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On the beam properties of radio pulsars with interpulse emission
High Energy Astrophysical Phenomena · Submitted 8 Oct 2019
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We show substantial evidence that the emission heights are larger at the beam edges than in the beam centre.
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The abstract, sentence by sentence
In the canonical picture of pulsars, radio emission arises from a narrow cone centered on the star's magnetic axis but many basic details remain unclear. We use high-quality polarization data taken with the Parkes radio telescope to constrain the geometry and emission heights of pulsars showing interpulse emission, and include the possibility that emission heights in the main and interpulse may be different. We show that emission heights are low in the centre of the beam, typically less than 3\% of the light cylinder radius. The emission beams are under-filled in longitude, with an average profile width only 60% of the maximal beam width and there is a strong preference for the visible emission to be located on the trailing part of the beam. We show substantial evidence that the emission heights are larger at the beam edges than in the beam centre. There is some indication that a fan-like emission beam explains the data better than conal structures. Finally, there is a strong correlation between handedness of circular polarization in the main and interpulse profiles which implies that the hand of circular polarization is determined by the hemisphere of the visible emission.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | In the canonical picture of pulsars, radio emission arises from a narrow cone centered on the star's magnetic axis but many basic details remain unclear. | background 0.96 | 0.04 | 0.02 | asserted 0.99 |
| s1 | We use high-quality polarization data taken with the Parkes radio telescope to constrain the geometry and emission heights of pulsars showing interpulse emission, and include the possibility that emission heights in the main and interpulse may be different. | method 0.76 | 0.96 | 0.05 | asserted 0.69 |
| s2 | We show that emission heights are low in the centre of the beam, typically less than 3\% of the light cylinder radius. | result 1.00 | 0.94 | 0.23 | asserted 1.00 |
| s3 | The emission beams are under-filled in longitude, with an average profile width only 60% of the maximal beam width and there is a strong preference for the visible emission to be located on the trailing part of the beam. | result 1.00 | 0.94 | 0.17 | asserted 1.00 |
| s4 | We show substantial evidence that the emission heights are larger at the beam edges than in the beam centre. | result 1.00 | 0.95 | 0.18 | asserted 0.96 |
| s5 | There is some indication that a fan-like emission beam explains the data better than conal structures. | result 0.66 | 0.89 | 0.10 | hedged possibility 0.99 |
| s6 | Finally, there is a strong correlation between handedness of circular polarization in the main and interpulse profiles which implies that the hand of circular polarization is determined by the hemisphere of the visible emission. | interpretation 0.53 | 0.90 | 0.19 | asserted 0.89 |
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The paper
Original abstract
In the canonical picture of pulsars, radio emission arises from a narrow cone centered on the star's magnetic axis but many basic details remain unclear. We use high-quality polarization data taken with the Parkes radio telescope to constrain the geometry and emission heights of pulsars showing interpulse emission, and include the possibility that emission heights in the main and interpulse may be different. We show that emission heights are low in the centre of the beam, typically less than 3\% of the light cylinder radius. The emission beams are under-filled in longitude, with an average profile width only 60% of the maximal beam width and there is a strong preference for the visible emission to be located on the trailing part of the beam. We show substantial evidence that the emission heights are larger at the beam edges than in the beam centre. There is some indication that a fan-like emission beam explains the data better than conal structures. Finally, there is a strong correlation between handedness of circular polarization in the main and interpulse profiles which implies that the hand of circular polarization is determined by the hemisphere of the visible emission.
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References
How the literature uses it
2 arXiv papers cite this in 6 sentences
Papers citing it · 3 sentences without a confident label
Uses its data or values 1 paper
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Note that for Figs. [ref] and [ref] the values of $r_s$, $α$, $ε$ and $ω$ have been taken from Ref. [ref] , whereas the values of $ψ$, $σ_ϕ$, $ϕ_o$, $τ$, $λ$ and $γ$ have been chosen such that our theoretical plots match best with observational plots in Figs. <ref> and [ref].
General relativistic effects on pulsar radiation · Pulse Profiles · 0.97
Cites it as background 1 paper
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Previous studies on interpulse pulsars have focused on population properties and beam evolution [ref] , as well as on the beam structure and emission regions [ref] .
On the Difference Between Pulsar Radio Emission Beams from the Two Poles · Introduction · 0.98
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