Profile Variation in PSR B0355+54 over a Narrow Frequency Range
We investigate changes in the shape of the averaged pulse profile in PSR B0355+54 (PSR J0358+5413) based on data obtained at the center frequency of 1250 MHz using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Our dataset consists of 12 non-consecutive observations, each lasting...
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2024-11-01
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| author | Shibo Jiang Lin Li Rai Yuen Jianping Yuan Jumei Yao Xun Shi Yonghua Xu Jianling Chen Zhigang Wen |
| author_facet | Shibo Jiang Lin Li Rai Yuen Jianping Yuan Jumei Yao Xun Shi Yonghua Xu Jianling Chen Zhigang Wen |
| author_sort | Shibo Jiang |
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| description | We investigate changes in the shape of the averaged pulse profile in PSR B0355+54 (PSR J0358+5413) based on data obtained at the center frequency of 1250 MHz using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Our dataset consists of 12 non-consecutive observations, each lasting between 1 and 2 h. Considerable variation is observed in the averaged profiles across the observations even though each is folded from thousands of single pulses. Changes in the profile are measured through the ratio (<i>R</i>) between the peak intensities of the leading and trailing components. We find that the averaged pulse profile exhibits significant variation across observations, but distinctive from typical profile mode-changing. By dividing the frequency bandwidth into eight sub-bands, we demonstrate that the shape of the averaged profile undergoes significant evolution with frequency. In general, the changes in <i>R</i> across the sub-bands are different in different observations, but its value is uniform at low frequencies implying a more consistent emission. We demonstrate that the profile stabilization timescale for this pulsar is much longer than commonly suggested for ordinary pulsars, which is likely due to non-uniform and varying arrangement of the emission sources in the emission region. |
| format | Article |
| id | doaj-art-5bf6eb78d05244068de4fdaa227cf78e |
| institution | OA Journals |
| issn | 2218-1997 |
| language | English |
| publishDate | 2024-11-01 |
| publisher | MDPI AG |
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| series | Universe |
| spelling | doaj-art-5bf6eb78d05244068de4fdaa227cf78e2025-08-20T01:54:04ZengMDPI AGUniverse2218-19972024-11-01101141610.3390/universe10110416Profile Variation in PSR B0355+54 over a Narrow Frequency RangeShibo Jiang0Lin Li1Rai Yuen2Jianping Yuan3Jumei Yao4Xun Shi5Yonghua Xu6Jianling Chen7Zhigang Wen8School of Physical Science and Technology, Xinjiang University, Urumqi 830046, ChinaSchool of Physical Science and Technology, Xinjiang University, Urumqi 830046, ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 830011, ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 830011, ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 830011, ChinaSouth-Western Institute for Astronomy Research (SWIFAR), Yunnan University, Kunming 650500, ChinaYunnan Observatories, Chinese Academy of Sciences, Kunming 650011, ChinaDepartment of Physics & Electronic Engineering, Yuncheng University, Yuncheng 044000, ChinaXinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 830011, ChinaWe investigate changes in the shape of the averaged pulse profile in PSR B0355+54 (PSR J0358+5413) based on data obtained at the center frequency of 1250 MHz using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Our dataset consists of 12 non-consecutive observations, each lasting between 1 and 2 h. Considerable variation is observed in the averaged profiles across the observations even though each is folded from thousands of single pulses. Changes in the profile are measured through the ratio (<i>R</i>) between the peak intensities of the leading and trailing components. We find that the averaged pulse profile exhibits significant variation across observations, but distinctive from typical profile mode-changing. By dividing the frequency bandwidth into eight sub-bands, we demonstrate that the shape of the averaged profile undergoes significant evolution with frequency. In general, the changes in <i>R</i> across the sub-bands are different in different observations, but its value is uniform at low frequencies implying a more consistent emission. We demonstrate that the profile stabilization timescale for this pulsar is much longer than commonly suggested for ordinary pulsars, which is likely due to non-uniform and varying arrangement of the emission sources in the emission region.https://www.mdpi.com/2218-1997/10/11/416pulsarsgeneral-starsneutron-radiation mechanismsnon-thermalmulti-frequencyPSR B0355+54 (PSR J0358+5413) |
| spellingShingle | Shibo Jiang Lin Li Rai Yuen Jianping Yuan Jumei Yao Xun Shi Yonghua Xu Jianling Chen Zhigang Wen Profile Variation in PSR B0355+54 over a Narrow Frequency Range Universe pulsars general-stars neutron-radiation mechanisms non-thermal multi-frequency PSR B0355+54 (PSR J0358+5413) |
| title | Profile Variation in PSR B0355+54 over a Narrow Frequency Range |
| title_full | Profile Variation in PSR B0355+54 over a Narrow Frequency Range |
| title_fullStr | Profile Variation in PSR B0355+54 over a Narrow Frequency Range |
| title_full_unstemmed | Profile Variation in PSR B0355+54 over a Narrow Frequency Range |
| title_short | Profile Variation in PSR B0355+54 over a Narrow Frequency Range |
| title_sort | profile variation in psr b0355 54 over a narrow frequency range |
| topic | pulsars general-stars neutron-radiation mechanisms non-thermal multi-frequency PSR B0355+54 (PSR J0358+5413) |
| url | https://www.mdpi.com/2218-1997/10/11/416 |
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