Ion–proton pulsars: Table 1.

Jones, P. B.

doi:10.1093/mnras/stw818

Cited by 27 publications

(47 citation statements)

References 48 publications

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“…These authors also propose that its source is at low altitude. Such circular polarization is an unambiguous indicator of emission from an ion-proton plasma (Jones 2016) and is consistent with their conclusion.…”

Section: Optical and Soft X-ray Emissionsupporting

confidence: 89%

“…The implications and conclusions reached follow from the following basis: that neutron stars which are sources of radio emission with the almost universal large negative spectral index are those with polar-cap Ω · Bs < 0 and an ion-proton ⋆ E-mail: p.jones1@physics.ox.ac.uk plasma. Observational and other evidence for this conclusion has been summarized previously (Jones 2016) and we believe it to be strong.…”

Section: Introductionsupporting

confidence: 73%

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Dark neutron stars

Jones¹

2017

Monthly Notices of the Royal Astronomical Society

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There is good evidence that electron-positron pair formation is not present in that section of the pulsar open magnetosphere which is the source of coherent radio emission, but the possibility of two-photon pair creation in an outer gap remains. Calculation of transition rates for this process based on measured whole-surface temperatures, combined with a survey of γ-ray, X-ray and optical luminosities, expressed per primary beam lepton, shows that few Fermi LAT pulsars have significant outergap pair creation. For radio-loud pulsars with positive polar-cap corotational charge density and an ion-proton plasma there must be an outward flow of electrons from some other part of the magnetosphere to maintain a constant net charge on the star. In the absence of pair creation, it is likely that this current is the source of GeV γemission observed by the Fermi LAT and its origin is in the region of the outer gap. With negative polar-cap corotational charge density, the compensating current in the absence of pair creation can consist only of ions or protons. These neutron stars are likely to be radio-quiet, have no observable γ-emission, and hence can be described as dark neutron stars.

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Section: Optical and Soft X-ray Emissionsupporting

confidence: 89%

Section: Introductionsupporting

confidence: 73%

Dark neutron stars

Jones¹

2017

Monthly Notices of the Royal Astronomical Society

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“…Regions of polar cap emitting only protons produce no unstable mode and no coherent radio emission. We refer to Jones (2016b) and papers cited therein for more complete details of this work.…”

Section: The Ion-proton Plasmamentioning

confidence: 99%

Radio-frequency microstructure and polarization in ion–proton pulsars

Jones¹

2017

Monthly Notices of the Royal Astronomical Society

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It is shown that the time-variability inherent in the ion-proton polar cap leads naturally to growth of Langmuir modes on narrow bundles of magnetic flux lines and that the observed size of micropulses is consistent with the smallest such bundle that can plausibly support the growth of the modes. The polarization of integrated pulse profiles is revisited, specifically, the π/2 position-angle jumps that are frequently observed accompanied by a zero in polarization. The fact that radiation emitted above ion-proton polar caps is not tangential to the local flux lines but has a finite angular distribution proves to be the essence of understanding this phenomenon as is a constraint on the shape of the polar cap. In principle, the behaviour should also be seen if the form of the polar-cap ion-proton area in a single pulse satisfies certain conditions which are explained here.

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“…The present paper describes a model polar cap based on these physical processes which have been examined in a number of previous papers (see Jones 2016a for a summary). The construction of a model polar cap based on precisely defined physical processes was not attempted in those papers and its lack is the motivation for this work.…”

Section: Introductionmentioning

confidence: 99%

A model of an ion-proton radio pulsar polar cap

Jones

2019

Monthly Notices of the Royal Astronomical Society

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A number of previous papers have developed an ion-proton theory of the pulsar polar cap. The basic equations summarizing this are given here with the results of sets of model step-to-step calculations of pulse-precursor profiles. The nature of step-tostep profile variations is described by calculated phase-resolved modulation indices.The conditions under which nulls are present in step sequences are analysed. The change of mean null length with neutron-star surface temperature shows a pathway ending in emission similar to the Rotating Radio Transients. The model accommodates exceptional pulsars, the millisecond pulsars (in principle), and the 8.5 s period PSR J2144-3933. These are considered separately and their emission mechanism discussed in some detail.

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Ion–proton pulsars: Table 1.

Cited by 27 publications

References 48 publications

Dark neutron stars

Dark neutron stars

Radio-frequency microstructure and polarization in ion–proton pulsars

A model of an ion-proton radio pulsar polar cap

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