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The role of beam geometry in population statistics and pulse profiles of radio and gamma-ray pulsars
Astrophysics · Submitted 20 Dec 2003
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Our findings suggest that further improvements are required in describing both the radio and $\gamma$-ray geometries.
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The abstract, sentence by sentence
We present results of a pulsar population synthesis study that incorporates a number of recent developments and some significant improvements over our previous study. We have included the results of the Parkes multi-beam pulsar survey in our select group of nine radio surveys, doubling our sample of radio pulsars. We adopted with some modifications the radio beam geometry of Arzoumanian, Chernoff & Cordes (2002). For the $\gamma$-ray beam, we have assumed the slot gap geometry described in the work of Muslimov & Harding (2003). To account for the shape of the distribution of radio pulsars in the $\dot P-P$ diagram, we continue to find that decay of the magnetic field on a timescale of 2.8 Myr is needed. With all nine surveys, our model predicts that EGRET should have seen 7 radio-quiet (below the sensitivity of these radio surveys) and 19 radio-loud $\gamma$-ray pulsars. AGILE (nominal sensitivity map) is expected to detect 13 radio-quiet and 37 radio-loud $\gamma$-ray pulsars, while GLAST, with greater sensitivity is expected to detect 276 radio-quiet and 344 radio-loud $\gamma$-ray pulsars. When the Parkes multi-beam pulsar survey is excluded, the ratio of radio-loud to radio-quiet $\gamma$-ray pulsars decreases, especially for GLAST. The decrease for EGRET is 45%, implying that some fraction of EGRET unidentified sources are radio-loud $\gamma$-ray pulsars. In the radio geometry adopted, short period pulsars are core dominated. Unlike the EGRET $\gamma$-ray pulsars, our model predicts that when two $\gamma$-ray peaks appear in the pulse profile, a dominant radio core peak appears in between the $\gamma$-ray peaks. Our findings suggest that further improvements are required in describing both the radio and $\gamma$-ray geometries.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present results of a pulsar population synthesis study that incorporates a number of recent developments and some significant improvements over our previous study. | contribution 0.99 | 0.84 | 0.04 | asserted 0.95 |
| s1 | We have included the results of the Parkes multi-beam pulsar survey in our select group of nine radio surveys, doubling our sample of radio pulsars. | method 0.71 | 0.90 | 0.03 | asserted 1.00 |
| s2 | We adopted with some modifications the radio beam geometry of Arzoumanian, Chernoff & Cordes (2002). | method 0.99 | 0.69 | 0.02 | asserted 0.98 |
| s3 | For the $\gamma$-ray beam, we have assumed the slot gap geometry described in the work of Muslimov & Harding (2003). | method 0.99 | 0.54 | 0.03 | asserted 0.90 |
| s4 | To account for the shape of the distribution of radio pulsars in the $\dot P-P$ diagram, we continue to find that decay of the magnetic field on a timescale of 2.8 Myr is needed. | result 0.93 | 0.91 | 0.14 | asserted 1.00 |
| s5 | With all nine surveys, our model predicts that EGRET should have seen 7 radio-quiet (below the sensitivity of these radio surveys) and 19 radio-loud $\gamma$-ray pulsars. | result 1.00 | 0.88 | 0.12 | asserted 0.99 |
| s6 | AGILE (nominal sensitivity map) is expected to detect 13 radio-quiet and 37 radio-loud $\gamma$-ray pulsars, while GLAST, with greater sensitivity is expected to detect 276 radio-quiet and 344 radio-loud $\gamma$-ray pulsars. | result 1.00 | 0.80 | 0.10 | asserted 0.64 |
| s7 | When the Parkes multi-beam pulsar survey is excluded, the ratio of radio-loud to radio-quiet $\gamma$-ray pulsars decreases, especially for GLAST. | result 1.00 | 0.87 | 0.09 | asserted 1.00 |
| s8 | The decrease for EGRET is 45%, implying that some fraction of EGRET unidentified sources are radio-loud $\gamma$-ray pulsars. | interpretation 0.86 | 0.83 | 0.10 | hedged possibility 0.67 |
| s9 | In the radio geometry adopted, short period pulsars are core dominated. | result 0.98 | 0.52 | 0.06 | asserted 1.00 |
| s10 | Unlike the EGRET $\gamma$-ray pulsars, our model predicts that when two $\gamma$-ray peaks appear in the pulse profile, a dominant radio core peak appears in between the $\gamma$-ray peaks. | result 0.99 | 0.90 | 0.11 | asserted 0.99 |
| s11 | Our findings suggest that further improvements are required in describing both the radio and $\gamma$-ray geometries. | future work 0.69 | 0.56 | 0.36 | hedged possibility 1.00 |
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Original abstract
We present results of a pulsar population synthesis study that incorporates a number of recent developments and some significant improvements over our previous study. We have included the results of the Parkes multi-beam pulsar survey in our select group of nine radio surveys, doubling our sample of radio pulsars. We adopted with some modifications the radio beam geometry of Arzoumanian, Chernoff & Cordes (2002). For the $\gamma$-ray beam, we have assumed the slot gap geometry described in the work of Muslimov & Harding (2003). To account for the shape of the distribution of radio pulsars in the $\dot P-P$ diagram, we continue to find that decay of the magnetic field on a timescale of 2.8 Myr is needed. With all nine surveys, our model predicts that EGRET should have seen 7 radio-quiet (below the sensitivity of these radio surveys) and 19 radio-loud $\gamma$-ray pulsars. AGILE (nominal sensitivity map) is expected to detect 13 radio-quiet and 37 radio-loud $\gamma$-ray pulsars, while GLAST, with greater sensitivity is expected to detect 276 radio-quiet and 344 radio-loud $\gamma$-ray pulsars. When the Parkes multi-beam pulsar survey is excluded, the ratio of radio-loud to radio-quiet $\gamma$-ray pulsars decreases, especially for GLAST. The decrease for EGRET is 45%, implying that some fraction of EGRET unidentified sources are radio-loud $\gamma$-ray pulsars. In the radio geometry adopted, short period pulsars are core dominated. Unlike the EGRET $\gamma$-ray pulsars, our model predicts that when two $\gamma$-ray peaks appear in the pulse profile, a dominant radio core peak appears in between the $\gamma$-ray peaks. Our findings suggest that further improvements are required in describing both the radio and $\gamma$-ray geometries.
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3 arXiv papers cite this in 4 sentences
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Cites it as background 1 paper
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Population synthesis models of radio and gamma-ray pulsars (e.g. [ref] ) have been used to try to predict the number of radio-loud and radio-quiet pulsars that will be detected by the new generation of gamma-ray telescopes (AGILE and $Fermi$).
Fermi Gamma-ray Space Telescope Observations of Gamma-ray Pulsars · Introduction · 0.86
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