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.
J., & Miller-Jones, J
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
fields
astro-ph.HE 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
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
-
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.
-
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.
-
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.