On Pair Production in the Crab Pulsar

Kunzl, Thomas; Lesch, H.; Jessner, A.; Hoensbroech, A. von

doi:10.1086/311610

Cited by 29 publications

(29 citation statements)

References 12 publications

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“…We therefore suggest the highly unsteady, bursty MP emission we see from 1 to 10 GHz reflects unsteady plasma flow due to sub-GJ charge densities in the emission region (cf. also Kunzl et al 1998, who drew the same conclusion from a somewhat different argument).…”

Section: à3mentioning

confidence: 70%

Radio Emission Signatures in the Crab Pulsar

Hankins

Eilek

2007

ApJ

257

331

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Our high time resolution observations of individual pulses from the Crab pulsar show that both the time and frequency signatures of the interpulse are distinctly different from those of the main pulse. Main pulses can occasionally be resolved into short-lived, relatively narrowband nanoshots. We believe these nanoshots are produced by soliton collapse in strong plasma turbulence. Interpulses at centimeter wavelengths are very different. Their dynamic spectrum contains regular, microsecond-long emission bands. We have detected these bands, proportionately spaced in frequency, from 4.5 to 10.5 GHz. The bands cannot easily be explained by any current theory of pulsar radio emission; we speculate on possible new models.

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Section: à3mentioning

confidence: 70%

Radio Emission Signatures in the Crab Pulsar

Hankins

Eilek

2007

ApJ

257

331

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“…Daugherty & Harding 1982; Hibschman & Arons 2001). Kunzl et al (1998) argued that too high a density of secondary particles in the magnetosphere is in contradiction to the observed low‐frequency emission from radio pulsars, implying η≲ 100. The physical parameters for the plasma in the closed‐field‐line region of a pulsar are also not well constrained.…”

Section: Dielectric Tensor For a Streaming Electron–positron Plasmamentioning

confidence: 99%

Wave modes in the magnetospheres of pulsars and magnetars

Wang

Lai

2007

Monthly Notices of the Royal Astronomical Society

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We study the wave propagation modes in the relativistic streaming pair plasma of the magnetospheres of pulsars and magnetars, focusing on the effect of vacuum polarization. We show that the combined plasma and vacuum polarization effects give rise to a vacuum resonance, where ‘avoided mode crossing’ occurs between the extraordinary mode and the (superluminous) ordinary mode. When a photon propagates from the vacuum‐polarization‐dominated region at small radii to the plasma‐dominated region at large radii, its polarization state may undergo significant change across the vacuum resonance. We map out the parameter regimes (e.g. field strength, plasma density and Lorentz factor) under which the vacuum resonance occurs and examine how wave propagation is affected by the resonance. Some possible applications of our results are discussed, including high‐frequency radio emission from pulsars and possibly magnetars, and optical/infrared emission from neutron star surfaces and inner magnetospheres.

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“…The operation of the curvature radiation in pulsar magnetosphere is, however, still a matter of debate (e.g. Luo & Melrose 1992; Kunzl et al 1998).…”

Section: Limitations On the Validity And Applicability Of The Lineamentioning

confidence: 99%

Altitude-dependent polarization in radio pulsars

Dyks

2008

Monthly Notices of the Royal Astronomical Society

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Because of the corotation, the polarization angle (PA) curve of a pulsar lags the intensity profile by 4r/Rlc rad in pulse phase. I present a simple and short derivation of this delay-radius relation to show that it is not caused by the aberration (understood as the normal beaming effect) but purely by contribution of corotation to the electron acceleration in the observer's frame. Available altitude-dependent formulae for the PA curve are expressed through observables and emission altitude to make them immediately ready to use in radio data modelling. The analytical approximations for the altitude-dependent PA curve are compared with exact numerical results to show how they perform at large emission altitudes. I also discuss several possible explanations for the opposite-than-normal shift of PA curve, exhibited by the pedestal emission of B1929+10 and B0950+08.Comment: 12 pages, 5 figures, accepted by MNRAS after minor change

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On Pair Production in the Crab Pulsar

Cited by 29 publications

References 12 publications

Radio Emission Signatures in the Crab Pulsar

Radio Emission Signatures in the Crab Pulsar

Wave modes in the magnetospheres of pulsars and magnetars

Altitude-dependent polarization in radio pulsars

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