An empirical model for the beams of radio pulsars
Motivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arise...
| Hoofdauteurs: | , |
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| Formaat: | Journal article |
| Taal: | English |
| Gepubliceerd in: |
2007
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| _version_ | 1826257548906332160 |
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| author | Karastergiou, A Johnston, S |
| author_facet | Karastergiou, A Johnston, S |
| author_sort | Karastergiou, A |
| collection | OXFORD |
| description | Motivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short-period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations. © 2007 RAS. |
| first_indexed | 2024-03-06T18:19:58Z |
| format | Journal article |
| id | oxford-uuid:05f10d01-2d4c-4faf-95fb-c459a74ef06b |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T18:19:58Z |
| publishDate | 2007 |
| record_format | dspace |
| spelling | oxford-uuid:05f10d01-2d4c-4faf-95fb-c459a74ef06b2022-03-26T08:59:56ZAn empirical model for the beams of radio pulsarsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:05f10d01-2d4c-4faf-95fb-c459a74ef06bEnglishSymplectic Elements at Oxford2007Karastergiou, AJohnston, SMotivated by recent results on the location of the radio emission in pulsar magnetospheres, we have developed a model which can account for the large diversity found in the average profile shapes of pulsars. At the centre of our model lies the idea that radio emission at a particular frequency arises from a wide range of altitudes above the surface of the star, and that it is confined to a region close to the last open field lines. We assert that the radial height range over which emission occurs is responsible for the complex average pulse shapes rather than the transverse (longitudinal) range proposed in most current models. By implementing an abrupt change in the height range to discriminate between young, short-period, highly energetic pulsars and their older counterparts, we obtain the observed transition between the simple and complex average pulse profiles observed in each group respectively. Monte Carlo simulations are used to demonstrate the match of our model to real observations. © 2007 RAS. |
| spellingShingle | Karastergiou, A Johnston, S An empirical model for the beams of radio pulsars |
| title | An empirical model for the beams of radio pulsars |
| title_full | An empirical model for the beams of radio pulsars |
| title_fullStr | An empirical model for the beams of radio pulsars |
| title_full_unstemmed | An empirical model for the beams of radio pulsars |
| title_short | An empirical model for the beams of radio pulsars |
| title_sort | empirical model for the beams of radio pulsars |
| work_keys_str_mv | AT karastergioua anempiricalmodelforthebeamsofradiopulsars AT johnstons anempiricalmodelforthebeamsofradiopulsars AT karastergioua empiricalmodelforthebeamsofradiopulsars AT johnstons empiricalmodelforthebeamsofradiopulsars |