLARIZATION PROPERTIES OF OPTICAL AND γ-RAY CLASSES OF BLAZARS

2010 ◽  
Vol 19 (06) ◽  
pp. 923-929
Author(s):  
I. AGUDO ◽  
C. THUM ◽  
H. WIESEMEYER ◽  
T. P. KRICHBAUM
Keyword(s):  
Linear Polarization ◽  
Position Angle ◽  
Polarization Degree ◽  
Polarization Angle ◽  
Marginal Effect ◽  
Bl Lacertae ◽  
All Optical ◽  
Linearly Polarized ◽  
Γ Ray ◽  
The One

We have performed the first 3.5 mm polarimetric survey of radio loud active galactic nuclei (AGN) with the IRAM 30 m Telescope. Unlike radio wavelengths, millimeter observations allow us to measure the intrinsic linearly polarized emission from AGN, thanks to the marginal effect of Faraday rotation and depolarization at mm wavelengths. The sample contains 145 sources, and it essentially consists of all flat-spectrum AGN with declinations accessible to the 30 m Telescope (Dec. ( J 2000.0) > -30°), and with 3 mm flux density ≳ 1 Jy, as measured from 1978 to 1994. LBAS quasars in our sample show larger luminosity than non-LBAS ones, which is consistent with previous work claiming larger Doppler factors for brighter γ-ray blazars. This effect cannot be claimed for BL Lacertae objects in our sample, which suggests that only quasars contribute to distribute LBAS blazars towards larger luminosities. We find a systematic 3.5 mm linear polarization degree excess by a factor of ~ 2 with regard to the one at 2 cm for all optical and γ-ray classes of sources considered here. Our sample shows a significant trend to increase the luminosity of their jets for decreasing linear polarization fraction. Unlike previous studies in the radio spectral range, we do not find a clear relation between the linear polarization angle and the jet structural position angle of any source class in our sample. This is interpreted as a markedly non-axisymmetric character of the 3 mm emitting region of radio loud AGN jets.

scholarly journals Characterization of mid-infrared polarization due to scattering in protoplanetary disks

2020 ◽  
Vol 634 ◽  
pp. A129 ◽  
Author(s):  
S. Heese ◽  
S. Wolf ◽  
R. Brauer
Keyword(s):  
Magnetic Fields ◽  
Linear Polarization ◽  
Radial Distance ◽  
Protoplanetary Disks ◽  
Field Studies ◽  
Central Star ◽  
Polarization Degree ◽  
Mid Infrared ◽  
Stellar Radiation ◽  
Linearly Polarized

Context. It is generally assumed that magnetic fields play an important role in the formation and evolution of protoplanetary disks. One way of observationally constraining magnetic fields is to measure polarized emission and absorption produced by magnetically aligned elongated dust grains. The fact that radiation also becomes linearly polarized by light scattering at optical to millimeter wavelengths complicates magnetic field studies. Aims. We characterize the linear polarization of mid-infrared radiation due to scattering of the stellar radiation and dust thermal re-emission radiation (self-scattering). Methods. We computed the radial polarization profiles at wavelengths across the N and Q bands for a broad range of circumstellar disk configurations. These simulations served as a basis to analyze the correlations between selected disk parameters and the resulting linear polarization. Results. We find that the thermal re-emission radiation is stronger than the scattered stellar radiation for disks with inner holes smaller than ~10 au within the considered parameter range. The mid-infrared polarization due to scattering shows several clear trends: for scattered stellar radiation only, the linear polarization degree decreases slightly with increasing radial distance, while it increases with radial distance for thermal re-emission radiation only and for a combination of scattered stellar radiation and thermal re-emission radiation. The linear polarization degree decreases with increasing disk flaring and luminosity of the central star. An increasing inner radius shifts the increase of the linear polarization degree further outside, while a larger scale height increases the linear polarization degree for small radial distances and decreases this degree further outside. For longer wavelengths, i.e., toward the Q band in our study, the linear polarization degree converges more slowly. Conclusions. We found several clear trends for polarization due to scattering. These trends are the basis to distinguish polarization due to scattering from polarization due to dichroic emission and absorption.

scholarly journals The Magnetic Field in M33

1990 ◽  
Vol 140 ◽  
pp. 210-210
Author(s):  
U.R. Buczilowski ◽  
R. Beck
Keyword(s):  
Magnetic Field ◽  
Linear Polarization ◽  
Supernova Remnant ◽  
Nearby Galaxy ◽  
Polarized Emission ◽  
The Galaxy ◽  
The Magnetic Field

Measurements at five radio wavelengths between 2.8 and 21.1 cm (Buczilowski and Beck, 1987) with the Effelsberg 100-m telescope make M33 the best studied nearby galaxy in linear polarization so far. The polarized emission is concentrated to the northwestern quadrant of the galaxy. Almost no polarization is detectable around the 35 known supernova remnant candidates. The explosions may have disturbed the interstellar magnetic field on scale sizes smaller than our antenna beams.

Anisotropy of the Porous Silicon Photoluminescence

1996 ◽  
Vol 452 ◽  
Author(s):  
G. Polisski ◽  
B. Averboukh ◽  
D. Kovalev ◽  
F. Koch
Keyword(s):  
Porous Silicon ◽  
Memory Effect ◽  
Linear Polarization ◽  
Polarized Light ◽  
Optical Excitation ◽  
Polarization Degree ◽  
Porous Si ◽  
Si Substrate ◽  
Plane Distribution

AbstractPolarization memory effect in the porous Si photoluminescence is studied. The anisotropy of the linear polarization degree is found in the samples etched with polarized light-assistance. The effect is explained by the anisotropie in plane distribution of the elongated Si crystallites. Under resonant optical excitation four-fold anisotropy of the photoluminescence polarization, linked to the crystalline axes of the bulk Si substrate, is observed.

P‐83: Polarized Emission from Perovskite Nanocrystals Encapsulated in Stretched Porous Films for Liquid Crystal Displays

2021 ◽  
Vol 52 (1) ◽  
pp. 1391-1394
Author(s):  
Gao Yiyang ◽  
Maksym F. Prodanov ◽  
Kang Chengbin ◽  
Valerii V. Vashchenko ◽  
Abhishek K. Srivastava
Keyword(s):  
Liquid Crystal ◽  
Liquid Crystal Displays ◽  
Porous Films ◽  
Perovskite Nanocrystals ◽  
Polarized Emission

scholarly journals Nanoscopic surface inspection by analyzing the linear polarization degree of the scattered light

2009 ◽  
Vol 34 (12) ◽  
pp. 1906 ◽  
Author(s):  
P. Albella ◽  
J. M. Saiz ◽  
J. M. Sanz ◽  
F. González ◽  
F. Moreno
Keyword(s):  
Linear Polarization ◽  
Scattered Light ◽  
Polarization Degree ◽  
Surface Inspection
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