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| Natura: | Preprint |
| Pubblicazione: |
2026
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| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2601.09691 |
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| _version_ | 1866908765477928960 |
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| author | Stum, Sébastien Le Cangemi, Floriane Coleiro, Alexis Guillot, Sébastien Chenevez, Jérôme Bacon, Philippe Bellemont, Nicolas Bouchet, Laurent Bouchet, Tristan Cavet, Cécile Cordier, Bertrand Foisseau, Antoine Godet, Olivier Goldwurm, Andrea Han, Xu-Hui Lachaud, Cyril Li, Zhaosheng Li, Hua-Li Qiu, Yu-Lei Rodriguez, Jérôme Tan, Wen-Jun Tao, L. Verwaerde, Lauryne Wang, Chen-Wei Wang, Jing Wei, Jianyan Wu, Chao Xie, Wen-Jin Xin, Li-Ping Xiong, Shaolin Zhang, Shuang-Nan Zheng, S. J. |
| author_facet | Stum, Sébastien Le Cangemi, Floriane Coleiro, Alexis Guillot, Sébastien Chenevez, Jérôme Bacon, Philippe Bellemont, Nicolas Bouchet, Laurent Bouchet, Tristan Cavet, Cécile Cordier, Bertrand Foisseau, Antoine Godet, Olivier Goldwurm, Andrea Han, Xu-Hui Lachaud, Cyril Li, Zhaosheng Li, Hua-Li Qiu, Yu-Lei Rodriguez, Jérôme Tan, Wen-Jun Tao, L. Verwaerde, Lauryne Wang, Chen-Wei Wang, Jing Wei, Jianyan Wu, Chao Xie, Wen-Jin Xin, Li-Ping Xiong, Shaolin Zhang, Shuang-Nan Zheng, S. J. |
| contents | On 2025 January 10, a thermonuclear (Type I) X-ray burst from the neutron star low-mass X-ray binary \textit{4U~0614+091} was detected with the ECLAIRs instrument on board the \textit{SVOM} mission. We present here a time-resolved spectroscopic analysis of the burst, along with the detection of burst oscillations within a 51-second interval during the decay phase. The oscillation frequency is measured to be $ν= 413.674 \pm 0.002\,\mathrm{Hz}$, consistent with previous reports. However, we detect a significant downward frequency drift over the burst duration, characterized by $\dotν = (-4.7 \pm 0.3) \times 10^{-3}\,\mathrm{Hz\,s^{-1}}$. This frequency evolution is atypical compared to those observed in similar burst oscillation sources. We tentatively attribute the observed drift to a Doppler shift induced by orbital motion. Under this interpretation, the inferred orbital period must be shorter than 20 minutes, placing \textit{4U~0614+091} among the most compact known low-mass X-ray binaries. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2601_09691 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Detection of Oscillations in a Type I X-Ray Burst of 4U 0614+091 with SVOM/ECLAIRs Stum, Sébastien Le Cangemi, Floriane Coleiro, Alexis Guillot, Sébastien Chenevez, Jérôme Bacon, Philippe Bellemont, Nicolas Bouchet, Laurent Bouchet, Tristan Cavet, Cécile Cordier, Bertrand Foisseau, Antoine Godet, Olivier Goldwurm, Andrea Han, Xu-Hui Lachaud, Cyril Li, Zhaosheng Li, Hua-Li Qiu, Yu-Lei Rodriguez, Jérôme Tan, Wen-Jun Tao, L. Verwaerde, Lauryne Wang, Chen-Wei Wang, Jing Wei, Jianyan Wu, Chao Xie, Wen-Jin Xin, Li-Ping Xiong, Shaolin Zhang, Shuang-Nan Zheng, S. J. High Energy Astrophysical Phenomena On 2025 January 10, a thermonuclear (Type I) X-ray burst from the neutron star low-mass X-ray binary \textit{4U~0614+091} was detected with the ECLAIRs instrument on board the \textit{SVOM} mission. We present here a time-resolved spectroscopic analysis of the burst, along with the detection of burst oscillations within a 51-second interval during the decay phase. The oscillation frequency is measured to be $ν= 413.674 \pm 0.002\,\mathrm{Hz}$, consistent with previous reports. However, we detect a significant downward frequency drift over the burst duration, characterized by $\dotν = (-4.7 \pm 0.3) \times 10^{-3}\,\mathrm{Hz\,s^{-1}}$. This frequency evolution is atypical compared to those observed in similar burst oscillation sources. We tentatively attribute the observed drift to a Doppler shift induced by orbital motion. Under this interpretation, the inferred orbital period must be shorter than 20 minutes, placing \textit{4U~0614+091} among the most compact known low-mass X-ray binaries. |
| title | Detection of Oscillations in a Type I X-Ray Burst of 4U 0614+091 with SVOM/ECLAIRs |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2601.09691 |