<i>Physics of the Pulsar Magnetosphere</i>

Бескин, В. С.; Gurevich, A. V.; Istomin, Ya. N.; Arons, Jonathan

doi:10.1063/1.2808674

Cited by 135 publications

(221 citation statements)

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“…Let us cite the work by Mestel, Panagi & Shibata (1999) who determined the pulsar magnetosphere in the case of a perpendicular rotator. They reproduced a special case of the results preserved by Beskin, Gurevich & Istomin (1983) who obtained solutions for arbitrary inclination angle. The current formed no only by the particle flow but also the displacement current act to distort field lines.…”

Section: The Pulsar Equationsupporting

confidence: 69%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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Neutron stars are fascinating astrophysical objects immersed in strong gravitational and electromagnetic fields, at the edge of our current theories. These stars manifest themselves mostly as pulsars, emitting a timely very stable and regular electromagnetic signal. Even though discovered almost fifty years ago, they still remain mysterious compact stellar objects. In this review, we summarize the most fundamental theoretical aspects of neutron star magnetospheres and winds. The main competing models explaining their radiative properties like multi-wavelength pulse shapes and spectra and the underlying physical processes such as pair creation and radiation mechanisms are scrutinized. A global but still rather qualitative picture slowly emerges thanks to recent advances in numerical simulations on the largest scales. However considerations about pulsar magnetospheres remain speculative. For instance, the exact composition of the magnetospheric plasma is not yet known. Is it solely filled with a mixture of e ± leptons or does it contain a non-negligible fraction of protons and/or ions? Is it almost entirely filled or mostly empty except for some small anecdotal plasma filled regions? Answers to these questions will strongly direct the description of the magnetosphere to seemingly contradictory results leading sometimes to inconsistencies. Nevertheless, accounts are given as to the latest developments in the theory of pulsar magnetospheres and winds, the existence of a possible electrosphere and physical insight obtained from related observational signatures of multi-wavelength pulsed emission.

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Section: The Pulsar Equationsupporting

confidence: 69%

Theory of pulsar magnetosphere and wind

Pétri

2016

J. Plasma Phys.

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“…The estimate that the pulsar inclination is more than 75 degrees is in contrast to a previous estimate of 34-52 degrees (Beskin et al 1993), which was made on the assumption that the X-rays were from a hot polar cap. That assumption now seems unlikely, as the soft X-ray pulse is very similar to the one seen in 7-rays and probably originates in the magnetosphere.…”

Section: The Synchrotron Nebula Around Psr 1509-58contrasting

confidence: 53%

“…In X-rays, the emission is concentrated in linear "jets", which are interpreted as tracers of the pulsar spin axis, and an elliptical torus that is thought to be in the equatorial plane. Although the mechanisms that concentrate the emission into these features are not well understood, simple geometric models gain support from the symmetry of the Crab at optical and X-ray wavelengths (Hester et al 1995) and from the two long X-ray jets connected with the Vela pulsar (Smith & Zimmermann, 1985, Markwardt & Ogelman, 1995.…”

Section: The Synchrotron Nebula Around Psr 1509-58mentioning

confidence: 99%

The X-ray synchrotron nebula around PSR 1509-58

Brazier

1996

International Astronomical Union Colloquium

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PSR 1509-58 is one of the youngest and most powerful pulsars known and is visible not only in soft X-rays, but in gamma-rays. Observations of its supernova remnant (MSH 15-52) offer a rare chance to study such a young pulsar and to explore its surroundings, which in X-rays include the pulsar’s 10×6 arcmin X-ray synchrotron nebula and the peculiar, filamentary optical nebula, RCW 89, that sits on the limb of MSH 15-52 (Seward & Harnden 1982, Seward et al. 1983). This paper will concentrate on the morphology of the synchrotron nebula.

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“…According to Beskin, Gurevich, & Istomin (1993);Spitkovsky (2006) ;Tchekhovskoy, Philippov, & Spitkovsky (2016), the spin-down power associated with magnetic field, E mag rot , can be estimated as…”

Section: Narrow Low-temperature Stability Peaks [Model (A)]mentioning

confidence: 99%

R modes and neutron star recycling scenario

Chugunov¹,

Gusakov²,

Kantor

2017

Monthly Notices of the Royal Astronomical Society

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To put new constraints on the r-mode instability window, we analyse the formation of millisecond pulsars (MSPs) within the recycling scenario, making use of three sets of observations: (a) X-ray observations of neutron stars (NSs) in low-mass X-ray binaries; (b) timing of millisecond pulsars; and (c) X-ray and UV observations of MSPs. As shown in previous works, r-mode dissipation by shear viscosity is not sufficient to explain observational set (a), and enhanced r-mode dissipation at the red-shifted internal temperatures T ∞ ∼ 10 8 K is required to stabilize the observed NSs. Here, we argue that models with enhanced bulk viscosity can hardly lead to a self-consistent explanation of observational set (a) due to strong neutrino emission, which is typical for these models (unrealistically powerful energy source is required to keep NSs at the observed temperatures). We also demonstrate that the observational set (b) , combined with the theory of internal heating and NS cooling, provides evidence of enhanced r-mode dissipation at low temperatures, T ∞ ∼ 2×10 7 K. Observational set (c) allows us to set an upper limit on the internal temperatures of MSPs, T ∞ < 2 × 10 7 K (assuming a canonical NS with the accreted crust). Recycling scenario can produce MSPs at these temperatures only if r-mode instability is suppressed in the whole MSP spin frequency range (ν 750 Hz) at temperatures 2 × 10 7 T ∞ 3 × 10 7 K, providing thus a new constraint on the r-mode instability window. These observational constraints are analysed in more details in application to the resonance uplift scenario of Gusakov et al. (2014b,a).

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Physics of the Pulsar Magnetosphere

Cited by 135 publications

References 0 publications

Theory of pulsar magnetosphere and wind

Theory of pulsar magnetosphere and wind

The X-ray synchrotron nebula around PSR 1509-58

R modes and neutron star recycling scenario

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