The timing and spectral properties of the 2022 outburst of SGR J1935+2154 observed with NICER
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arXiv
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| Auteurs principaux: | , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866929673784524800 |
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| author | Yu-Cong, Fu Lin, Lin Ming-Yu, Ge Teruaki, Enoto Chin-Ping, Hu George, Younes Ersin, Göğüş Christian, Malacaria |
| author_facet | Yu-Cong, Fu Lin, Lin Ming-Yu, Ge Teruaki, Enoto Chin-Ping, Hu George, Younes Ersin, Göğüş Christian, Malacaria |
| contents | The magnetar SGR J1935+2154 entered a new active episode on October 10, 2022, with X-ray bursts and enhanced persistent emission. At the tail of high burst rate interval, lasting several hours, radio bursts were detected, revealing the connection between the X-ray activities and radio emissions. We analyzed observations of SGR J1935+2154 for nearly three months, using data from Neutron Star Interior Composition Explorer (NICER). We report the timing and spectral results following the onset of this outburst. In general, the X-ray flux of the persistent emission decays exponentially. While a flare is evident on the light curve, a fast radio burst (FRB) was detected immediately following the peak of this flare. We found a phase jump of pulse profile, with a deviation of $0.16\pm0.03$ phase, which is related to the glitch. The spectra are well fit with the combination of a blackbody and a power law model. The decay of the outburst is dominated by the drop of the non-thermal component, which also leads to the increase of thermal proportion. The photon index of the power law is inversely correlated with both the unabsorbed flux and the burst rate. We find that unlike the large variety of the persistent emission around FRB 221014, the X-ray properties are very stable when FRBs 221021 and 221201 happened. These results manifest the connection between glitch, phase jump, X-ray burst, and radio burst, crucial for studying the mutation in twisted magnetic fields and constraining the trigger mechanism of radio bursts. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2501_07049 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The timing and spectral properties of the 2022 outburst of SGR J1935+2154 observed with NICER Yu-Cong, Fu Lin, Lin Ming-Yu, Ge Teruaki, Enoto Chin-Ping, Hu George, Younes Ersin, Göğüş Christian, Malacaria High Energy Astrophysical Phenomena The magnetar SGR J1935+2154 entered a new active episode on October 10, 2022, with X-ray bursts and enhanced persistent emission. At the tail of high burst rate interval, lasting several hours, radio bursts were detected, revealing the connection between the X-ray activities and radio emissions. We analyzed observations of SGR J1935+2154 for nearly three months, using data from Neutron Star Interior Composition Explorer (NICER). We report the timing and spectral results following the onset of this outburst. In general, the X-ray flux of the persistent emission decays exponentially. While a flare is evident on the light curve, a fast radio burst (FRB) was detected immediately following the peak of this flare. We found a phase jump of pulse profile, with a deviation of $0.16\pm0.03$ phase, which is related to the glitch. The spectra are well fit with the combination of a blackbody and a power law model. The decay of the outburst is dominated by the drop of the non-thermal component, which also leads to the increase of thermal proportion. The photon index of the power law is inversely correlated with both the unabsorbed flux and the burst rate. We find that unlike the large variety of the persistent emission around FRB 221014, the X-ray properties are very stable when FRBs 221021 and 221201 happened. These results manifest the connection between glitch, phase jump, X-ray burst, and radio burst, crucial for studying the mutation in twisted magnetic fields and constraining the trigger mechanism of radio bursts. |
| title | The timing and spectral properties of the 2022 outburst of SGR J1935+2154 observed with NICER |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2501.07049 |