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| Format: | Preprint |
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2025
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| Online-Zugang: | https://arxiv.org/abs/2507.03644 |
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| _version_ | 1866909675849515008 |
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| author | Choudhury, Sreetama Das R., Bhuvana G. Das, Santabrata Nandi, Anuj |
| author_facet | Choudhury, Sreetama Das R., Bhuvana G. Das, Santabrata Nandi, Anuj |
| contents | We perform a comprehensive wide-band ($3-100$keV) spectro-temporal analysis of 13 outbursting BH-XRBs, using data (quasi)simultaneous with radio observations to unravel the complex disc-jet connection. RXTE observations are analyzed for XTEJ1859+226, GX339-4 (2002, 2006, and 2010 outbursts), 4U1543-47, H1743-322 (2003 and 2009 outbursts), XTEJ1550-564, XTEJ1752-223, XTEJ1650-500, SwiftJ1753.5-0127, XTEJ1748-288, and GROJ1655-40. For SwiftJ1727.8-1613 and MAXIJ1535-571, we utilize HXMT data, while both AstroSat and HXMT observations are analyzed for SwiftJ1658.2-4242. Type-C QPOs observed in harder states (LHS, HIMS; $F_{nth}\ge0.4$) exhibit positive lag for low-inclination sources ($i<50^{\circ}$), whereas it generally exhibits negative lag for high-inclination sources ($i>60^{\circ}$), except XTEJ1550-564, SwiftJ1727.8-1613, H1743-322 (2003 outburst) and GROJ1655-40. Notably, type-A QPOs exhibit negative lags ($\sim1-10$ms) regardless of source inclination, while type-B QPOs show positive lags in low-inclination sources, and both positive and negative lags ($\sim1-15$ms) in high-inclination sources, typically occurring in SIMS ($F_{nth}\lesssim0.45$). Systematic appearance of type-A QPOs preceding radio flares in several sources suggests that type-A QPOs indicate telltale signs of jet ejection, while type-B QPOs are closely linked with radio flares (i.e., transient jets). Present findings suggest the corona evolves from a radially extended to a vertically elongated structure during the type-C to type-B transition via type-A QPOs, with type-B QPOs linked to radially compact or vertically extended coronal geometries, resembling jet ejection. The strong radio-X-ray luminosity correlation seems to provide compelling evidence of accretion-powered jets. Finally, we find that jets in SIMS are moderately relativistic in nature with velocities $\gtrsim 0.3-0.8c$ in BH-XRBs under consideration. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_03644 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Revisiting Disc-Jet Coupling in Black Hole X-ray Binaries: On the Nature of Disc Dynamics and Jet Velocity Choudhury, Sreetama Das R., Bhuvana G. Das, Santabrata Nandi, Anuj High Energy Astrophysical Phenomena We perform a comprehensive wide-band ($3-100$keV) spectro-temporal analysis of 13 outbursting BH-XRBs, using data (quasi)simultaneous with radio observations to unravel the complex disc-jet connection. RXTE observations are analyzed for XTEJ1859+226, GX339-4 (2002, 2006, and 2010 outbursts), 4U1543-47, H1743-322 (2003 and 2009 outbursts), XTEJ1550-564, XTEJ1752-223, XTEJ1650-500, SwiftJ1753.5-0127, XTEJ1748-288, and GROJ1655-40. For SwiftJ1727.8-1613 and MAXIJ1535-571, we utilize HXMT data, while both AstroSat and HXMT observations are analyzed for SwiftJ1658.2-4242. Type-C QPOs observed in harder states (LHS, HIMS; $F_{nth}\ge0.4$) exhibit positive lag for low-inclination sources ($i<50^{\circ}$), whereas it generally exhibits negative lag for high-inclination sources ($i>60^{\circ}$), except XTEJ1550-564, SwiftJ1727.8-1613, H1743-322 (2003 outburst) and GROJ1655-40. Notably, type-A QPOs exhibit negative lags ($\sim1-10$ms) regardless of source inclination, while type-B QPOs show positive lags in low-inclination sources, and both positive and negative lags ($\sim1-15$ms) in high-inclination sources, typically occurring in SIMS ($F_{nth}\lesssim0.45$). Systematic appearance of type-A QPOs preceding radio flares in several sources suggests that type-A QPOs indicate telltale signs of jet ejection, while type-B QPOs are closely linked with radio flares (i.e., transient jets). Present findings suggest the corona evolves from a radially extended to a vertically elongated structure during the type-C to type-B transition via type-A QPOs, with type-B QPOs linked to radially compact or vertically extended coronal geometries, resembling jet ejection. The strong radio-X-ray luminosity correlation seems to provide compelling evidence of accretion-powered jets. Finally, we find that jets in SIMS are moderately relativistic in nature with velocities $\gtrsim 0.3-0.8c$ in BH-XRBs under consideration. |
| title | Revisiting Disc-Jet Coupling in Black Hole X-ray Binaries: On the Nature of Disc Dynamics and Jet Velocity |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2507.03644 |