Electrohydrodynamic mechanism of plasma ejection in radio pulsars

Muslimov, A. G.; Tsygan, A. I.

doi:10.1007/bf01005968

Cited by 30 publications

(44 citation statements)

References 18 publications

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“…Recently, however, two important alterations have been made to the theory. First, the importance of general relativistic frame dragging in the creation of the accelerating potential was discovered by Muslimov & Tsygan (1990, 1992 and later elaborated by Muslimov & Harding (1997). Second, several authors (Sturner, Dermer, & Michel 1995 ;Luo 1996 ;Zhang et al 1997) have suggested that inverse Compton scattering (ICS) is an important, perhaps the dominant, high-energy photon emission mechanism, rather than the curvature radiation proposed by the earlier theories.…”

Section: Introductionmentioning

confidence: 99%

“…Given the potential, the PFF height sets the Ðnal Lorentz factor of the beam, determining the energy budget of the polar cap region. This paper calculates, in a direct analytic manner, and for an arbitrary pulsar, the height of the PFF in the presence of the Muslimov & Tsygan (1990, 1992 accelerating potential and including the e †ects of inverse Compton scattering. Qualitatively, two rates combine to position the PFF : the creation rate of photons capable of pair-producing and the rate at which those photons can pair-produce.…”

Section: Introductionmentioning

confidence: 99%

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Pair Multiplicities and Pulsar Death

Hibschman

Arons

2001

ApJ

143

154

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Through a simple model of particle acceleration and pair creation above the polar caps of rotationpowered pulsars, we calculate the height of the pair formation front (PFF) and the dominant photon emission mechanism for the pulsars in the Princeton catalog. We Ðnd that for most low-and moderateÐeld pulsars, the height of the PFF and the Ðnal Lorentz factor of the primary beam is set by nonresonant inverse Compton scattering (NRICS), in the Klein-Nishina limit. NRICS is capable of creating pairs over a wide range of pulsar parameters without invoking a magnetic Ðeld more complicated than a centered dipole, although we still require a reduced radius of curvature for most millisecond pulsars. For short-period pulsars, the dominant process is curvature radiation, while for extremely high Ðeld pulsars, it is resonant inverse Compton scattering (RICS). The dividing point between NRICS dominance and curvature dominance is very temperature dependent ; large numbers of pulsars dominated by NRICS at a stellar temperature of 106 K are dominated by curvature at 105 K. Our principle result is a new determination of the theoretical pulsar death line. Proper inclusion of ICS allows us to reach the conclusion that all known radio pulsars are consistent with pair creation above their polar caps, assuming steady acceleration of a space chargeÈlimited particle beam. We identify a new region of the diagram where P-P0 slow pulsars with narrow radiation beams should be found in sufficiently large surveys. We also show that the injection rate of electrons and positrons into the Crab Nebula inferred from the polar cap pair creation model at the present epoch (1039 electrons and positrons s~1) suffices to explain the nebular X-ray and c-ray emission, the best empirical measure of the instantaneous particle-loss rate from any pulsar, but that the contemporary injection rate is about a factor of 5 below the rate averaged over the nebulaÏs history required to explain the nebular radio emission (assuming that the nebular radio source is homogeneous). It is not clear whether this discrepancy can be resolved by evolutionary e †ects and by better treatment of nebular inhomogeneity or is an indication of another particle source in the pulsarÏs magnetosphere.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Pair Multiplicities and Pulsar Death

Hibschman

Arons

2001

ApJ

143

154

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“…The buoyancy force f B is of the order of H c 1 φ 0 /8π R ∼ 1.0 dyne cm −1 (Muslimov & Tsygan 1985; Jones 2006), where H c 1 is the superconductor lower critical field and R is the neutron‐star radius. This term can arise because the normal to superconducting transition is so fast that the superconductor is in a steady, but not necessarily complete equilibrium state.…”

Section: Application To Proton Vorticesmentioning

confidence: 99%

“…Tinkham 1996). Steady‐state motion of the proton vortices is determined by the balance of the Magnus force, electromagnetic interactions, external forces including buoyancy forces (Muslimov & Tsygan 1985; Jones 2006) and interaction with vortices of the rotating neutron superfluid (Muslimov & Tsygan 1985; Sauls 1989; Jones 1991; Ruderman, Zhu & Chen 1998), and forces derived from interactions between the quasi‐particles of the system. The distinct populations of superfluid quasi‐particles concerned are those localized in the cores of proton vortices and those delocalized in the continuum.…”

Section: Introductionmentioning

confidence: 99%

Fermion zero-mode influence on neutron-star magnetic field evolution

Jones¹

2009

Monthly Notices of the Royal Astronomical Society

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The quantum phenomenon of spectral flow which has been observed in laboratory superfluids, such as 3He-B, controls the drift velocity of proton type II superconductor vortices in the liquid core of a neutron star and so determines the rate at which magnetic flux can be expelled from the core to the crust. In the earliest and most active phases of the anomalous X-ray pulsars and soft-gamma repeaters, the rates are low and consistent with a large fraction of the active crustal flux not linking the core. If normal neutrons are present in an appreciable core matter-density interval, the spectral flow force limits flux expulsion in cases of rapid spin-down, such as in the Crab pulsar or in the propeller phase of binary systems.Comment: Additional references and extended explanation: to be published in Monthly Notices of the Royal Astronomical Societ

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“…Wind Accretion 10 −14 − 10 There is likely to be a strong inter-pinning between the proton fluxoids and the neutron vortices (Muslimov & Tsygan 1985a;Sauls 1989). In a spinning down neutron star the neutron vortices migrate outward and by virtue of inter-pinning drag the proton fluxoids along to the outer crust.…”

Section: Spin-down Induced Flux Expulsionmentioning

confidence: 99%