Transient Faraday-complex spectropolarimetric structure detected during radio flaring of Swift J1727 implies internal Faraday rotation from electron-proton jet plasma with rotating mass ~10^21 g, a small fraction of accreted mass.
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Type-C QPO amplitudes correlate linearly with jet inclination up to 8 Hz in BH LMXBs, lower on decay than rise, reproducible by precessing hot flow if misalignment ≥10-15°.
RGS spectra of V4641 Sgr reveal narrow N and O lines from a dense, multi-phase, photoionized disk atmosphere with log ξ ≈ 3.1 and 0.36 and velocities 540-720 km/s.
Radio precedes X-ray Compton luminosity by ~3 days in the rising hard state but lags by ~8 days in the decaying hard state of GX 339-4, with inner magnetic field strength estimated from accretion rate and truncation radius accounting for both.
citing papers explorer
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Spectropolarimetric detection of baryonic mass loading in a transient relativistic jet: application to the black hole X-ray binary Swift J1727.8$-$1613
Transient Faraday-complex spectropolarimetric structure detected during radio flaring of Swift J1727 implies internal Faraday rotation from electron-proton jet plasma with rotating mass ~10^21 g, a small fraction of accreted mass.
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The strength of Type-C quasi-periodic oscillations in black hole X-ray binaries correlates with the jet inclination
Type-C QPO amplitudes correlate linearly with jet inclination up to 8 Hz in BH LMXBs, lower on decay than rise, reproducible by precessing hot flow if misalignment ≥10-15°.
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Dense, multi-phase accretion disk atmosphere in the low-luminosity state of black hole transientV4641 Sgr
RGS spectra of V4641 Sgr reveal narrow N and O lines from a dense, multi-phase, photoionized disk atmosphere with log ξ ≈ 3.1 and 0.36 and velocities 540-720 km/s.
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Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion
Radio precedes X-ray Compton luminosity by ~3 days in the rising hard state but lags by ~8 days in the decaying hard state of GX 339-4, with inner magnetic field strength estimated from accretion rate and truncation radius accounting for both.