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Formation and evolution of transient jets and their cavities in black-hole X-ray binaries
High Energy Astrophysical Phenomena · Submitted 6 Jul 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We propose a model explaining the origin of transient/episodic jets in black-hole X-ray binaries, in which they are caused by transitions from a collimated, strongly magnetized, jet to a wide, un-collimated, outflow.
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The abstract, sentence by sentence
We propose a model explaining the origin of transient/episodic jets in black-hole X-ray binaries, in which they are caused by transitions from a collimated, strongly magnetized, jet to a wide, un-collimated, outflow. The change occurs when the accretion flow leaves the magnetically-choked state due to an increase of the accretion rate for a weakly varying magnetic flux. The formed powerful jet then detaches from its base, and propagates as a discrete ejection. The uncollimated outflow then produces a relativistic plasma that fills surrounding of the black hole, contributing to the formation of a low-density cavity. While the pressure in the cavity is in equilibrium with the surrounding interstellar medium (ISM), its inertia is orders of magnitude lower than that of the ISM. This implies that the plasma cannot efficiently decelerate the ejecta, explaining most of the observations. The modest deceleration within the cavities observed in some cases can be then due to the presence of clouds and/or filaments, forming a wide transition zone between the cavity and the ISM.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We propose a model explaining the origin of transient/episodic jets in black-hole X-ray binaries, in which they are caused by transitions from a collimated, strongly magnetized, jet to a wide, un-collimated, outflow. | contribution 0.92 | 0.41 | 0.75 | speculative 0.62 |
| s1 | The change occurs when the accretion flow leaves the magnetically-choked state due to an increase of the accretion rate for a weakly varying magnetic flux. | method 0.60 | 0.20 | 0.11 | asserted 0.99 |
| s2 | The formed powerful jet then detaches from its base, and propagates as a discrete ejection. | method 0.46 | 0.18 | 0.12 | asserted 1.00 |
| s3 | The uncollimated outflow then produces a relativistic plasma that fills surrounding of the black hole, contributing to the formation of a low-density cavity. | method 0.27 | 0.21 | 0.09 | asserted 0.97 |
| s4 | While the pressure in the cavity is in equilibrium with the surrounding interstellar medium (ISM), its inertia is orders of magnitude lower than that of the ISM. | result 0.50 | 0.22 | 0.07 | asserted 1.00 |
| s5 | This implies that the plasma cannot efficiently decelerate the ejecta, explaining most of the observations. | interpretation 0.99 | 0.26 | 0.41 | asserted 0.75 |
| s6 | The modest deceleration within the cavities observed in some cases can be then due to the presence of clouds and/or filaments, forming a wide transition zone between the cavity and the ISM. | interpretation 0.97 | 0.20 | 0.07 | hedged possibility 0.94 |
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Original abstract
We propose a model explaining the origin of transient/episodic jets in black-hole X-ray binaries, in which they are caused by transitions from a collimated, strongly magnetized, jet to a wide, un-collimated, outflow. The change occurs when the accretion flow leaves the magnetically-choked state due to an increase of the accretion rate for a weakly varying magnetic flux. The formed powerful jet then detaches from its base, and propagates as a discrete ejection. The uncollimated outflow then produces a relativistic plasma that fills surrounding of the black hole, contributing to the formation of a low-density cavity. While the pressure in the cavity is in equilibrium with the surrounding interstellar medium (ISM), its inertia is orders of magnitude lower than that of the ISM. This implies that the plasma cannot efficiently decelerate the ejecta, explaining most of the observations. The modest deceleration within the cavities observed in some cases can be then due to the presence of clouds and/or filaments, forming a wide transition zone between the cavity and the ISM.
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