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.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
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astro-ph.HE 5years
2026 5representative citing papers
The earliest 1.3 mm observations of GRB 260127A detect 6.9 mJy emission 12.6 minutes post-trigger with a later non-detection implying decline at least as fast as t^{-0.5}, consistent with forward or reverse shock scenarios.
Discovery of Spearman correlation 0.8 between energy-dependent time lag and polarization degree in Swift J1727.8-1613, with theoretical arguments for additional mechanisms beyond inverse Comptonization.
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.
citing papers explorer
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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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Rapid-response 1.3 mm Observations of GRB 260127A with the Submillimeter Array
The earliest 1.3 mm observations of GRB 260127A detect 6.9 mJy emission 12.6 minutes post-trigger with a later non-detection implying decline at least as fast as t^{-0.5}, consistent with forward or reverse shock scenarios.
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Bridging X-ray Polarization with Timing & Spectroscopic Parameters of a galactic black hole: Swift J1727.8-1613
Discovery of Spearman correlation 0.8 between energy-dependent time lag and polarization degree in Swift J1727.8-1613, with theoretical arguments for additional mechanisms beyond inverse Comptonization.
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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.