Cascade process in strong magnetic and electric fields under astrophysical conditions

Alber, Ya. I.; Krotova, Z. N.; Eidman, V.Ya.

doi:10.1007/bf01002454

Cited by 15 publications

(9 citation statements)

References 3 publications

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“…In the first work about modelling of time‐dependent cascades by Al’Ber et al (1975) a zero‐dimensional model was used – only temporal, but not spatial, variations in particle number density were considered. In that model, the production of larger amount of particles than necessary for screening of the electric field was due to the time delay between the photon emissions and absorptions.…”

Section: Discussionmentioning

confidence: 99%

“…Only few attempts have been made before to construct quantitative models for non‐stationary cascades. Al’Ber, Krotova & Eidman (1975) were the first, their model was 0D – it accounted only for variability in time. It predicted strong time variability in pair creation rate due to the delay between emission of a high‐energy photon and its decay into an electron–positron pair.…”

Section: Introductionmentioning

confidence: 99%

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Time-dependent pair cascades in magnetospheres of neutron stars - I. Dynamics of the polar cap cascade with no particle supply from the neutron star surface

Timokhin¹

2010

Monthly Notices of the Royal Astronomical Society

177

139

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I argue that the problem of electromagnetically driven electron–positron cascades in magnetospheres of neutron stars must be addressed starting from first principles. I describe a general numerical algorithm for doing self‐consistent kinetic simulations of electron–positron cascades – wherein particle acceleration, pair creation and screening of the electric field are calculated simultaneously – and apply it to model the Ruderman & Sutherland cascade in one dimension. I find that pair creation is quite regular and quasi‐periodic. In each cycle a blob of ultra‐relativistic electron–positron plasma is generated; it propagates into the magnetosphere leaving a tail of less relativistic plasma behind, and the next discharge occurs when this mildly relativistic plasma leaves the polar cap. A short burst of pair formation is followed by a longer quiet phase when accelerating electric field is screened and no pairs are produced. Some of freshly injected electron–positrons pairs get trapped in plasma oscillations creating a population of low‐energy particles. The cascade easily adjusts to the current density required by the pulsar magnetosphere by reversing some of the low‐energy particles. Each discharge generates a strong coherent superluminal electrostatic wave, which may be relevant for the problem of pulsar radioemission.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Time-dependent pair cascades in magnetospheres of neutron stars - I. Dynamics of the polar cap cascade with no particle supply from the neutron star surface

Timokhin¹

2010

Monthly Notices of the Royal Astronomical Society

177

139

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“…The inhomogeneities, which lead to (partially) coherent radiation, are associated with evolution of instabilities of the bunches in magnetospheric plasma [4]. Initial inhomogeneities already appear at the electrons emission from the surface of the star or at the beginning of the positrons return motion in the lower magnetosphere [5,[35][36][37][38][39] (for the analogies in the electron beams ejected from the Sun see e.g. [40]).…”

Section: Discussionmentioning

confidence: 99%

On the Mystery of the Interpulse Shift in the Crab Pulsar

Конторович¹,

Trofymenko²

2017

JPSA

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Abstract:A new mechanism of radiation emission in the polar gap of a pulsar is proposed. It is the curvature radiation emitted by positrons moving towards the surface of the neutron star along inclined magnetic field and reflected from the surface. Such radiation interferes with transition radiation emitted from the neutron star when positrons hit the surface. Proposed mechanism explains the mystery of the interpulse shift in the Crab pulsar at high frequencies discovered by Moffett and Hankins twenty years ago. We have found also reflected energy flux and spectrum, discussed coherence and disappearance of interpulse shift with increase of frequency.

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“…See Lyne & Manchester (1988). (1975), as well as by Eidman's group (Al'ber et al 1975). The continuous escape of particles along the open field lines leads to formation of a strong electric field along the magnetic field.…”

Section: Electron-positron Generationmentioning

confidence: 99%

Radio Pulsars

et al. 2015

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Almost 50 years after radio pulsars were discovered in 1967, our understanding of these objects remains incomplete. On the one hand, within a few years it became clear that neutron star rotation gives rise to the extremely stable sequence of radio pulses, that the kinetic energy of rotation provides the reservoir of energy, and that electromagnetic fields are the braking mechanism. On the other hand, no consensus regarding the mechanism of coherent radio emission or the conversion of electromagnetic energy to particle energy yet exists. In this review, we report on three aspects of pulsar structure that have seen recent progress: the self-consistent theory of the magnetosphere of an oblique magnetic rotator; the location, geometry, and optics of radio emission; and evolution of the angle between spin and magnetic axes. These allow us to take the next step in understanding the physical nature of the pulsar activity.

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Cascade process in strong magnetic and electric fields under astrophysical conditions

Cited by 15 publications

References 3 publications

Time-dependent pair cascades in magnetospheres of neutron stars - I. Dynamics of the polar cap cascade with no particle supply from the neutron star surface

Time-dependent pair cascades in magnetospheres of neutron stars - I. Dynamics of the polar cap cascade with no particle supply from the neutron star surface

On the Mystery of the Interpulse Shift in the Crab Pulsar

Radio Pulsars

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