The Variability of Persistent Radio Sources of Fast Radio Bursts
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arXiv
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| Auteurs principaux: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866913509505236992 |
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| author | Yang, Ai Yuan Feng, Yi Tsai, Chao-Wei Li, Di Shi, Hui Wang, Pei Yang, Yuan-Pei Zhang, Yong-Kun Niu, Chen-Hui Yao, Ju-Mei Cui, Yu-Zhu Su, Ren-Zhi Li, Xiao-Feng Zhang, Jun-Shuo Zhu, Yu-Hao Cotton, W. D. |
| author_facet | Yang, Ai Yuan Feng, Yi Tsai, Chao-Wei Li, Di Shi, Hui Wang, Pei Yang, Yuan-Pei Zhang, Yong-Kun Niu, Chen-Hui Yao, Ju-Mei Cui, Yu-Zhu Su, Ren-Zhi Li, Xiao-Feng Zhang, Jun-Shuo Zhu, Yu-Hao Cotton, W. D. |
| contents | Over 700 bright millisecond-duration radio transients, known as Fast Radio Bursts (FRBs), have been identified to date. Nevertheless, the origin of FRBs remains unknown. The two repeating FRBs (FRB 20121102A and FRB 20190520B) have been verified to be associated with persistent radio sources (PRSs), making them the best candidates to study the nature of FRBs. Monitoring the variability in PRSs is essential for understanding their physical nature. We conducted 22 observations of the PRSs linked to FRB 20121102A and FRB 20190520B using the Karl G. Jansky Very Large Array (VLA), to study their variability. We have observed significant flux variability for the PRSs of FRB 20121102A and FRB 20190520B, with a confidence level exceeding 99.99%, based on the observations covering the longest timescale recorded to date. The observed variability of the two PRSs exhibits no significant difference in amplitude across both short and long timescales. We found that the radio-derived star formation rates of the two FRB hosts are significantly higher than those measured by the optical $H_α$ emissions, indicating that their host galaxies are highly obscured or most radio emissions are not from star formation processes. The observed timescale of PRS flux evolution constrained the magnetic field of FRB 20121102A with $B_\parallel\gtrsim1~{\rm mG}$ and FRB 20190520B with $B_\parallel\gtrsim0.1~{\rm mG}$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2409_13170 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Variability of Persistent Radio Sources of Fast Radio Bursts Yang, Ai Yuan Feng, Yi Tsai, Chao-Wei Li, Di Shi, Hui Wang, Pei Yang, Yuan-Pei Zhang, Yong-Kun Niu, Chen-Hui Yao, Ju-Mei Cui, Yu-Zhu Su, Ren-Zhi Li, Xiao-Feng Zhang, Jun-Shuo Zhu, Yu-Hao Cotton, W. D. High Energy Astrophysical Phenomena Astrophysics of Galaxies Over 700 bright millisecond-duration radio transients, known as Fast Radio Bursts (FRBs), have been identified to date. Nevertheless, the origin of FRBs remains unknown. The two repeating FRBs (FRB 20121102A and FRB 20190520B) have been verified to be associated with persistent radio sources (PRSs), making them the best candidates to study the nature of FRBs. Monitoring the variability in PRSs is essential for understanding their physical nature. We conducted 22 observations of the PRSs linked to FRB 20121102A and FRB 20190520B using the Karl G. Jansky Very Large Array (VLA), to study their variability. We have observed significant flux variability for the PRSs of FRB 20121102A and FRB 20190520B, with a confidence level exceeding 99.99%, based on the observations covering the longest timescale recorded to date. The observed variability of the two PRSs exhibits no significant difference in amplitude across both short and long timescales. We found that the radio-derived star formation rates of the two FRB hosts are significantly higher than those measured by the optical $H_α$ emissions, indicating that their host galaxies are highly obscured or most radio emissions are not from star formation processes. The observed timescale of PRS flux evolution constrained the magnetic field of FRB 20121102A with $B_\parallel\gtrsim1~{\rm mG}$ and FRB 20190520B with $B_\parallel\gtrsim0.1~{\rm mG}$. |
| title | The Variability of Persistent Radio Sources of Fast Radio Bursts |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2409.13170 |