PSR B2111+46: a test of the inverse Compton scattering model of radio emission

Zhang, H.; Qiao, G. J.; Han, J. L.; Lee, K. J.; Wang, Hong Guang

doi:10.1051/0004-6361:20066550

Cited by 19 publications

(13 citation statements)

References 26 publications

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“…By fitting Gaussians to its intensity profiles at frequencies 610 MHz and 1408 MHz, we could identify five sub-components: a central (core) component, a pair of inner components and a pair of outer components. Our values of the phase locations of the component peaks are in close agreement with the ones given by Zhang et al (2007) for PSR B2111+46. One can guess at the presence of two inner components hidden between the core and the outer components even by visual inspection.…”

Section: Psr B2111+46supporting

confidence: 90%

Absolute emission altitude of pulsars: PSRs B1839+09, B1916+14, and B2111+46

Thomas

Gangadhara

2010

A&A

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Aims. We study the mean profiles of the multi-component pulsars PSRs B1839+09, B1916+14 and B2111+46. We estimate the emission height of the core components, and hence find the absolute emission altitudes corresponding to the conal components. Methods. By fitting Gaussians to the emission components, we determine the phase location of the component peaks. Our findings indicate that the emission beams of these pulsars have the nested core-cone structures. Based on the phase location of the component peaks, we estimate the aberration-retardation (A/R) phase shifts in the profiles. Due to the A/R phase shift, the peak of the core component in the intensity profile and the inflection point of the polarization angle swing are found to be symmetrically shifted in the opposite directions with respect to the meridional plane in such a way that the core shifts towards the leading side and the polarization angle inflection point towards the trailing side. Results. We have been able to locate the phase location of the meridional plane and to estimate the absolute emission altitude of both the core and the conal components relative to the neutron star center, using the exact expression for the A/R phase shift given by Gangadhara (2005).

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Section: Psr B2111+46supporting

confidence: 90%

Absolute emission altitude of pulsars: PSRs B1839+09, B1916+14, and B2111+46

Thomas

Gangadhara

2010

A&A

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“…This pulsar has a multicomponent profile, with a well‐identified core component and two cones of emission (e.g. Zhang et al 2007). It has a rotation period of 1.014 s and α= 14 and β=−1.4 (Mitra & Li 2004).…”

Section: Resultsmentioning

confidence: 99%

Understanding the effects of geometry and rotation on pulsar intensity profiles

Thomas¹,

Gupta²,

Gangadhara³

2010

Monthly Notices of the Royal Astronomical Society

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We have developed a method to compute the possible distribution of radio emission regions in a typical pulsar magnetosphere, taking into account the viewing geometry and rotational effects of the neutron star. Our method can estimate the emission altitude and the radius of curvature of particle trajectory as a function of rotation phase for a given inclination angle, impact angle, spin period, Lorentz factor, field line constant and the observation frequency. Further, using curvature radiation as the basic emission mechanism, we simulate the radio intensity profiles that would be observed from a given distribution of emission regions, for different values of radio frequency and Lorentz factor. We show clearly that rotation effects can introduce significant asymmetries into the observed radio profiles. We investigate the dependency of profile features on various pulsar parameters. We find that the radiation from a given ring of field lines can be seen over a large range of pulse longitudes, originating at different altitudes, with varying spectral intensity. Preferred heights of emission along discrete sets of field lines are required to reproduce realistic pulsar profiles, and we illustrate this for a known pulsar. Finally, we show how our model provides feasible explanations for the origin of core emission, and also for one‐sided cones which have been observed in some pulsars.

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“…(1) It is suspected that the radio emission beam of pulsars may include core and multi-cone components (Rankin 1983(Rankin , 1993Lyne & Manchester 1988;Wu et al 1992Wu et al , 1998Manchester 1995;Zhang et al 2007). Now, the pulse profiles of PSRs B0329+54 and B1642−03 show obvious multi-peak, which can be described by multiGaussian functions ( 5 Gaussians for PSR B0329+54 and 3 Gaussians for PSR B1642−03, see Fig.1 and Fig.2 for details ), which supports the scenario of core and cone components.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…In these two regions, the radio emission is believed to be generated by inverse Compton scattering (ICS) process between the secondary relativistic particles and low frequency waves (Qiao 1988a,b;Qiao & Lin 1998). The ICS model can explain the pulse profiles with peaks number from one to five (Qiao & Lin 1998;Zhang et al 2007), the widening or narrowing profiles with frequency increasing, the "mode changing" behavior (Qiao et al 1996;Zhang et al 1997a,b), and the polarization (Xu et al 1997(Xu et al , 2000(Xu et al , 2001. Besides, this model combined with CG and AG can explain many observation phenomena at high energy bands (Qiao et al 2004a;Lee et al 2006aLee et al ,b, 2009Lee et al , 2010Du et al 2010Du et al , 2011Du et al , 2012Du et al , 2013Du et al , 2015.…”

Section: Introductionmentioning

confidence: 99%

Investigating the multifrequency pulse profiles of PSRs B0329+54 and B1642–03 in an inverse Compton scattering model

Shang

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The emission geometries, e.g. the emission region height, the beam shape, and radiusto-frequency mapping, are important predictions of pulsar radiation model. The multiband radio observations carry such valuable information. In this paper, we study two bright pulsars, (PSRs B0329+54 and B1642−03) and observe them in high frequency (2.5 GHz, 5 GHz, and 8 GHz). The newly acquired data together with historical archive provide an atlas of multi-frequency profiles spanning from 100 MHz to 10 GHz. We study the frequency evolution of pulse profiles and the radiation regions with the these data. We firstly fit the pulse profiles with Gaussian functions to determine the phase of each component, and then calculate the radiation altitudes of different emission components and the radiation regions. We find that the inverse Compton scattering (ICS) model can reproduce the radiation geometry of these two pulsars. But for PSR B0329+54 the radiation can be generated in either annular gap (AG) or core gap (CG), while the radiation of PSR B1642−03 can only be generated in the CG. This difference is caused by the inclination angle and the impact angle of these two pulsars. The relation of beaming angle (the angle between the radiation direction and the magnetic axis) and the radiation altitudes versus frequency is also presented by modelling the beam-frequency evolution in the ICS model. The multi-band pulse profiles of these two pulsars can be described well by the ICS model combined with the CG and AG.

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PSR B2111+46: a test of the inverse Compton scattering model of radio emission

Cited by 19 publications

References 26 publications

Absolute emission altitude of pulsars: PSRs B1839+09, B1916+14, and B2111+46

Absolute emission altitude of pulsars: PSRs B1839+09, B1916+14, and B2111+46

Understanding the effects of geometry and rotation on pulsar intensity profiles

Investigating the multifrequency pulse profiles of PSRs B0329+54 and B1642–03 in an inverse Compton scattering model

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