The strength of Type-C quasi-periodic oscillations in black hole X-ray binaries correlates with the jet inclination
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| Main Authors: | , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| _version_ | 1866914606490845184 |
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| author | Vincentelli, F. M. Bollemeijer, N. Veledina, A. Altamirano, D. Bu, Q. Carotenuto, F. Casella, P. Cavecchi, Y. Ma, R. Marcel, G. Mastroserio, G. Motta, S. Zhang, L. |
| author_facet | Vincentelli, F. M. Bollemeijer, N. Veledina, A. Altamirano, D. Bu, Q. Carotenuto, F. Casella, P. Cavecchi, Y. Ma, R. Marcel, G. Mastroserio, G. Motta, S. Zhang, L. |
| contents | X-ray quasi-periodic oscillations (QPOs) are a characteristic feature of low-mass X-ray binaries (LMXBs). These oscillations have been studied for decades and revealed a rich and complex phenomenology that is still not fully understood. RXTE archival studies have shown that the amplitude of these oscillations differs significantly between black holes (BH) with high or low inclination. Yet, the actual dependence on inclination has never been adequately estimated. Thanks to the improvement of inclination measurements through radio observations and the recent observations by the HXMT satellite, we quantified for the first time the dependence of Type-C QPO amplitudes on the jet inclination of individual BH LMXBs. Our analysis reveals the presence of a significant linear correlation up to 8 Hz, strengthening the case for a ''geometrical'' origin of the QPOs. In addition, for a given QPO frequency, we observe systematically lower amplitudes during the decay of outbursts compared to the rise. This data collection represents a key benchmark for any QPO model. Our comparison with the predictions from a precessing hot flow shows that the amplitude of the QPOs can be reproduced by this scenario if the spin-orbit misalignment is at least $\approx$10-15$^\circ$. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2605_27510 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | The strength of Type-C quasi-periodic oscillations in black hole X-ray binaries correlates with the jet inclination Vincentelli, F. M. Bollemeijer, N. Veledina, A. Altamirano, D. Bu, Q. Carotenuto, F. Casella, P. Cavecchi, Y. Ma, R. Marcel, G. Mastroserio, G. Motta, S. Zhang, L. High Energy Astrophysical Phenomena X-ray quasi-periodic oscillations (QPOs) are a characteristic feature of low-mass X-ray binaries (LMXBs). These oscillations have been studied for decades and revealed a rich and complex phenomenology that is still not fully understood. RXTE archival studies have shown that the amplitude of these oscillations differs significantly between black holes (BH) with high or low inclination. Yet, the actual dependence on inclination has never been adequately estimated. Thanks to the improvement of inclination measurements through radio observations and the recent observations by the HXMT satellite, we quantified for the first time the dependence of Type-C QPO amplitudes on the jet inclination of individual BH LMXBs. Our analysis reveals the presence of a significant linear correlation up to 8 Hz, strengthening the case for a ''geometrical'' origin of the QPOs. In addition, for a given QPO frequency, we observe systematically lower amplitudes during the decay of outbursts compared to the rise. This data collection represents a key benchmark for any QPO model. Our comparison with the predictions from a precessing hot flow shows that the amplitude of the QPOs can be reproduced by this scenario if the spin-orbit misalignment is at least $\approx$10-15$^\circ$. |
| title | The strength of Type-C quasi-periodic oscillations in black hole X-ray binaries correlates with the jet inclination |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2605.27510 |