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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
| Published: |
2023
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2308.08832 |
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| _version_ | 1866929495305355264 |
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| author | Wang, Pei Li, Jian Ji, Long Hou, Xian Gugercinoglu, Erbil Li, Di Torres, Diego F. Chen, Yutong Niu, Jiarui Zhu, Weiwei Zhang, Bing Liang, En-wei Zhang, Li Ge, Mingyu Dai, Zigao Lin, Lin Han, Jinlin Feng, Yi Niu, Chenhui Zhang, Yongkun Zhou, Dengjiang Xu, Heng Zhang, Chunfeng Jiang, Jinchen Miao, Chenchen Yuan, Mao Wang, Weiyang Yue, Youling Wu, Yunsheng Wang, Yabiao Wang, Chengjie Gan, Zhenye Li, Yuxi Sun, Zhongyi Chi, Mingmin |
| author_facet | Wang, Pei Li, Jian Ji, Long Hou, Xian Gugercinoglu, Erbil Li, Di Torres, Diego F. Chen, Yutong Niu, Jiarui Zhu, Weiwei Zhang, Bing Liang, En-wei Zhang, Li Ge, Mingyu Dai, Zigao Lin, Lin Han, Jinlin Feng, Yi Niu, Chenhui Zhang, Yongkun Zhou, Dengjiang Xu, Heng Zhang, Chunfeng Jiang, Jinchen Miao, Chenchen Yuan, Mao Wang, Weiyang Yue, Youling Wu, Yunsheng Wang, Yabiao Wang, Chengjie Gan, Zhenye Li, Yuxi Sun, Zhongyi Chi, Mingmin |
| contents | Magnetars are neutron stars with extremely strong magnetic fields, frequently powering high-energy activity in X-rays. Pulsed radio emission following some X-ray outbursts have been detected (\citealt{Camilo2006,camilo2007a}), albeit its physical origin is unclear. It has long been speculated that the origin of magnetars' radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154's X-ray outburst and its associated Fast Radio Burst (FRB) 20200428, a radio pulsar phase was discovered. Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2308_08832 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | X-ray hardening preceding the onset of SGR 1935+2154's radio pulsar phase Wang, Pei Li, Jian Ji, Long Hou, Xian Gugercinoglu, Erbil Li, Di Torres, Diego F. Chen, Yutong Niu, Jiarui Zhu, Weiwei Zhang, Bing Liang, En-wei Zhang, Li Ge, Mingyu Dai, Zigao Lin, Lin Han, Jinlin Feng, Yi Niu, Chenhui Zhang, Yongkun Zhou, Dengjiang Xu, Heng Zhang, Chunfeng Jiang, Jinchen Miao, Chenchen Yuan, Mao Wang, Weiyang Yue, Youling Wu, Yunsheng Wang, Yabiao Wang, Chengjie Gan, Zhenye Li, Yuxi Sun, Zhongyi Chi, Mingmin High Energy Astrophysical Phenomena Magnetars are neutron stars with extremely strong magnetic fields, frequently powering high-energy activity in X-rays. Pulsed radio emission following some X-ray outbursts have been detected (\citealt{Camilo2006,camilo2007a}), albeit its physical origin is unclear. It has long been speculated that the origin of magnetars' radio signals is different from those from canonical pulsars, although convincing evidence is still lacking. Five months after magnetar SGR 1935+2154's X-ray outburst and its associated Fast Radio Burst (FRB) 20200428, a radio pulsar phase was discovered. Here we report the discovery of X-ray spectral hardening associated with the emergence of periodic radio pulsations from SGR 1935+2154 and a detailed analysis of the properties of the radio pulses. The observations suggest that radio emission originates from the outer magnetosphere of the magnetar, and the surface heating due to the bombardment of inward-going particles from the radio emission region is responsible for the observed X-ray spectral hardening. |
| title | X-ray hardening preceding the onset of SGR 1935+2154's radio pulsar phase |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2308.08832 |