Potential drops above pulsar polar caps - Acceleration of nonneutral beams from the stellar surface

Fawley, William M.; Arons, Jonathan; Scharlemann, E.T.

doi:10.1086/155573

Cited by 109 publications

(72 citation statements)

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“…where GJ is the GJ charge density and the term j R is a combination of the fields and their derivatives and is given explicitly in Fawley et al (1977). The electromagnetic fields, current density, and charge density are in the corotating frame.…”

Section: Oscillating Pair-creating Electric Fieldmentioning

confidence: 99%

“…Reflecting secondaries ( positrons if the primaries are electrons) provide a net quasistatic charge density, such that the PFF may be regarded as a thin surface with a surface charge density. The resulting additional electrostatic field screens out the initial E k above the PFF (e.g., Fawley et al 1977;Arons & Scharlemann 1979;Shibata et al 1998). In some pulsar models pairs are also assumed to be produced in an ''outer gap'' (Cheng et al 1986), and current conservation can be achieved by the currents through the inner and outer gaps being part of a global circuit (Shibata 1991).…”

Section: Introductionmentioning

confidence: 99%

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Large‐Amplitude, Pair‐creating Oscillations in Pulsar and Black Hole Magnetospheres

Levinson

Melrose

Judge

et al. 2005

ApJ

103

136

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A time-dependent model for pair creation in a pulsar magnetosphere is developed in which the parallel electric field oscillates with large amplitude. Electrons and positrons are accelerated periodically, and the amplitude of the oscillations is assumed to be large enough to cause creation of upgoing and downgoing pairs at different phases of the oscillation. With a charge-starved initial condition, we find that the oscillations result in bursts of pair creation in which the pair density rises exponentially with time. The pair density saturates at N AE ' E 2 0 /(8 m e c 2 À thr ), where E 0 is the parallel electric field in the charge-starved initial state and À thr is the Lorentz factor for effective pair creation. The frequency of oscillations following the pair creation burst is given roughly by ! osc ¼ eE 0 /(8m e cÀ thr ). A positive feedback keeps the system stable, such that the average pair creation rate balances the loss rate due to pairs escaping the magnetosphere.

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Section: Oscillating Pair-creating Electric Fieldmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Large‐Amplitude, Pair‐creating Oscillations in Pulsar and Black Hole Magnetospheres

Levinson

Melrose

Judge

et al. 2005

ApJ

103

136

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“…There are other models of the space-charge-limited potential, such as the model discussed by Michel (1974) and also by Fawley, Arons & Scharlemann (1977) and Cheng & Ruderman (1977), which do not rely on field line curvature and in general give a lower voltage. The potential discussed by Michel (1974) arises from the deviation of the charge density from the GJ value because of particle inertia, i.e.…”

Section: Limits On Particle Energies By Resonant Inverse Compton Scatmentioning

confidence: 99%

“…the velocity v(x) and the magnetic field B(x) have different scaling with x, such that the charge density cannot be maintained at the GJ density all the way along open field lines. The corresponding potential can be described by (Fawley, Arons & Scharlemann 1977) φ…”

Section: Limits On Particle Energies By Resonant Inverse Compton Scatmentioning

confidence: 99%

Resonant Inverse Compton Scattering above Polar Caps: Gap Acceleration Efficiency for Young Pulsars

Luo

Protheroe

1998

Publ. – Astron. Soc. Aust

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It is shown that for moderately hot polar caps (with effective temperature of ∼10 6 K), the efficiency of polar gap acceleration is lower compared to the case in which the polar caps are relatively cool and inverse Compton scattering plays no role in controlling the gap. For young pulsars with superstrong magnetic fields (≥ 10 9 T) and hot polar caps (with temperature of ≥5×10 6 K), because of the energy loss of electrons or positrons due to resonant inverse Compton scattering in the vicinity of polar caps, pair cascades occur at distances further away from the polar cap, and in this case we have a relatively high acceleration efficiency, with ions carrying most of the particle luminosity.

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“…Further out, the usual effects of field line curvature (one way or the other) need to be included. By contrast MT follow the approach of Jon Arons and colleagues (Fawley et al 1977;Scharlemann et al 1978): they assume that v stays equal to c. (They do not discuss the initial acceleration by a super-GJ density from v < c to v « c, an essential feature of the Arons et al solution). The continuity condition (11) then requires ap e oc B on a streamline.…”

Section: Gmdr 2 J Fr G \[Rmentioning

confidence: 99%

General Relativistic Electrodynamics and Pulsar Theory

Mestel

1996

International Astronomical Union Colloquium

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Potential drops above pulsar polar caps - Acceleration of nonneutral beams from the stellar surface

Cited by 109 publications

References 0 publications

Large‐Amplitude, Pair‐creating Oscillations in Pulsar and Black Hole Magnetospheres

Large‐Amplitude, Pair‐creating Oscillations in Pulsar and Black Hole Magnetospheres

Resonant Inverse Compton Scattering above Polar Caps: Gap Acceleration Efficiency for Young Pulsars

General Relativistic Electrodynamics and Pulsar Theory

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