Plasma model of pulsar emission and some observational consequences

Kazbegi, A. Z.; Machabeli, G. Z.; Melikidze, George I.; Smirnova, T. V.

doi:10.1007/bf01004795

Cited by 27 publications

(38 citation statements)

References 4 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Importance of anomalous cyclotron resonance for pulsar radio emission has been discussed in Refs. [10,11,12]. A curious property of anomalous cyclotron resonance is that cyclotron waves can be emitted at frequencies well below the local cyclotron frequency (recall that in Crab near the light cylinder ω p /ω B ∼ 2 × 10 −3 ).…”

Section: Crab Giant Pulsesmentioning

confidence: 99%

Neutron star magnetospheres: the binary pulsar, Crab and magnetars

Lyutikov

2008

AIP Conference Proceedings

View full text Add to dashboard Cite

Abstract. A number of disparate observational and theoretical pieces of evidence indicate that, contrary to the conventional wisdom, neutron stars' closed field lines are populated by dense, hot plasma and may be responsible for producing some radio and high energy emission. This conclusion is based on eclipse modeling of the binary pulsar system PSR J0737-3039A/B (Lyutikov & Thompson 2005), a quantitative theory of Crab giant pulses (Lyutikov 2007) and a number of theoretical works related to production of non-thermal spectra in magnetars through resonant scattering. In magnetars, dense pair plasma is produced by twisting magnetic field lines and associated electric fields required to lift the particles from the surface. In long period pulsars, hot particles on closed field lines can be efficiently trapped by magnetic mirroring, so that relatively low supply rate, e.g. due to a drift from open field lines, may result in high density. In short period pulsars, magnetic mirroring does not work; large densities may still be expected at the magnetic equator near the Y-point. SECRET LIVES OF CLOSED FIELD LINESOur understanding of pulsars is based on the Goldreich-Julian model [1], which postulates that pulsars are endowed with dipolar magnetic field; most magnetic field lines close back to the star, while those originating near the magnetic poles are open to infinity. All the action, like generation of radio and high energy emission, is assumed to take place on open field lines. Closed lines are assumed to be nearly dead, only carrying a particle density equal to the minimal charge density required by the electrodynamic conditions.A number of recent observational and theoretical developments indicate that (at least in some parts of magnetosphere) the real particle density on closed field lines exceeds this minimal value by a large factor, of the order of 10 4 − 10 5 and that these particles can produce radio and high energy emission, as we describe in these proceedings. Eclipses in the double pulsar PSR J0737-3039A/BIn this system a fast recycled Pulsar A with period P A = 22.7 msec orbits a slower but younger Pulsar B which has a period P B = 2.77 sec in tightest binary neutron star orbit of 2.4 hours [2]. In addition to testing general relativity, this system provides a truly golden opportunity to verify and advance our models of pulsars magnetospheres, mechanisms of generation of radio emission and properties of their relativistic winds. This is made possible by a lucky fact that the line of sight lies almost in the orbital plane, with inclination less than half degree [3,4]. Most strikingly, Pulsar A is eclipsed

show abstract

Section: Crab Giant Pulsesmentioning

confidence: 99%

Neutron star magnetospheres: the binary pulsar, Crab and magnetars

Lyutikov

2008

AIP Conference Proceedings

View full text Add to dashboard Cite

show abstract

“…The aim of this paper is to explain the phenomenon of drifting subpulses in pulsar radio emission within the framework of the theory developed previously (Kazbegi et al 1989a(Kazbegi et al , 1989b(Kazbegi et al , 1991. The pulsar magnetosphere is filled with an electron-positron plasma flowing along the open magnetic field lines.…”

Section: Introductionmentioning

confidence: 99%

The Nature of Pulsar Subpulse Drift

Kazbegi¹,

Machabeli²,

Melkidze³

1991

Aust. J. Phys.

View full text Add to dashboard Cite

A possible mechanism for the explanation of pulsar subpulse drift is suggested. In the region of the open magnetic field lines the existence of an electron-positron plasma penetrated by a primary particle beam is assumed. There is a possibility of excitation of large-scale drift waves propagating transversely to the magnetic field lines. These waves can affect the fulfilment of the radio-wave generation conditions. If the pulsar angular velocity is near to the frequency of the drift waves one should observe regular drift phenomena.

show abstract

“…This theory can also be ruled out on observational grounds (Lesch, Kramer, & Kunzl 1998). In addition to the work of Lesch et al (1998) we note that this theory also fails to explain the observed correlations of the conal peaks (Kazbegi et al 1991a) and the large size of the emitting region (Gwinn et al 1997).…”

Section: Introductionmentioning

confidence: 74%

“…We discuss the linear theory of wave excitation in the pulsar magnetosphere developed by Lominadze, Machabeli, & Mikhailovskii (1979), Machabeli & Usov (1979), Kazbegi et al (1991a), Kazbegi, Machabeli, & Melikidze (1991b), , and .…”

Section: Introductionmentioning

confidence: 99%

The Mechanisms for the Generation of Pulsar Radio and High-energy Emission

Machabeli

2001

Publ. – Astron. Soc. Aust

View full text Add to dashboard Cite

The recent theory of propagation and generation of waves in a pulsar’s magnetosphere is discussed. In particular we consider models of pulsar radio emission due to plasma instabilities. Wave–particle interactions can lead to quasilinear diffusion increasing a particle’s pitch-angle. The recent model of γ-ray emission from synchrotron radiation as a result of quasilinear diffusion is discussed.

show abstract

Plasma model of pulsar emission and some observational consequences

Cited by 27 publications

References 4 publications

Neutron star magnetospheres: the binary pulsar, Crab and magnetars

Neutron star magnetospheres: the binary pulsar, Crab and magnetars

The Nature of Pulsar Subpulse Drift

The Mechanisms for the Generation of Pulsar Radio and High-energy Emission

Contact Info

Product

Resources

About