No Measurable Changes in Radio and X-ray Emission Surrounding Glitches in the Young Pulsar PSR J2229+6114
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| Main Authors: | , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| author | Xia, Wenke Main, Robert A. Ng, Mason Kaspi, Victoria M. Hessels, Jason W. Cassity, Alyssa Denney, Abigail K. Fonseca, Emmanuel Good, Deborah C. Kumar, Ajay Kunkel, Lars Meyers, Bradley W. Pearlman, Aaron B. Stairs, Ingrid |
| author_facet | Xia, Wenke Main, Robert A. Ng, Mason Kaspi, Victoria M. Hessels, Jason W. Cassity, Alyssa Denney, Abigail K. Fonseca, Emmanuel Good, Deborah C. Kumar, Ajay Kunkel, Lars Meyers, Bradley W. Pearlman, Aaron B. Stairs, Ingrid |
| contents | We present our first result from an ongoing pulsar glitch monitoring campaign at the Canadian Hydrogen Intensity Mapping Experiment (CHIME), in which we analyzed the radio and X-ray emission surrounding four glitches in PSR J2229+6114. Using daily CHIME observations, we detected a glitch in PSR J2229+6114 in near-real time and triggered an X-ray follow-up with NuSTAR two days after the glitch. We identified three additional glitch events in archival CHIME/Pulsar observations that coincided with an independent X-ray observing campaign with NICER. Our data show no measurable changes in the source's X-ray and radio emission during the four glitch events, in stark contrast to the post-glitch activity in high-magnetic-field, rotation-powered pulsars (RPPs), which have been observed to exhibit magnetar-like X-ray outbursts immediately after large glitches. Those high-magnetic-field (high-B) RPPs are considered transitional objects between ordinary RPPs and magnetars, thereby leading to a unifying neutron star model in which the inferred dipolar surface magnetic field strength serves as a unifying parameter. However, such a model remains challenged, in part, by the lack of constraints near the low-B end of the high-B regime, and our result provides additional evidence that magnetar-like post-glitch activity is likely more common among high-B RPPs. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2605_13011 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | No Measurable Changes in Radio and X-ray Emission Surrounding Glitches in the Young Pulsar PSR J2229+6114 Xia, Wenke Main, Robert A. Ng, Mason Kaspi, Victoria M. Hessels, Jason W. Cassity, Alyssa Denney, Abigail K. Fonseca, Emmanuel Good, Deborah C. Kumar, Ajay Kunkel, Lars Meyers, Bradley W. Pearlman, Aaron B. Stairs, Ingrid High Energy Astrophysical Phenomena We present our first result from an ongoing pulsar glitch monitoring campaign at the Canadian Hydrogen Intensity Mapping Experiment (CHIME), in which we analyzed the radio and X-ray emission surrounding four glitches in PSR J2229+6114. Using daily CHIME observations, we detected a glitch in PSR J2229+6114 in near-real time and triggered an X-ray follow-up with NuSTAR two days after the glitch. We identified three additional glitch events in archival CHIME/Pulsar observations that coincided with an independent X-ray observing campaign with NICER. Our data show no measurable changes in the source's X-ray and radio emission during the four glitch events, in stark contrast to the post-glitch activity in high-magnetic-field, rotation-powered pulsars (RPPs), which have been observed to exhibit magnetar-like X-ray outbursts immediately after large glitches. Those high-magnetic-field (high-B) RPPs are considered transitional objects between ordinary RPPs and magnetars, thereby leading to a unifying neutron star model in which the inferred dipolar surface magnetic field strength serves as a unifying parameter. However, such a model remains challenged, in part, by the lack of constraints near the low-B end of the high-B regime, and our result provides additional evidence that magnetar-like post-glitch activity is likely more common among high-B RPPs. |
| title | No Measurable Changes in Radio and X-ray Emission Surrounding Glitches in the Young Pulsar PSR J2229+6114 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2605.13011 |