On the circular polarization in pulsar emission

Kazbegi, A. Z.; Machabeli, G. Z.; Melikidze, George I.

doi:10.1093/mnras/253.3.377

Cited by 148 publications

(158 citation statements)

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“…Though there were many theoretical e †orts (e.g., Gil & Snakowski 1990), no consensus was ever reached on how pulsar polarization was generated (Radhakrishnan 1992 ;Melrose 1995). For example, the observed circular polarization in pulsar radio emission could either be converted from the linear polarization in the pulsar magnetosphere via the propagation e †ect (Melrose 1979 ;Cheng & Ruderman 1979 ;von Hoensbroech & Lesch 1999) or plasma process (e.g., Kazbegi, Machabeli, & Melikidze 1991) or originate from the emission process intrinsically (Radhakrishnan & Rankin 1990 ;Michel 1987 ;Gangadhara 1997).…”

Section: Introductionmentioning

confidence: 99%

An Inverse Compton Scattering Model of Pulsar Emission. III. Polarization

Liu

Han

et al. 2000

ApJ

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Qiao and his collaborators recently proposed an inverse Compton scattering model to explain radio emission from pulsars. In this paper, we investigate the polarization properties of pulsar emission in the model. First of all, using the lower frequency approximation, we derived the analytical amplitude of the inverse Compton scattered wave of a single electron in a strong magnetic Ðeld. We found that the outgoing radio emission of a single relativistic electron scattering o † the "" low-frequency waves ÏÏ produced by gap sparking should be linearly polarized and have no circular polarization at all. However, considering the coherency of the emission from a bunch of electrons, we found that the outgoing radiation from the inner part of the emission beam, i.e., that from the lower emission altitudes, preferentially has to have circular polarization. Computer simulations show that the polarization properties, such as the sense reversal of circular polarization near the pulse center, the S-shape of position angle swing of the linear polarization, and a strong linear polarization in conal components, can be reproduced in the ICS model.

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Section: Introductionmentioning

confidence: 99%

An Inverse Compton Scattering Model of Pulsar Emission. III. Polarization

Liu

Han

et al. 2000

ApJ

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“…Kazbegi et al (1992) demonstrated that the aforementioned waves are excited if the cyclotron resonance condition…”

Section: Main Considerationmentioning

confidence: 99%

Quasi-linear diffusion driving the synchrotron emission in active galactic nuclei

Osmanov

Machabeli

2010

A&A

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Aims. We study the role of the quasi-linear diffusion (QLD) in producing X-ray emission by means of ultra-relativistic electrons in AGN magnetospheric flows. Methods. We examined two regions: (a) an area close to the black hole and (b) the outer magnetosphere. The synchrotron emission has been studied for ultra-relativistic electrons and was shown that the QLD generates the soft and hard X-rays, close to the black hole and on the light cylinder scales respectively. Results. By considering the cyclotron instability, we show that despite the short synchrotron cooling timescales, the cyclotron modes excite transverse and longitudinal-transversal waves. On the other hand, it is demonstrated that the synchrotron reaction force and a force responsible for the conservation of the adiabatic invariant tend to decrease the pitch angles, whereas the diffusion, that pushes back on electrons by means of the aforementioned waves, tends to increase the pitch angles. By examining the quasi-stationary state, we investigate a regime in which these two processes are balanced and a non-vanishing value of pitch angles is created. Conclusions.

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“…The particles moving along the curved field lines drift perpendicularly to the curvature plane. The existence of the drift motion creates the necessary conditions for developing a CDI (see e.g., Kazbegi et al 1989Kazbegi et al , 1991aShapakidze et al 2003). The mechanism excites transverse drift modes providing the magnetic field with the toroidal component.…”

Section: Introductionmentioning

confidence: 99%

Dynamical feedback of the curvature drift instability on its saturation process

Osmanov¹,

Shapakidze²,

Machabeli³

2009

A&A

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Aims. We investigate the reconstruction of pulsar magnetospheres close to the light cylinder surface to study the curvature drift instability (CDI) responsible for the twisting of magnetic field lines in the mentioned zone. The influence of plasma dynamics on the saturation process of the CDI is studied. Methods. On the basis of the Euler, continuity, and induction equations, we derive the increment of the CDI and analyze parametrically excited drift modes. The dynamics of the reconstruction of the pulsar magnetosphere is studied analytically. Results. We show that there is a possibility of a parametrically excited rotational-energy pumping-process in the drift modes. It is indicated by the generation of a toroidal component of the magnetic field that transforms the field lines into such a configuration, in which plasma particles do not experience any forces. At this stage, the instability process saturates and the further amplification of the toroidal component to the magnetic field lines is suspended.

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On the circular polarization in pulsar emission

Cited by 148 publications

References 0 publications

An Inverse Compton Scattering Model of Pulsar Emission. III. Polarization

An Inverse Compton Scattering Model of Pulsar Emission. III. Polarization

Quasi-linear diffusion driving the synchrotron emission in active galactic nuclei

Dynamical feedback of the curvature drift instability on its saturation process

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