2017MNRAS.472.4598D


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.13CEST05:36:02

2017MNRAS.472.4598D - Mon. Not. R. Astron. Soc., 472, 4598-4617 (2017/December-3)

The origin of radio pulsar polarization.

DYKS J.

Abstract (from CDS):

Polarization of radio pulsar profiles involves a number of poorly understood, intriguing phenomena, such as the existence of comparable amounts of orthogonal polarization modes (OPMs), strong distortions of polarization angle (PA) curves into shapes inconsistent with the rotating vector model (RVM), and the strong circular polarization V which can be maximum (instead of zero) at the OPM jumps. It is shown that the comparable OPMs and large V result from a coherent addition of phase-delayed waves in natural propagation modes, which are produced by a linearly polarizedemitted signal. The coherent mode summation implies opposite polarizationproperties to those known from the incoherent case, in particular, the OPM jumps occur at peaks of V, whereas V changes sign at a maximum linear polarization fraction L/I. These features are indispensable to interpret various observed polarization effects. It is shown that statistical properties of emission and propagation can be efficiently parametrized in a simple model of coherent mode addition, which is successfully applied to complex polarization phenomena, such as the stepwise PA curve of PSR B1913+16 and the strong PA distortions within core components of pulsars B1933+16 and B1237+25. The inclusion of coherent mode addition opens the possibility for a number of new polarization effects, such as inversion of relative modal strength, twin minima in L/I coincident with peaks in V, 45° PA jumps in weakly polarized emission, and loop-shaped core PA distortions. The empirical treatment of the coherency of mode addition makes it possible to advance the understanding of pulsar polarization beyond the RVM model.

Abstract Copyright: © 2017 The Author Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): radiation mechanisms: non-thermal - pulsars: general - pulsars: individual: PSR B1237+25 - pulsars: individual: PSR B1913+16 - pulsars: individual: PSR B1933+16 - pulsars: individual: PSR B1919+21 - pulsars: individual: PSR B1919+21

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 PSR B0301+19 Psr 03 04 33.115 +19 32 51.40           ~ 207 0
2 PSR B0329+54 Psr 03 32 59.3462817079 +54 34 45.047901390           ~ 588 1
3 PSR J0437-47 Psr 04 37 15.99744 -47 15 09.7170           DC 784 0
4 PSR B0525+21 Psr 05 28 52.308 +22 00 01.00     14.30     ~ 333 0
5 PSR B0823+26 Psr 08 26 51.4 +26 37 23           ~ 474 1
6 PSR J1024-0719 Psr 10 24 38.697 -07 19 19.07           ~ 193 0
7 PSR B1133+16 Psr 11 36 03.0720 +15 51 15.500           ~ 618 0
8 PSR B1237+25 Psr 12 39 40.386 +24 53 49.87           ~ 421 0
9 PSR B1541+09 Psr 15 43 38.815 +09 29 16.50           ~ 183 0
10 PSR B1839+09 Psr 18 41 55.9380 +09 12 08.300           ~ 107 0
11 PSR B1857-26 Psr 19 00 47.5440 -26 00 44.200           ~ 158 0
12 PSR J1915+1606 Psr 19 15 27.99999 +16 06 27.4034     22.5     ~ 936 1
13 PSR B1919+21 Psr 19 21 44.815 +21 53 02.25           ~ 354 0
14 PSR B1933+16 Psr 19 35 47.7012077756 +16 16 40.025845719           ~ 277 1
15 PSR B1946+35 Psr 19 48 25.0067 +35 40 11.057           ~ 156 0
16 PSR B2110+27 Psr 21 13 04.3895 +27 54 02.290           ~ 94 0

    Equat.    Gal    SGal    Ecl

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2021.04.13-05:36:02

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