A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST
We report on a single-pulse study of PSR J1239+0326 discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in the Commensal Radio Astronomy FAST Survey. The observations were conducted at a central frequency of 1.25 GHz. The integrated pulse profile of PSR J1239+0326 shows fo...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adc576 |
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| author | R. Rejep W. W. Zhu N. Wang W. M. Yan J. P. Yuan M. Kramer L. Q. Meng E. Gügercinoğlu M. Yuan W. Y. Wang Z. W. Wu Q. D. Wu D. Zhao S. Q. Wang H. M. Tedila S. J. Dang M. Y. Xue P. Wang The FAST Collaboration |
| author_facet | R. Rejep W. W. Zhu N. Wang W. M. Yan J. P. Yuan M. Kramer L. Q. Meng E. Gügercinoğlu M. Yuan W. Y. Wang Z. W. Wu Q. D. Wu D. Zhao S. Q. Wang H. M. Tedila S. J. Dang M. Y. Xue P. Wang The FAST Collaboration |
| author_sort | R. Rejep |
| collection | DOAJ |
| description | We report on a single-pulse study of PSR J1239+0326 discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in the Commensal Radio Astronomy FAST Survey. The observations were conducted at a central frequency of 1.25 GHz. The integrated pulse profile of PSR J1239+0326 shows four distinct components, implying a central line of sight traversing a presumed double cone core emission beam. We found correlations between intensities of the first and fourth components and the second and the core components, indicating that the charges emitted between the correlated components may be related. Based on rotating vector model fitting, we estimated the inclination angle between the magnetic and the rotational axes to be 10°. No nulls, giant pulses, or giant micropulses were detected during observation sessions. Outer-cone components are observed to display “even-odd” subpulse modulation with quasiperiodicity around 2 P , where P is the rotational period of the pulsar. The trailing component exhibits energy modulation with quasiperiodicities of 19 P and 26 P . This two-mode modulation could result from the combination of sub-pulse drifts and the feedback between the voltage difference across the polar gap and surface thermal emission by backflowing charges. |
| format | Article |
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| institution | OA Journals |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-98d7a345599642be8f2076f035d045a32025-08-20T01:51:04ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198511110.3847/1538-4357/adc576A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FASTR. Rejep0W. W. Zhu1https://orcid.org/0000-0001-5105-4058N. Wang2https://orcid.org/0000-0002-9786-8548W. M. Yan3https://orcid.org/0000-0002-7662-3875J. P. Yuan4https://orcid.org/0000-0002-5381-6498M. Kramer5https://orcid.org/0000-0002-4175-2271L. Q. Meng6https://orcid.org/0000-0002-2885-568XE. Gügercinoğlu7M. Yuan8https://orcid.org/0000-0003-1874-0800W. Y. Wang9https://orcid.org/0000-0001-9036-8543Z. W. Wu10https://orcid.org/0000-0002-1381-7859Q. D. Wu11D. Zhao12https://orcid.org/0009-0007-8062-1454S. Q. Wang13https://orcid.org/0000-0003-4498-6070H. M. Tedila14https://orcid.org/0000-0002-5815-6548S. J. Dang15https://orcid.org/0000-0002-2060-5539M. Y. Xue16https://orcid.org/0000-0001-8018-1830P. Wang17https://orcid.org/0000-0002-3386-7159The FAST CollaborationNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cnNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cn; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of ChinaMax-Planck-Institut für Radioastronomie , Auf dem Hügel 69, D-53121 Bonn, GermanyNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cnNational Space Science Center, Chinese Academy of Sciences , Beijing 100190, People’s Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cnXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cnXinjiang Astronomical Observatory, Chinese Academy of Sciences , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of China ; na.wang@xao.ac.cn; Key Laboratory of Radio Astronomy, Chinese Academy of Sciences , Urumqi, Xinjiang 830011, People’s Republic of China; Xinjiang Key Laboratory of Radio Astrophysics , 150 Science 1-Street, Urumqi, Xinjiang 830011, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cn; Arba Minch University , Arba Minch 21, EthiopiaSchool of Physics and Electronic Science, Guizhou Normal University , Guiyang 550001, People’s Republic of China; Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing, Guizhou Normal University , Guiyang 550001, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cnNational Astronomical Observatories, Chinese Academy of Sciences , A20 Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China ; zhuww@nao.cas.cnWe report on a single-pulse study of PSR J1239+0326 discovered by the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in the Commensal Radio Astronomy FAST Survey. The observations were conducted at a central frequency of 1.25 GHz. The integrated pulse profile of PSR J1239+0326 shows four distinct components, implying a central line of sight traversing a presumed double cone core emission beam. We found correlations between intensities of the first and fourth components and the second and the core components, indicating that the charges emitted between the correlated components may be related. Based on rotating vector model fitting, we estimated the inclination angle between the magnetic and the rotational axes to be 10°. No nulls, giant pulses, or giant micropulses were detected during observation sessions. Outer-cone components are observed to display “even-odd” subpulse modulation with quasiperiodicity around 2 P , where P is the rotational period of the pulsar. The trailing component exhibits energy modulation with quasiperiodicities of 19 P and 26 P . This two-mode modulation could result from the combination of sub-pulse drifts and the feedback between the voltage difference across the polar gap and surface thermal emission by backflowing charges.https://doi.org/10.3847/1538-4357/adc576Pulsars |
| spellingShingle | R. Rejep W. W. Zhu N. Wang W. M. Yan J. P. Yuan M. Kramer L. Q. Meng E. Gügercinoğlu M. Yuan W. Y. Wang Z. W. Wu Q. D. Wu D. Zhao S. Q. Wang H. M. Tedila S. J. Dang M. Y. Xue P. Wang The FAST Collaboration A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST The Astrophysical Journal Pulsars |
| title | A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST |
| title_full | A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST |
| title_fullStr | A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST |
| title_full_unstemmed | A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST |
| title_short | A Detailed Single-pulse Study of Four-component Pulsar PSR J1239+0326 Discovered by FAST |
| title_sort | detailed single pulse study of four component pulsar psr j1239 0326 discovered by fast |
| topic | Pulsars |
| url | https://doi.org/10.3847/1538-4357/adc576 |
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