Making the invisible visible: Magnetic fields in accretion flows revealed by X-ray polarization
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arXiv
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| Autori principali: | , |
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866910696203091968 |
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| author | Barnier, Samuel Done, Chris |
| author_facet | Barnier, Samuel Done, Chris |
| contents | Large scale, strong magnetic fields are often evoked in black hole accretion flows, for jet launching in the low/hard state and to circumvent the thermal instability in the high/soft state. Here we show how these ideas are strongly challenged by X-ray polarization measurements from IXPE. Quite general arguments show that equipartition large scale fields in the accretion flow should be of order $10^{6-8}$~G. These produce substantial Faraday rotation and/or depolarization. Since IXPE observes polarisation in both spectral states, this sets upper limits to coherent large scale (vertical, radial or azimulthal) magnetic fields in the photosphere of $B\lesssim 5\times10^6$~G. While we stress that Faraday rotation should be calculated for each individual simulation (density, field geometry and emissivity), it seems most likely that there are no equipartition strength large scale ordered fields inside the photosphere of the X-ray emitting gas. Strong poloidal fields can still power a Blandford-Znajek jet in the low/hard state if they thread the black hole horizon rather than the X-ray emitting flow, but this could also be challenged by (lack of) depolarisation from vacuum birefringence. Instead, an alternative solution is that the low/hard state jet is dominated by pairs so can be accelerated by lower fields. Strong toroidal fields could still stabilise the disc in the high/soft state if they are buried beneath the photosphere, though this seems unlikely due to magnetic buoyancy. Fundamentally, polarization data from IXPE means that magnetic fields in black hole accretion flows are no longer invisible and unconstrained. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_12815 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Making the invisible visible: Magnetic fields in accretion flows revealed by X-ray polarization Barnier, Samuel Done, Chris High Energy Astrophysical Phenomena Large scale, strong magnetic fields are often evoked in black hole accretion flows, for jet launching in the low/hard state and to circumvent the thermal instability in the high/soft state. Here we show how these ideas are strongly challenged by X-ray polarization measurements from IXPE. Quite general arguments show that equipartition large scale fields in the accretion flow should be of order $10^{6-8}$~G. These produce substantial Faraday rotation and/or depolarization. Since IXPE observes polarisation in both spectral states, this sets upper limits to coherent large scale (vertical, radial or azimulthal) magnetic fields in the photosphere of $B\lesssim 5\times10^6$~G. While we stress that Faraday rotation should be calculated for each individual simulation (density, field geometry and emissivity), it seems most likely that there are no equipartition strength large scale ordered fields inside the photosphere of the X-ray emitting gas. Strong poloidal fields can still power a Blandford-Znajek jet in the low/hard state if they thread the black hole horizon rather than the X-ray emitting flow, but this could also be challenged by (lack of) depolarisation from vacuum birefringence. Instead, an alternative solution is that the low/hard state jet is dominated by pairs so can be accelerated by lower fields. Strong toroidal fields could still stabilise the disc in the high/soft state if they are buried beneath the photosphere, though this seems unlikely due to magnetic buoyancy. Fundamentally, polarization data from IXPE means that magnetic fields in black hole accretion flows are no longer invisible and unconstrained. |
| title | Making the invisible visible: Magnetic fields in accretion flows revealed by X-ray polarization |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2404.12815 |