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°.
J., & Miller-Jones, J
6 Pith papers cite this work. Polarity classification is still indexing.
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2026 6verdicts
UNVERDICTED 6representative citing papers
A relativistic funnel scattering model with variable bulk velocity reproduces the ~23% hard-state and ~12% soft-state polarization in Cygnus X-3 at low inclination using half-opening angles of 13-16 degrees.
The GeV emission zone in Cygnus X-3 is too large and magnetized too weakly to accelerate protons to PeV energies, so the PeV gamma rays must originate from a more compact inner region with rapid magnetic field dissipation.
The counterjet dominates PeV photon production in Cyg X-3 due to longer interaction paths through the donor star's wind at low inclination.
A recurring 0.03 Hz radio QPO was detected in the 2025 flare of GRS 1915+105 at >5.9 sigma in one epoch, identical across S- and X-bands and prior years, indicating an intrinsic accretion-jet timescale.
A review of extreme gamma-ray transients defined as catastrophic events or extreme particle acceleration regimes, covering diagnostics, instruments, and source classes.
citing papers explorer
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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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Relativistic Scattering in the Funnel of Cygnus X-3
A relativistic funnel scattering model with variable bulk velocity reproduces the ~23% hard-state and ~12% soft-state polarization in Cygnus X-3 at low inclination using half-opening angles of 13-16 degrees.
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Constraining the PeV gamma-ray emission zone of Cygnus X-3 with contemporaneous GeV timing and spectral observations
The GeV emission zone in Cygnus X-3 is too large and magnetized too weakly to accelerate protons to PeV energies, so the PeV gamma rays must originate from a more compact inner region with rapid magnetic field dissipation.
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The counterjet dominates the production of PeV photons from Cyg X-3
The counterjet dominates PeV photon production in Cyg X-3 due to longer interaction paths through the donor star's wind at low inclination.
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A 0.03 Hz Radio Quasi-periodic Oscillation During the 2025 Flare of GRS 1915+105
A recurring 0.03 Hz radio QPO was detected in the 2025 flare of GRS 1915+105 at >5.9 sigma in one epoch, identical across S- and X-bands and prior years, indicating an intrinsic accretion-jet timescale.
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Extreme Transients in Gamma Rays
A review of extreme gamma-ray transients defined as catastrophic events or extreme particle acceleration regimes, covering diagnostics, instruments, and source classes.